%% Books
@inbook{SK-Chapter,
Author = {Walter, CW},
Title = {The super-kamiokande experiment},
Pages = {19-43},
Booktitle = {Neutrino Oscillations: Present Status and Future
Plans},
Publisher = {World Scientific},
Editor = {J. Thomas and P. Vahle},
Chapter = {The Super-Kamiokande Experiment},
Year = {2008},
Month = {January},
ISBN = {9789812771964},
url = {http://arxiv.org/abs/0802.1041},
Abstract = {Super-Kamiokande is a 50 kiloton water Cherenkov detector
located at the Kamioka Observatory of the Institute for
Cosmic Ray Research, University of Tokyo. It was designed to
study neutrino oscillations and carry out searches for the
decay of the nucleon. The Super-Kamiokande experiment began
in 1996 and in the ensuing 10 years of running has produced
extremely important results in the fields of atmospheric and
solar neutrino oscillations. Furthermore, it has set
stringent limits on the decay of the nucleon and the
existence of dark matter and astrophysical sources of
neutrinos. Perhaps most crucially, Super-Kamiokande was the
first to definitively show that neutrinos have mass and
undergo flavor oscillations. This chapter will summarize the
published scientific output of the experiment with a
particular emphasis on the atmospheric neutrino
results.},
Doi = {10.1142/9789812771971_0002},
Key = {SK-Chapter}
}
%% Papers Published
@article{fds248724,
Author = {Ahlen, SP and Ambrosio, M and Auriemma, G and Baldini, A and Barbarino,
GC and Barish, B and Battistoni, G and Bellotti, R and Bemporad, C and Bernardini, P and Bilokon, H and Bisi, V and Bloise, C and Bussino, S and Cafagna, F and Calicchio, M and Campana, P and Cecchini, S and Cei, F and Chiarella, V and Chrysicopoulou, P and Cormack, R and Coutu, S and De
Marzo, C and De Cataldo and G and De Vincenzi and M and Di Credico and A and Diehl, E and Erriquez, O and Fabbri, M and Favuzzi, C and Forti, C and Foti, L and Fusco, P and Giacomelli, G and Giannini, G and Giglietto, N and Giubellino, P and Grassi, M and Green, P and Grillo, A and Guarino, F and Gustavino, C and Heinz, R and Hong, J and Iarocci, E and Klein, S and Lamanna, E and Lane, C and Levin, D and Lipari, P and Liu, G and Liu, R and Longo, M and Ludlam, G and Mancarella, G and Mandrioli, G and Margiotta-Neri, A and Marin, A and Marini, A and Martello, D and Martellotti, G and Marzari-Chiesa, A and Masera, M and Matteuzzi, P and Michael, DG and Miller, L and Monacelli, P and Monteno, M and Mufson, S and Musser, J and Osteria, G and Pal, B and Palamara, O and Patera, V and Patrizii, L and Pazzi, R and Peck, CW and Petrakis, J and Petrera, S and Pignatano, N and Pistilli, P and Predieri, F and Raino, A and Ramello,
L and Reynoldson, J and Ronga, F and Rosa, G and Sanzani, GL and Satta, L and Scapparoni, E and Scholberg, K and Sciubba, A and Serra-Lugaresi, P and Severi, M and Smith, C and Spinelli, P and Spinetti, M and Spurio, M and Steele, J},
Title = {Cosmic ray search for strange quark matter with the macro
detector},
Journal = {Nuclear Physics B (Proceedings Supplements)},
Volume = {24},
Number = {2},
Pages = {191-194},
Publisher = {Elsevier BV},
Year = {1991},
Month = {January},
ISSN = {0920-5632},
url = {http://dx.doi.org/10.1016/0920-5632(91)90323-7},
Abstract = {The MACRO detector is sensitive to any fast or slow highly
ionizing massive particles in cosmic rays. These include
"nuclearites" or strange quark matter. The negative result
of a search lasting about 20 months using 1 12 of the
detector has yielded a flux limit of 1.1 × 10-14cm-2sr-1s-1
for strange matter with mass 10-11 g < m < 0.1g. For m >
0.1gg, the limit is 5.5 × 10-15cm-2sr-1s-1. Since the
velocity range of nuclearites to which MACRO is sensitive
extends to near the escape velocity of the earth, the flux
limit not only applies to nuclearites of galactic or
extra-galactic origin but also applies to nuclearites that
are trapped in the solar system. © 1991.},
Doi = {10.1016/0920-5632(91)90323-7},
Key = {fds248724}
}
@article{fds248691,
Author = {Ahlen, S and Ambrosio, M and Antolini, R and Auriemma, G and Baker, R and Baldini, A and Barbarino, GC and Barish, BC and Battistoni, G and Bellotti, R and Bemporad, C and Bernardini, P and Bilokon, H and Bisi,
V and Bloise, C and Bower, C and Bussino, S and Cafagna, F and Calicchio,
M and Campana, P and Campana, D and Carboni, M and Cecchini, S and Cei, F and Chiarella, V and Chiera, C and Cobis, A and Cormack, R and Corona, A and Coutu, S and DeCataldo, G and DeMarzo, C and De Vincenzi and M and Di
Credico, A and Diehl, E and Dekhissi, H and Erriquez, O and Favuzzi, C and Ficenec, D and Forti, C and Foti, L and Fusco, P and Giacomelli, G and Giannini, G and Giglietto, N and Giubellino, P and Grassi, M and Green,
P and Grillo, A and Guarino, F and Gustavino, C and Habig, A and Heinz, R and Hong, JT and Iarocci, E and Katsavounidis, E and Kearns, E and Klein, S and Kyriazopoulou, S and Lamanna, E and Lane, C and Lee, C and Levin, D and Lipari, P and Liu, G and Liu, R and Longo, MJ and Ludlam, G and Mancarella,
G and Mandrioli, G and Margiotta-Neri, A and Marin, A and Marini, A and Martello, D and Martellotti, G and Marzari Chiesa and A and Masera, M and Matteuzzi, P and Michael, DG and Miller, L and Monacelli, P and Monteno,
M and Mufson, S and Musser, J and Nicoló, D and Nutter, S and Okada, C and Osteria, G and Palamara, O and Parlati, S and Patera, V and Patrizii, L and Pazzi, R and Peck, CW and Petrakis, J and Petrera, S and Pignatano, ND and Pistilli, P and Predieri, F and Ramello, L},
Title = {Search for neutrino bursts from collapsing stars with the
MACRO detector},
Journal = {Astroparticle Physics},
Volume = {1},
Number = {1},
Pages = {11-25},
Publisher = {Elsevier BV},
Year = {1992},
Month = {January},
ISSN = {0927-6505},
url = {http://dx.doi.org/10.1016/0927-6505(92)90005-K},
Doi = {10.1016/0927-6505(92)90005-K},
Key = {fds248691}
}
@article{fds248748,
Author = {Bellotti, R and Cafagna, F and Calicchio, M and De Cataldo and G and De
Marzo, C and Erriquez, O and Favuzzi, C and Fusco, P and Giglietto, N and Spinelli, P and Petrakis, J and Antolini, R and Bam, BB and Cecchini, S and Giacomelli, G and Mandrioli, G and Margiotta-Neri, A and Matteuzzi,
P and Patrizii, L and Predieri, F and Scapparone, E and Serra Lugaresi,
P and Spurio, M and Togo, V and Ahlen, S and Cormack, R and Kearns, E and Klein, S and Ludlam, G and Marin, A and Okada, C and Stone, J and Sulak, L and Worstell, W and Barish, B and Coutu, S and Hong, J and Katsuvounidis, E and Kyriazopoulou, S and Liu, G and Liu, R and Michael, D and Peck, C and Pignatano, N and Scholberg, K and Steele, J and Walter, C and Lane, C and Steinberg, R and Battistoni, G and Bilokon, H and Bloise, C and Campana,
P and Cavallo, P and Chiarella, V and Forti, C and Grillo, A and Iarocci,
E and Marini, A and Patera, V and Ronga, F and Satta, L and Spinetti, M and Valenti, V and Gustavino, C and Reynoldson, J and Habig, A and Heinz, R and Miller, L and Mufson, S and Musser, J and Nutter, S and Di Credico and A and Monacelli, P and Bernardini, P and Mancarella, G and Martello, D and Palamara, O and Petrera, S and Pistilli, P and Surdo, A and Diehl, E and Levin, D and Longo, M and Smith, C and Tarlé, G and Ambrosio, M and Barbarino, GC and Guarino, F and Osteria, G and Baldini, A and Bemporad,
C and Cei, F and Giannini, G and Grassi, M and Pazzi, R and Auriemma, G and Bussino, S and Chiera, C and Chrysicopoulou, P},
Title = {Search for stellar gravitational collapse by MACRO:
Characteristics and results},
Journal = {Nuclear Physics B (Proceedings Supplements)},
Volume = {28},
Number = {1},
Pages = {61-64},
Publisher = {Elsevier BV},
Year = {1992},
Month = {January},
ISSN = {0920-5632},
url = {http://dx.doi.org/10.1016/0920-5632(92)90147-K},
Abstract = {The first MACRO lower supermodule has been sensitive to
antineutrinos from stellar gravitational collapse since
spring 1989. The results with the 44 tonnes of liquid
scintillator which have been instrumented to search for
stellar gravitational collapse are discussed here. ©
1992.},
Doi = {10.1016/0920-5632(92)90147-K},
Key = {fds248748}
}
@booklet{Bellotti92,
Author = {Belloti, R and Cafagna, F and Callichio, M and De Cataldo and G and De
Marzo, C and Enriquez, O and Favuzzi, C and Fusco, P and Giglietto, N and Spinelli, P and Petrakis, J and Cecchini, S and Giacomelli, G and Mandrioli, G and Margiotta-Neri, A and Matteuzzi, P and Patrizii, L and Predieri, F and Sanzani, GL and Scapparone, E and Serra Lugaresi and P and Spurio, M and Togo, V and Ahlen, S and Cormack, R and Kearns, E and Klein,
S and Ludlam, G and Marin, A and Okada, C and Stone, JL and Sulak, L and Worstell, W and Barish, B and Coutu, S and Hong, J and Katsuvounidis, E and Kyriazopoulou, S and Liu, G and Liu, R and Michael, D and Peck, C and Pignatano, N and Scholberg, K and Steele, J and Walter, CW and Lane, C and Steinberg, R and Battistoni, G and Bilokon, H and Bloise, C and Campana,
P and Carboni, M and Chiarella, V and Forti, C and Grillo, A and Iarocci,
E and Marini, A and Patera, V and Ronga, F and Satta, L and Spinetti, M and Valente, V and Gustavino, C and Reynoldson, J and Habig, A and Heinz, R and Miller, L and Mufson, S and Musser, J and Nutter, S and Di Credico and A and Monacelli, P and Bernardini, P and Mancarella, G and Martello, D and Palamara, O and Petrera, S and Pistilli, P and Surdo, A and Diehl, E and Levin, D and Longo, M and Smith, C and Tarlé, G and Ambrosio, M and Barbarino, GC and Guarino, F and Osteria, G and Baldini, A and Bemporad,
C and Cei, F and Giannini, G and Grassi, M and Pazzi, R and Auriemma, G and Bussino, S and Chiera, C and Chrysicopoulou, P and Corona,
A},
Title = {Measurement of electromagnetic and TEV muon components of
extensive air showers by eas-top and MACRO
experiments},
Journal = {Nuclear Physics B (Proceedings Supplements)},
Volume = {28},
Number = {1},
Pages = {393-396},
Publisher = {Elsevier BV},
Year = {1992},
Month = {January},
ISSN = {0920-5632},
url = {http://dx.doi.org/10.1016/0920-5632(92)90201-3},
Abstract = {The simultaneous observation of the electromagnetic and TeV
muon components of extensive air showers by the EAS-TOP and
MACRO detectors, respectively, is described for a period of
100 days in 1990. The two detectors and their combined
resolutions are briefly reviewed and muon multiplicity
distributions for various detector configurations are
presented. A first analysis of the physical parameters Nμ
and Ne related to the study of the primary composition at
Eν = 1014 - 1016 eV is also presented. ©
1992.},
Doi = {10.1016/0920-5632(92)90201-3},
Key = {Bellotti92}
}
@article{fds248692,
Author = {Ahlen, SP and Ambrosio, M and Auriemma, G and Baldini, A and Barbarino,
GC and Barish, B and Battistoni, G and Bellotti, R and Bemporad, C and Bernardini, P and Bilokon, H and Bisi, V and Bloise, C and Bussino, S and Cafagna, F and Calicchio, M and Campana, P and Cecchini, S and Cei, F and Chiarella, V and Chrysicopoulou, P and Cormack, R and Coutu, S and De
Marzo, C and De Cataldo and G and De Vincenzi and M and Di Credico and A and Diehl, E and Erriquez, O and Fabbri, M and Favuzzi, C and Forti, C and Foti, L and Fusco, P and Giacomelli, G and Giannini, G and Giglietto, N and Giubellino, P and Grassi, M and Green, P and Grillo, A and Guarino, F and Gustavino, C and Heinz, R and Hong, J and Iarocci, E and Klein, S and Lamanna, E and Lane, C and Levin, D and Lipari, P and Liu, G and Liu, R and Longo, M and Ludlam, G and Mancarella, G and Mandrioli, G and Margiotta-Neri, A and Marin, A and Marini, A and Martello, D and Martellotti, G and Marzari-Chiesa, A and Masera, M and Matteuzzi, P and Michael, D and Miller, L and Monacelli, P and Monteno, M and Mufson, S and Musser, J and Osteria, G and Pal, B and Palamara, O and Patera, V and Patrizii, L and Pazzi, R and Peck, C and Petrakis, J and Petrera, S and Pignatano, N and Pistilli, P and Predieri, F and Ramello, L and Reynoldson, J and Ronga, F and Rosa, G and Sanzani, GL and Satta, L and Scapparone, E and Scholberg, K and Sciubba, A and Serra-Lugaresi, P and Severi, M and Smith, C and Spinelli, P and Spinetti, M and Spurio, M and Steele, J and Steinberg, R},
Title = {Arrival time distributions of very high energy cosmic ray
muons in MACRO},
Journal = {Nuclear Physics, Section B},
Volume = {370},
Number = {2},
Pages = {432-444},
Publisher = {Elsevier BV},
Year = {1992},
Month = {February},
ISSN = {0550-3213},
url = {http://dx.doi.org/10.1016/0550-3213(92)90292-J},
Abstract = {We present a study of the correlations in the arrival times
of about 1016 single and multiple muons detected by the
first two MACRO supermodules. The time correlations, from
milliseconds to several hundrends of seconds, have been
analyzed in terms of the random distribution, with which
they are consistent. An analysis of the arrival times (up to
180 ns) of the muons from the same multimuon event is also
given. © 1992.},
Doi = {10.1016/0550-3213(92)90292-J},
Key = {fds248692}
}
@article{fds328069,
Author = {Petrera, S},
Title = {Search of strange quark matter using MACRO
detector},
Journal = {Nuclear Physics B - Proceedings Supplements},
Volume = {28},
Number = {1},
Pages = {306-309},
Publisher = {Elsevier BV},
Year = {1992},
Month = {July},
url = {http://dx.doi.org/10.1016/0920-5632(92)90189-y},
Doi = {10.1016/0920-5632(92)90189-y},
Key = {fds328069}
}
@article{fds328070,
Author = {Palamara, O},
Title = {Multiple muons and primary cosmic composition studies with
MACRO},
Journal = {Nuclear Physics B - Proceedings Supplements},
Volume = {28},
Number = {1},
Pages = {389-392},
Publisher = {Elsevier BV},
Year = {1992},
Month = {July},
url = {http://dx.doi.org/10.1016/0920-5632(92)90200-c},
Doi = {10.1016/0920-5632(92)90200-c},
Key = {fds328070}
}
@booklet{Ahlen92b,
Author = {Ahlen, S and Ambrosio, M and Antolini, R and Auriemma, G and Baldini, A and Bam, BB and Barbarino, GC and Barish, BC and Battistoni, G and Bellotti,
R and Bemporad, C and Bernardini, P and Bilokon, H and Bisi, V and Bloise,
C and Bussino, S and Cafagna, F and Calicchio, M and Campana, P and Campana, D and Carboni, M and Cecchini, S and Cei, F and Chiarella, V and Chiera, C and Cobis, A and Cormack, R and Corona, A and Coutu, S and DeCataldo, G and DeMarzo, C and De Vincenzi M, and Di Credico A, and Diehl, E and Erriquez, O and Favuzzi, C and Ficenec, D and Forti, C and Foti, L and Fusco, P and Giacomelli, G and Giannini, G and Giglietto, N and Giubellino, P and Grassi, M and Green, P and Grillo, A and Guarino, F and Gustavino, C and Habig, A and Heinz, R and Hong, JT and Iarocci, E and Katsavounidis, E and Kearns, E and Klein, S and Kyriazopoulou, S and Lamanna, E and Lane, C and Lee, C and Levin, D and Lipari, P and Liu, G and Liu, R},
Title = {Study of the ultrahigh-energy primary-cosmic-ray composition
with the MACRO experiment.},
Journal = {Physical review. D, Particles and fields},
Volume = {46},
Number = {3},
Pages = {895-902},
Year = {1992},
Month = {August},
ISSN = {0556-2821},
url = {http://dx.doi.org/10.1103/physrevd.46.895},
Abstract = {We present the analysis of multiple-muon events collected
with one supermodule (1013 h live time) and two supermodules
(1195 h live time) of the MACRO detector at Gran Sasso,
Italy. Multimuon rates are shown to be sensitive to
primary-cosmic-ray energies between 50 TeV and several
thousand TeV. Experimental data are compared with the
expected rates from two composition models: a light (i.e.,
proton-rich) and a heavy (i.e., Fe-rich) composition. The
predictions are based on a Monte Carlo simulation of the
hadronic interactions of cosmic-ray nuclei, followed by a
detailed tracking of the muons through the rock and the
experimental apparatus. The results show good sensitivity of
the MACRO detector to primary composition. The data exhibit
a preference towards the light composition model. © 1992
The American Physical Society.},
Doi = {10.1103/physrevd.46.895},
Key = {Ahlen92b}
}
@booklet{Ahlen92a,
Author = {Ahlen, S and Ambrosio, M and Antolini, R and Auriemma, G and Baker, R and Baldini, A and Barbarino, GC and Barish, BC and Battistoni, G and Bellotti, R and Bemporad, C and Bernardini, P and Bilokon, H and Bisi,
V and Bloise, C and Bussino, S and Cafagna, F and Calicchio, M and Campana,
P and Campana, D and Carboni, M and Cecchini, S and Cei, F and Chiarella,
V and Chiera, C and Cobis, A and Cormack, R and Corona, A and Coutu, S and DeCataldo, G and Dekhissi, H and DeMarzo, C and De Vincenzi M, and Di
Credico A, and Diehl, E and Erriquez, O and Favuzzi, C and Ficenec, D and Forti, C and Foti, L and Fusco, P and Giacomelli, G and Giannini, G and Giglietto, N and Giubellino, P and Grassi, M and Green, P and Grillo, A and Guarino, F and Gustavino, C and Habig, A and Heinz, R and Hong, JT and Iarocci, E and Katsavounidis, E and Kearns, E and Klein, S and Kyriazopoulou, S and Lamanna, E and Lane, C and Lee, C and Levin, D and Lipari, P and Liu, G},
Title = {Search for nuclearites using the MACRO detector.},
Journal = {Physical review letters},
Volume = {69},
Number = {13},
Pages = {1860-1863},
Year = {1992},
Month = {September},
ISSN = {0031-9007},
url = {http://dx.doi.org/10.1103/physrevlett.69.1860},
Abstract = {A negative search using 1/12 of the eventual MACRO detector
has yielded nuclearite flux limits of 1.1×10-14 cm-2 sr-1
s-1 for 10-10<m<0.1 g, and 5.5×10-15 cm-2 sr-1 s-1
for m>0.1 g. We have modified the formula of De Rújula
and Glashow for the light yield of nuclearites to include
the uv light absorbed and reemitted in the visible region,
and proved that the MACRO sensitivity extends almost to the
escape velocity of the Earth. Our flux limit, therefore, can
be used to address nuclearites that are possibly trapped in
the solar system. © 1992 The American Physical
Society.},
Doi = {10.1103/physrevlett.69.1860},
Key = {Ahlen92a}
}
@booklet{Ahlen92,
Author = {Ahlen, S and Ambrosio, M and Antolini, R and Auriemma, G and Baldini, A and Barbarino, GC and Barish, BC and Battistoni, G and Bellotti, R and Bemporad, C and Bernardini, P and Bilokon, H and Bisi, V and Bloise, C and Bussino, S and Cafagna, F and Calicchio, M and Campana, D and Campana,
P and Carboni, M and Cecchini, S and Cei, F and Chiarella, V and Chiera, C and Cobis, A and Cormack, R and Corona, A and Coutu, S and DeCataldo, G and Dekhussi, H and DeMarzo, C and De Vincenzi M, and Di Credico A, and Diehl, E and Erriquez, O and Favuzzi, C and Ficenec, D and Forti, C and Foti, L and Fusco, P and Giacomelli, G and Giannini, G and Giglietto, N and Giubellino, P and Grassi, M and Green, P and Grillo, A and Guarino, F and Gustavino, C and Habig, A and Heinz, R and Hong, JT and Iarocci, E and Katsavounidis, E and Kearns, E and Klein, S and Kyriazopoulou, S and Lamanna, E and Lane, C and Lee, C and Levin, DS and Lipari, P and Liu, G and Liu, R},
Title = {Measurement of the decoherence function with the MACRO
detector at Gran Sasso.},
Journal = {Physical review. D, Particles and fields},
Volume = {46},
Number = {11},
Pages = {4836-4845},
Year = {1992},
Month = {December},
ISSN = {0556-2821},
url = {http://dx.doi.org/10.1103/physrevd.46.4836},
Abstract = {A measurement of the underground muon decoherence function
has been performed using the multiple muon events collected
by the MACRO detector at the Gran Sasso National Laboratory.
A detector-independent analysis is presented for different
zenith regions and rock depths; this allows direct
comparison with any model of hadronic interactions. The
measured decoherence function is compared with the
predictions of a Monte Carlo simulation based on data taken
by recent collider experiments. © 1992 The American
Physical Society.},
Doi = {10.1103/physrevd.46.4836},
Key = {Ahlen92}
}
@article{fds248749,
Author = {Ahlen, S and Ambrosio, M and Antolini, R and Auriemma, G and Baldini, A and Barbarino, GC and Barish, B and Battistoni, G and Bellotti, R and Bemporad, C and Bernardini, P and Bilokon, H and Bisi, V and Bloise, C and Boiano, A and Bower, C and Bussino, S and Cafagna, F and Calicchio, M and Campana, P and Campana, D and Candela, A and Carboni, M and Cecchini, S and Cei, F and Chiarella, V and Chiera, C and Cobis, A and Cormack, R and Corona, A and Cosson, D and Coutu, S and D'Antone, I and De Cataldo and G and De Marzo and C and Denni, U and De Seriis and N and DeVincenzi, M and Di
Credico, A and Diehl, E and Diotallevi, R and Erriquez, O and Favuzzi,
C and Ficenec, D and Forti, C and Foti, L and Frani, A and Fusco, P and Gherarducci, F and Giacomelli, G and Giannini, G and Giglietto, N and Giubellino, P and Grassi, M and Green, P and Grillo, A and Guarino, F and Gustavino, C and Habig, A and Hanson, J and Hazen, E and Heinz, R and Hong,
JT and Iarocci, E and Katsavounidis, E and Kearns, E and Klein, S and Kyriazopoulou, S and Lamanna, E and Lane, C and Lee, C and Levin, D and Lipari, P and Liu, G and Liu, R and Longo, MJ and Ludlam, G and Mancarella,
G and Mandrioli, G and Marin, A and Marini, A and Martello, D and Martellotti, G and Marzari Chiesa and A and Masera, M and Matteuzzi, P and Mengucci, A and Merritt, S and Michael, DG and Miller, L and Monacelli,
P and Mongelli, M and Monteno, M and Mufson, S and Musser, J and Nutter, S and Okada, C and Osteria, G and Palamara, O and Parascandalo,
P},
Title = {First supermodule of the MACRO detector at Gran
Sasso},
Journal = {Nuclear Inst. and Methods in Physics Research,
A},
Volume = {324},
Number = {1-2},
Pages = {337-362},
Year = {1993},
Month = {January},
ISSN = {0168-9002},
url = {http://dx.doi.org/10.1016/0168-9002(93)90997-V},
Abstract = {In this paper the design, construction and performance of
the lower part of the first supermodule of the MACRO
detector is described. © 1993.},
Doi = {10.1016/0168-9002(93)90997-V},
Key = {fds248749}
}
@article{fds326733,
Author = {Ahlen, S and Ambrosio, M and Antolini, R and Auriemma, G and Baldini, A and Bam, B and Barbarino, G and Barish, B and Battistoni, G and Bellotti, R and Bemporad, C and Bernardini, P and Bilokon, H and Bisi, V and Bloise, C and Bussino, S and Cafagna, F and Calicchio, M and Campana, P and Campana,
D and Carboni, M and Cecchini, S and Cei, F and Chiarella, V and Chiera, C and Cobis, A and Cormack, R and Corona, A and Coutu, S and Decataldo, G and Dekhissi, H and Demarzo, C and de Vincenzi, M and di Credico, A and Diehl, E and Erriquez, O and Favuzzi, C and Ficenec, D and Forti, C and Foti, L and Fusco, P and Giacomelli, G and Giannini, G and Giglietto, N and Giubellino, P and Grassi, M and Green, P and Grillo, A and Guarino, F and Gustavino, C and Habig, A and Heinz, R and Hong, J and Iarocci, E and Katsavounidis, E and Kearns, E and Klein, S and Kyriazopoulou, S and Lamanna, E and Lane, C and Lee, C and Levin, D and Lipari, P and Liu, G and Liu, R and Longo, M and Ludlam, G and Mancarella, G and Mandrioli, G and Margiotta-Neri, A and Marin, A and Marini, A and Martello, D and Martellotti, G and Marzari Chiesa and A and Masera, M and Matteuzzi, P and Michael, D and Miller, JL and Monacelli, P and Monteno, M and Mufson,
SL and Musser, J and Nutter, S and Okada, C and Osteria, G and Palamara, O and Parlati, S and Patera, V and Patrizii, L and Pazzi, R and Peck, C and Petrakis, J and Petrera, S and Pignatano, N and Pistilli, P and Predieri, F and Ramello, L and Reynoldson, J and Ronga, F and Rosa, G and Satriano, C and Satta, L and Scapparone, E and Scholberg, K and Sciubba,
A and Serra Lugaresi and P and Severi, M and Sitta, M and Spinelli, P and Spinetti, M and Spurio, M and Steele, J and Steinberg, R and Stone, J and Sulak, L and Surdo, A and Tarle, G and Togo, V and Valente, V and Verdone,
G and Walter, C and Webb, R and Worstell, W and The MACRO
Collaboration},
Title = {Muon astronomy with the MACRO detector},
Journal = {The Astrophysical Journal},
Volume = {412},
Number = {1},
Pages = {301-301},
Publisher = {American Astronomical Society},
Year = {1993},
Month = {July},
url = {http://dx.doi.org/10.1086/172921},
Doi = {10.1086/172921},
Key = {fds326733}
}
@booklet{Ahlen94,
Author = {Ahlen, S and Ambrosio, M and Antolini, R and Auriemma, G and Baker, R and Baldini, A and Bam, BB and Barbarino, GC and Barish, BC and Battistoni,
G and Bellotti, R and Bemporad, C and Bernandini, P and Bilokon, H and Bisi, V and Bloise, C and Bower, C and Bussino, S and Cafagna, F and Calicchio, M and Campana, D and Campana, P and Carboni, M and Cecchini,
S and Cei, F and Chiarella, V and Cormack, R and Corona, A and Coutu, S and De
Cataldo G, and Dekhissi, H and De Marzo C, and De Vincenzi M, and Di
Credico A, and Diehl, E and Erriquez, O and Favuzzi, C and Ficenec, D and Forti, C and Fusco, P and Giacomelli, G and Giannini, G and Giglietto,
N and Giubellino, P and Grassi, M and Green, P and Grillo, A and Guarino,
F and Guarnaccia, P and Gustavino, C and Habig, A and Heinz, R and Hong,
JT and Iarocci, E and Katsavounidis, E and Kearns, E and Klein, S and Kyriazopoulou, S and Lamanna, E and Lane, C and Lee, C and Levin, D and Lipari, P and Liu, G},
Title = {Search for slowly moving magnetic monopoles with the MACRO
detector.},
Journal = {Physical review letters},
Volume = {72},
Number = {5},
Pages = {608-612},
Year = {1994},
Month = {January},
ISSN = {0031-9007},
url = {http://dx.doi.org/10.1103/physrevlett.72.608},
Abstract = {A search for slowly moving magnetic monopoles in the cosmic
radiation was conducted from October 1989 to November 1991
using the large liquid scintillator detector subsystem of
the first supermodule of the MACRO detector at the Gran
Sasso underground laboratory. The absence of candidates
established an upper limit on the monopole flux of 5.6 ×
10-15 cm-2 sr-1 s-1 at 90% confidence level in the velocity
range of 10-4 ≃ β < 4 × 10-3. This result places a
new constraint on the abundance of monopoles trapped in our
solar system. © 1994 The American Physical
Society.},
Doi = {10.1103/physrevlett.72.608},
Key = {Ahlen94}
}
@booklet{Bernardini94,
Author = {Ahlen, S and Ambrosio, M and Antolini, R and Auriemma, G and Baker, R and Baldini, A and Barbarino, GC and Barish, BC and Battistoni, G and Bellotti, R and Bemporad, C and Bernardini, P and Bilokon, H and Bisi,
V and Bloise, C and Bower, C and Bussino, S and Cafagna, F and Calicchio,
M and Campana, D and Carboni, M and Cecchini, S and Cei, F and Chiarella,
V and Corona, A and Coutu, S and Cataldo, GD and Dekhissi, H and Marzo, CD and Vincenzi, MD and Credico, AD and Diehl, E and Erriquez, O and Favuzzi,
C and Forti, C and Fusco, P and Giacomelli, G and Giannini, G and Giglietto, N and Grassi, M and Green, P and Grillo, A and Guarino, F and Guarnaccia, P and Gustavino, C and Habig, A and Hanson, K and Heinz, R and Hong, JT and Iarocci, E and Katsavounidis, E and Kearns, E and Kyeizopoulou, S and Lamanna, E and Lane, C and Levin, D and Lipari, P and Liu, G and Liu, R and Longo, MJ and Lu, Y and Ludlam, G and Mancarella, G and Mandrioli, G and Margiotta-Neri, A and Marin, A and Marini, A and Martello, D and Marzari Chiesa and A and Mazziotta, MN and Michael, DG and Mikheyev, S and Miller, L and Mittelbrun, M and Monacelli, P and Monteno, M and Mufson, S and Musser, J and Nicoló, D and Nolty, R and Okada, C and Osteria, G and Palamara, O and Parlati, S and Patera, V and Patrizii, L and Pavesi, B and Pazzi, R and Peck, CW and Petrakis, J and Petrera, S and Pignatano, ND and Pistilli, P and Rainó, A and Reynoldson, J and Ronga, F and Sanzgiri, A and Satriano, C and Satta, L and Scapparone, E},
Title = {Muon astrophysics with the MACRO detector},
Journal = {Nuclear Physics B (Proceedings Supplements)},
Volume = {35},
Number = {C},
Pages = {229-234},
Publisher = {Elsevier BV},
Year = {1994},
Month = {January},
ISSN = {0920-5632},
url = {http://dx.doi.org/10.1016/0920-5632(94)90248-8},
Abstract = {Muon events collected with the streamer tube system of MACRO
have been used to study the vertical muon intensity and to
search for astrophysical point sources. New upper limits on
the muon fluxes coming from source candidates have been
obtained. The μ pair distance distribution and multimuon
rates are presented and compared with Monte Carlo
predictions for different primary cosmic rays composition
models. © 1994.},
Doi = {10.1016/0920-5632(94)90248-8},
Key = {Bernardini94}
}
@booklet{Navarra94,
Author = {NAVARRA, G and AHLEN, S and AMBROSIO, M and ANTOLINI, R and AURIEMMA, G and BAKER, R and BALDINI, A and BARBARINO, GC and BARISH, BC and BATTISTONI,
G and BELLOTTI, R and BEMPORAD, C and BERNARDINI, P and BILOKON, H and BISI, V and BLOISE, C and BOWER, C and BUSSINO, S and CAFAGNA, F and CALICCHIO, M and CAMPANA, D and CARBONI, M and CECCHINI, S and CEI, F and CHIARELLA, V and CORONA, A and COUTU, S and DECATALDO, G and DEKHISSI,
H and DEMARZO, C and DEVINCENZI, M and DICREDICO, A and DIEHL, E and ERRIQUEZ, O and FAVUZZI, C and FORTI, C and FUSCO, P and GIACOMELLI, G and GIANNINI, G and GIGLIETTO, N et al.},
Title = {Study of the cosmic ray primary composition at E0 ∼ 1000
TeV by EAS-TOP and MACRO at Gran Sasso},
Journal = {Nuclear Physics B - Proceedings Supplements},
Volume = {35},
Pages = {257-258},
Publisher = {Elsevier BV},
Year = {1994},
Month = {May},
ISSN = {0550-3213},
url = {http://gateway.webofknowledge.com/gateway/Gateway.cgi?GWVersion=2&SrcApp=PARTNER_APP&SrcAuth=LinksAMR&KeyUT=WOS:A1994NT28000044&DestLinkType=FullRecord&DestApp=ALL_WOS&UsrCustomerID=47d3190e77e5a3a53558812f597b0b92},
Doi = {10.1016/0920-5632(94)90255-0},
Key = {Navarra94}
}
@article{fds248750,
Author = {Ambrosio, M and Antolini, R and Auriemma, G and Baker, R and Baldini, A and Bam, B and Barbarino, GC and Barish, BC and Battistoni, G and Bellotti,
R and Bemporad, C and Bernardini, P and Bilokon, H and Bisi, V and Bloise,
C and Bower, C and Bussino, S and Cafagna, F and Calicchio, M and Campana,
D and Carboni, M and Corona, A and Cecchini, S and Cei, F and Chiarella, V and Cormack, R and Coutu, S and DeCataldo, G and Dekhissi, H and DeMarzo, C and De Vincenzi M, and Di Credico A, and Diehl, E and Erriquez, O and Favuzzi, C and Forti, C and Fusco, P and Giacomelli, G and Giannini, G and Giglietto, N and Grassi, M and Green, P and Grillo, A and Guarino, F and Guarnaccia, P and Gustavino, C and Habig, A and Heinz, R and Hong, JT and Iarocci, E and Katsavounidis, E and Kearns, E and Kertzman, M and Kyriazopoulou, S and Lamanna, E and Lane, C and Lee, C and Levin, DS and Lipari, P and Liu, G and Liu, R and Longo, MJ and Lu, Y and Ludlam,
G},
Title = {Coincident observation of air C-caronerenkov light by a
surface array and muon bundles by a deep underground
detector.},
Journal = {Physical review. D, Particles and fields},
Volume = {50},
Number = {5},
Pages = {3046-3058},
Year = {1994},
Month = {September},
ISSN = {0556-2821},
url = {http://dx.doi.org/10.1103/physrevd.50.3046},
Abstract = {We report on the simultaneous observation of atmospheric
erenkov light by a prototype five telescope array, GRACE,
(Gran Sasso Air erenkov Experiment) with deep underground
muons in the MACRO (Monopole Astrophysics and Cosmic Ray
Observatory). The telescope array was deployed at Campo
Imperatore above the Gran Sasso Laboratory for a run
completed in the fall of 1992. The total live time for the
combined surface-underground operation was ∼100 h during
which more than 300 events were seen in coincidence. The
efficacy of this technique to monitor the electromagnetic
and penetrating muon components of a cosmic-ray-induced
cascade is discussed. © 1994 The American Physical
Society.},
Doi = {10.1103/physrevd.50.3046},
Key = {fds248750}
}
@article{fds361718,
Author = {Collaboration, TMACRO and Hong, JT},
Title = {Multiple Muon Measurements with MACRO},
Year = {1994},
Month = {October},
Abstract = {The MACRO experiment at Gran Sasso provides means for
detailed studies of multiple coincident penetrating cosmic
ray muons. In this paper we concentrate on the studies of
the ultrahigh energy primary cosmic ray composition using
muon bundle multiplicities, muon pair lateral and angular
separation distributions.},
Key = {fds361718}
}
@booklet{Aglietta94,
Author = {Aglietta, M and Alessandro, B and Antonioli, P and Arneodo, F and Bergamasco, L and Bertaina, M and Fauth, AC and Castagnoli, C and Castellina, A and Cattadori, C and Chiavassa, A and Cini, G and D'Ettorre Piazzoli and B and Di Sciascio and G and Fulgione, W and Galeotti, P and Ghia, PL and Iacovacci, M and Mannocchi, G and Melagrana, C and Morello, C and Navarra, G and Riccati, L and Saavedra,
O and Trinchero, GC and Vallania, P and Vernetto, S and Ahlen, S and Ambrosio, M and Antolini, R and Auriemma, G and Baker, R and Baldini, A and Barbarino, GC and Barish, BC and Battistoni, G and Bellotti, R and Bemporad, C and Bernardini, P and Bilokon, H and Bisi, V and Bloise, C and Bower, C and Bussino, S and Cafagna, F and Calicchio, M and Campana, D and Carboni, M and Cecchini, S and Cei, F and Chiarella, V and Cormack, R and Corona, A and Coutu, S and DeCataldo, G and Dekhissi, H and DeMarzo, C and De Mitri and M and De Vincenzi and M and Di Credico and A and Diehl, E and Erriquez, O and Favuzzi, C and Ficenec, D and Forti, C and Fusco, P and Giacomelli, G and Giannini, G and Giglietto, N and Goretti, M and Grassi, M and Green, P and Grillo, A and Guarino, F and Guarnaccia, P and Gustavino, C and Habig, A and Hanson, K and Heinz, R and Hong, JT and Iarocci, E and Katsavounidis, E and Kearns, E and Klein, S and Kyriazopoulou, S and Lamanna, E and Lane, C and Levin, DS and Lipari, P and Liu, G and Liu, R and Longo, MJ and Lu, Y and Ludlam, G and Mancarella, G and Mandrioli, G and Margiotta-Neri, A and Marin, A and Marini, A and Martello, D},
Title = {Study of the primary cosmic ray composition around the knee
of the energy spectrum},
Journal = {Physics Letters B},
Volume = {337},
Number = {3-4},
Pages = {376-382},
Publisher = {Elsevier BV},
Year = {1994},
Month = {October},
ISSN = {0370-2693},
url = {http://gateway.webofknowledge.com/gateway/Gateway.cgi?GWVersion=2&SrcApp=PARTNER_APP&SrcAuth=LinksAMR&KeyUT=WOS:A1994PL95300023&DestLinkType=FullRecord&DestApp=ALL_WOS&UsrCustomerID=47d3190e77e5a3a53558812f597b0b92},
Abstract = {A study of the primary cosmic ray composition in the energy
range 5ṡ1014-5ṡ1015 eV is performed through the analysis
of the deep underground muons and of the e.m. component of
Extensive Air Showers detected in coincidence by the MACRO
and EAS-TOP experiments at the Gran Sasso Laboratory. We
conclude that: a) pure proton and Iron primary beams are
excluded by the experimental data; b) a fraction of nuclei
heavier than Helium is necessary to explain the experimental
data both below and above the knee; c) a mixed composition,
obtained a priori from extrapolations of the spectra
directly measured below 100 TeV, yields a reasonable account
of the observations up to the knee of the primary spectrum.
© 1994.},
Doi = {10.1016/0370-2693(94)90991-1},
Key = {Aglietta94}
}
@booklet{Ambrosio95a,
Author = {Ambrosio, M and Antolini, R and Auriemma, G and Baker, R and Baldini, A and Barbarino, GC and Barish, BC and Battistoni, G and Bellotti, R and Bemporad, C and Bernardini, P and Bilokon, H and Bisi, V and Bloise, C and Bower, C and Bussino, S and Cafagna, F and Calicchio, M and Campana, D and Carboni, M and Castellano, M and Cecchini, S and Cei, F and Chiarella,
V and Corona, A and Coutu, S and De Cataldo and G and Dekhissi, H and De
Marzo, C and De Mitri and I and De Vincenzi and M and Di Credico and A and Erriquez, O and Favuzzi, C and Forti, C and Fusco, P and Giacomelli, G and Giannini, HG and Giglietto, N and Goretti, M and Grassi, M and Grillo,
A and Guarino, F and Guarnaccia, P and Gustavino, C and Habig, A and Hanson, K and Hawthorne, A and Heinz, R and Hong, JT and Iarocci, E and Katsavounidis, E and Kearns, E and Kyriazopoulou, S and Lamanna, E and Eane, C and Levin, DS and Lipari, P and Liu, R and Longley, NP and Longo,
MJ and Lu, Y and Ludlam, G and Mancarella, G and Mandrioli, G and Margiotta-Neri, A and Marini, A and Martello, D and Marzari-Chiesa,
A and Mazziotta, MN and Michael, DG and Mikheyev, S and Miller, L and Mittelbrunn, M and Monacelli, P and Montaruli, T and Monteno, M and Mufson, S and Musser, J and Nicoló, D and Nolty, R and Okada, C and Orth,
C and Osteria, G and Palamara, O and Parlati, S and Patera, V and Patrizii,
L and Pazzi, R and Peck, CW and Petrera, S and Pignatano, ND and Pistilli,
P and Popa, V and Rainó, A and Reynoldson, J and Ronga, F and Rubizzo, U and Sanzgiri, A and Sartogo, F},
Title = {Performance of the MACRO streamer tube system in the search
for magnetic monopoles},
Journal = {Astroparticle Physics},
Volume = {4},
Number = {1},
Pages = {33-43},
Publisher = {Elsevier BV},
Year = {1995},
Month = {January},
ISSN = {0927-6505},
url = {http://gateway.webofknowledge.com/gateway/Gateway.cgi?GWVersion=2&SrcApp=PARTNER_APP&SrcAuth=LinksAMR&KeyUT=WOS:A1995TA34600004&DestLinkType=FullRecord&DestApp=ALL_WOS&UsrCustomerID=47d3190e77e5a3a53558812f597b0b92},
Abstract = {We describe the techniques chosen to search tor magnetic
monopoles using the MACRO streamer tube sub-system. The
hardware and the details of the analysis procedures will be
discussed also. The results for slowly moving monopoles are
reported from a first data taking period using only part of
the detector. © 1995 Elsevier Science B.V. All rights
reserved.},
Doi = {10.1016/0927-6505(95)00023-A},
Key = {Ambrosio95a}
}
@booklet{Ahlen95,
Author = {Ahlen, S and Ambrosio, M and Antolini, R and Auriemma, G and Baker, R and Baldini, A and Barbarino, GC and Barish, BC and Battistoni, G and Bellotti, R and Bemporad, C and Bernardini, P and Bilokon, H and Bisi,
V and Bloise, C and Bower, C and Bussino, S and Cafagna, F and Calicchio,
M and Campana, D and Carboni, M and Castellano, M and Cecchini, S and Cei,
F and Celio, P and Chiarella, V and Cormack, R and Corona, A and Coutu, S and De Cataldo and G and Dekhissi, H and De Marzo and C and Diehl, E and De Mitri,
I and De Vincenzi and M and Di Credico and A and Erriquez, O and Favuzzi, C and Forti, C and Fusco, P and Giacomelli, G and Giannini, G and Giglietto,
N and Grassi, M and Green, P and Grillo, A and Guarino, F and Guarnaccia,
P and Gustavino, C and Habig, A and Hanson, K and Hawthorne, A and Heinz,
R and Hong, JT and Iarocci, E and Katsavounidis, E and Kearns, E and Kyriazopoulou, S and Lamanna, E and Lane, C and Levin, DS and Lipari, P and Liu, G and Liu, R and Longley, NP and Longo, MJ and Lu, Y and Ludlam, G and Mancarella, G and Mandrioli, G and Margiotta-Neri, A and Marin, A and Marini, A and Martello, D and Marzari-Chiesa, A and Mazziotta, MN and Michael, DG and Mikheyev, S and Miller, L and Mittelbrunn, M and Monacelli, P and Montaruli, T and Monteno, M and Mufson, S and Musser,
J and Nicoló, D and Nolty, R and Nutter, S and Okada, C and Orth, C and Osteria, G and Palamara, O and Parlati, S and Patera, V and Patrizii, L and Pazzi, R and Peck, CW and Petrakis, J and Petrera, S and Pignatano,
ND},
Title = {Atmospheric neutrino flux measurement using upgoing
muons},
Journal = {Physics Letters B},
Volume = {357},
Number = {3},
Pages = {481-486},
Publisher = {Elsevier BV},
Year = {1995},
Month = {September},
ISSN = {0370-2693},
url = {http://dx.doi.org/10.1016/0370-2693(95)00958-N},
Abstract = {We report on the first measurement of the flux of upgoing
muons resulting from interactions of atmospheric neutrinos
in the rock below MACRO. The ratio of the observed to the
expected number of events integrated over all nadir angles
is 0.73 ± .09stat. ± .06sys. ± .12theor.. The flux of
upgoing muons as a function of nadir angle is presented and
compared to Monte Carlo expectations. At the 90% confidence
level, the data are consistent with no neutrino oscillations
or some possible oscillation hypothese with the parameters
suggested by the Kamiokande contained-event analysis. ©
1995.},
Doi = {10.1016/0370-2693(95)00958-N},
Key = {Ahlen95}
}
@booklet{Ambrosio95,
Author = {Ambrosio, M and Antolini, R and Auriemma, G and Baker, R and Baldini, A and Barbarino, GC and Barish, BC and Battistoni, G and Bellotti, R and Bemporad, C and Bernardini, P and Bilokon, H and Bisi, V and Bloise, C and Bower, C and Bussino, S and Cafagna, F and Calicchio, M and Campana, D and Carboni, M and Castellano, M and Cecchini, S and Cei, F and Celio, P and Chiarella, V and Corona, A and Coutu, S and De Cataldo G, and Dekhissi,
H and De Marzo C, and De Mitri I, and De Vincenzi M, and Di Credico
A, and Erriquez, O and Favuzzi, C and Forti, C and Fusco, P and Giacomelli, G and Giannini, G and Giglietto, N and Grassi, M and Grillo,
A and Guarino, F and Guarnaccia, P and Gustavino, C and Habig, A and Hanson, K and Hawthorne, A and Heinz, R and Hong, JT and Iarocci, E and Katsavounidis, E and Kearns, E and Kyriazopoulou, S and Lamanna, E and Lane, C and Levin, DS and Lipari, P and Liu, R and Longley, NP and Longo,
MJ and Lu, Y and Ludlam, G and Mancarella, G},
Title = {Vertical muon intensity measured with MACRO at the Gran
Sasso laboratory.},
Journal = {Physical review. D, Particles and fields},
Volume = {52},
Number = {7},
Pages = {3793-3802},
Year = {1995},
Month = {October},
ISSN = {0556-2821},
url = {http://dx.doi.org/10.1103/physrevd.52.3793},
Abstract = {The vertical underground muon intensity has been measured in
the slant depth range 3200-7000 hg cm-2 (standard rock) with
the completed lower part of the MACRO detector at the Gran
Sasso laboratory, using a large sample of data. These
observations are used to compute the surface muon flux and
the primary ''all-nucleon'' spectrum. An analysis of
systematic uncertainties introduced by the interaction
models in the atmosphere and the underground propagation of
muons is presented. A comparison of our results with
published data is also presented. © 1995 The American
Physical Society.},
Doi = {10.1103/physrevd.52.3793},
Key = {Ambrosio95}
}
@booklet{Ambrosio96a,
Author = {Ambrosio, M and Antolini, R and Auriemma, G and Baker, R and Baldini, A and Barbarino, GC and Barish, BC and Battistoni, G and Bellotti, R and Bemporad, C and Bernardini, P and Bilokon, H and Bisi, V and Bloise, C and Bosio, T and Bower, C and Bussino, S and Cafagna, F and Calicchio, M and Campana, D and Carboni, M and Castellano, M and Cecchini, S and Cei, F and Chiarella, V and Corona, A and Coutu, S and DeCataldo, G and Dekhissi,
H and DeMarzo, C and De Mitri and I and DeVincenzi, M and DiCredico, A and Erriquez, O and Fantini, R and Favuzzi, C and Forti, C and Fusco, P and Giacomelli, G and Giannini, G and Giglietto, N and Goretti, M and Grassi, M and Grillo, A and Guarino, F and Guamaccia, P and Gustavino,
C and Habig, A and Hanson, K and Hawthorne, A and Heinz, R and Hong, JT and Iarocci, E and Katsavounidis, E and Kearns, E and Kyriazopoulou, S and Lamanna, E and Lane, C and Levin, DS and Lipari, P and Liu, G and Liu, R and Longley, NP and Longo, MJ and Lu, Y and Ludlam, G and Mancarella, G and Mandrioli, G and MargiottaNeri, A and Marini, A and Martello, D and MarzariChiesa, A and Mazziotta, MN and Michael, DG and Mikheyev, S and Miller, L and Mittelbrunn, M and Monacelli, P and Montaruli, T and Monteno, M and Mufson, S and Musser, J and Nicolo, D and Nolty, R and Okada, C and Orth, C and Osteria, G and Palamara, O and Parlati, S and Patera, V and Patrizii, L and Pazzi, R and Peck, CW and Petrera, S and Pignatano, ND and Pistilli, P and Popa, V and Raino, A and Reynoldson,
J and Ronga, F and Rubizzo, U and Sanzgiri, A and Sartogo, F and Satriano,
C and Satta, L and Scapparone, E and Scholberg, K and Sciubba, A and SerraLugaresi, P and Severi, M and Sitta, M and Spada, PF and Spinelli,
P and Spinetti, M and Spurio, M and Steinberg, R and Stone, JL and Sulak,
LR and Surdo, A and Tarle, G and Togo, V and Valente, V and Walter, CW and Webb, R},
Title = {Study of primary interactions with multiple muons in
MACRO},
Journal = {NUCLEAR PHYSICS B},
Pages = {447-449},
Year = {1996},
ISSN = {0550-3213},
url = {http://gateway.webofknowledge.com/gateway/Gateway.cgi?GWVersion=2&SrcApp=PARTNER_APP&SrcAuth=LinksAMR&KeyUT=WOS:A1996UN01900093&DestLinkType=FullRecord&DestApp=ALL_WOS&UsrCustomerID=47d3190e77e5a3a53558812f597b0b92},
Key = {Ambrosio96a}
}
@booklet{Ambrosio96,
Author = {Ambrosio, M and Antolini, R and Auriemma, G and Baker, R and Baldini, A and Barbarino, GC and Barish, BC and Battistoni, G and Bellotti, R and Bemporad, C and Bernardini, P and Bilokon, H and Bisi, V and Bloise, C and Bosio, T and Bower, C and Bussino, S and Cafagna, F and Calicchio, M and Campana, D and Carboni, M and Castellano, M and Cecchini, S and Cei, F and Chiarella, V and Corona, A and Coutu, S and DeCataldo, G and Dekhissi,
H and DeMarzo, C and De Mitri and I and DeVincenzi, M and DiCredico, A and Erriquez, O and Fantini, R and Favuzzi, C and Forti, C and Fusco, P and Giacomelli, G and Giannini, G and Giglietto, N and Goretti, M and Grassi, M and Grillo, A and Guarino, F and Guamaccia, P and Gustavino,
C and Habig, A and Hanson, K and Hawthorne, A and Heinz, R and Hong, JT and Iarocci, E and Katsavounidis, E and Kearns, E and Kyriazopoulou, S and Lamanna, E and Lane, C and Levin, DS and Lipari, P and Liu, G and Liu, R and Longley, NP and Longo, MJ and Lu, Y and Ludlam, G and Mancarella, G and Mandrioli, G and Neri, AM and Marini, A and Martello, D and MarzariChiesa, A and Mazziotta, MN and Michael, DG and Mikheyev, S and Miller, L and Mittelbrunn, M and Monacelli, P and Montaruli, T and Monteno, M and Mufson, S and Musser, J and Nicolo, D and Nolty, R and Okada, C and Orth, C and Osteria, G and Palamara, O and Parlati, S and Patera, V and Patrizii, L and Pazzi, R and Peck, CW and Petrera, S and Pignatano, ND and Pistilli, P and Popa, V and Raino, A and Reynoldson,
J and Ronga, F and Rubizzo, U and Sanzgiri, A and Sartogo, F and Satriano,
C and Satta, L and Scapparone, E and Scholberg, K and Sciubba, A and SerraLugaresi, P and Severi, M and Sitta, M and Spada, PF and Spinelli,
P and Spinetti, M and Spurio, M and Steinberg, R and Stone, JL and Sulak,
LR and Surdo, A and Tarle, G and Togo, V and Valente, V and Walter, CW and Webb, R},
Title = {Search for neutrinos from the Sun and the Earth with the
MACRO detector},
Journal = {NUCLEAR PHYSICS B},
Pages = {87-90},
Year = {1996},
ISSN = {0550-3213},
url = {http://gateway.webofknowledge.com/gateway/Gateway.cgi?GWVersion=2&SrcApp=PARTNER_APP&SrcAuth=LinksAMR&KeyUT=WOS:A1996UN01900021&DestLinkType=FullRecord&DestApp=ALL_WOS&UsrCustomerID=47d3190e77e5a3a53558812f597b0b92},
Key = {Ambrosio96}
}
@booklet{Ambrosio97a,
Author = {Ambrosio, M and Antolini, R and Auriemma, G and Baker, R and Baldini, A and Barbarino, GC and Barish, BC and Battistoni, G and Bellotti, R and Bemporad, C and Bernardini, P and Bilokon, H and Bisi, V and Bloise, C and Bosio, T and Bower, C and Bussino, S and Cafagna, F and Calicchio, M and Campana, D and Carboni, M and Castellano, M and Cecchini, S and Cei, F and Chiarella, V and Corona, A and Coutu, S and De Cataldo and G and Dekhissi,
H and De Marzo and C and De Mitri and I and De Vincenzi and M and Di Credico and A and Erriquez, O and Fantini, R and Favuzzi, C and Forti, C and Fusco, P and Giacomelli, G and Giannini, G and Giglietto, N and Goretti, M and Grassi, M and Grillo, A and Guarino, F and Guarnaccia, P and Gustavino,
C and Habig, A and Hanson, K and Hawthorne, A and Heinz, R and Hong, JT and Iarocci, E and Katsavounidis, E and Kearns, E and Kyriazopoulou, S and Lamanna, E and Lane, C and Levin, DS and Lipari, P and Longley, NP and Longo, MJ and Mancarella, G and Mandrioli, G and Margiotta-Neri, A and Marini, A and Martello, D and Marzari-Chiesa, A and Mazziotta, MN and Michael, DG and Mikheyev, S and Miller, L and Monacelli, P and Montaruli, T and Monteno, M and Mufson, S and Musser, J and Nicoló, D and Nolty, R and Okada, C and Orth, C and Osteria, G and Palamara, O and Parlati, S and Patera, V and Patrizii, L and Pazzi, R and Peck, CW and Petrera, S and Pistilli, P and Popa, V and Rainó, A and Reynoldson, J and Ricciardi, M and Ronga, F and Rubizzo, U and Sanzgiri, A and Sartogo, F and Satriano, C and Satta, L},
Title = {High energy cosmic ray physics with underground muons in
MACRO. I. Analysis methods and experimental
results},
Journal = {Physical Review D - Particles, Fields, Gravitation and
Cosmology},
Volume = {56},
Number = {3},
Pages = {1407-1417},
Publisher = {American Physical Society (APS)},
Year = {1997},
Month = {January},
ISSN = {0556-2821},
url = {http://dx.doi.org/10.1103/PhysRevD.56.1407},
Abstract = {In this paper, the first of a two-part work, we present the
reconstruction and measurement of muon events detected
underground by the MACRO experiment at Gran Sasso [Formula
presented] 1.3 TeV in atmosphere). The main aim of this work
is to discuss the muon multiplicity distribution as measured
in the detector. The data sample analyzed consists of
[Formula presented] muon events, of which [Formula
presented] 263 000 are multiple muons, corresponding to a
total live time of 5850 h. In this sample, the observed
multiplicities extend above [Formula presented]=35, with
intermuon separations up to 50 m and beyond. Additional
complementing measurements, such as the inclusive muon flux,
the angular distribution, and the muon separation
distribution (decoherence), are also included. The physical
interpretation of the results presented here is reported in
the following companion paper. © 1997 The American Physical
Society.},
Doi = {10.1103/PhysRevD.56.1407},
Key = {Ambrosio97a}
}
@booklet{Ambrosio97b,
Author = {Ambrosio, M and Antolini, R and Auriemma, G and Baker, R and Baldini, A and Barbarino, GC and Barish, BC and Battistoni, G and Bellotti, R and Bemporad, C and Bernardini, P and Bilokon, H and Bisi, V and Bloise, C and Bosio, T and Bower, C and Bussino, S and Cafagna, F and Calicchio, M and Campana, D and Carboni, M and Castellano, M and Cecchini, S and Cei, F and Chiarella, V and Corona, A and Coutu, S and De Cataldo and G and Dekhissi,
H and De Marzo and C and De Mitri and I and De Vincenzi and M and Di Credico and A and Erriquez, O and Fantini, R and Favuzzi, C and Forti, C and Fusco, P and Giacomelli, G and Giannini, G and Giglietto, N and Goretti, M and Grassi, M and Grillo, A and Guarino, F and Guarnaccia, P and Gustavino,
C and Habig, A and Hanson, K and Hawthorne, A and Heinz, R and Hong, JT and Iarocci, E and Katsavounidis, E and Kearns, E and Kyriazopoulou, S and Lamanna, E and Lane, C and Levin, DS and Lipari, P and Longley, NP and Longo, MJ and Mancarella, G and Mandrioli, G and Margiotta-Neri, A and Marini, A and Martello, D and Marzari-Chiesa, A and Mazziotta, MN and Michael, DG and Mikheyev, S and Miller, L and Monacelli, P and Montaruli, T and Monteno, M and Mufson, S and Musser, J and Nicoló, D and Nolty, R and Okada, C and Orth, C and Osteria, G and Palamara, O and Parlati, S and Patera, V and Patrizii, L and Pazzi, R and Peck, CW and Petrera, S and Pistilli, P and Popa, V and Rainó, A and Reynoldson, J and Ricciardi, M and Ronga, F and Rubizzo, U and Sanzgiri, A and Sartogo, F and Satriano, C and Satta, L},
Title = {High energy cosmic ray physics with underground muons in
MACRO. II. Primary spectra and composition},
Journal = {Physical Review D - Particles, Fields, Gravitation and
Cosmology},
Volume = {56},
Number = {3},
Pages = {1418-1436},
Publisher = {American Physical Society (APS)},
Year = {1997},
Month = {January},
ISSN = {0556-2821},
url = {http://dx.doi.org/10.1103/PhysRevD.56.1418},
Abstract = {Multimuon data from the MACRO experiment at Gran Sasso have
been analyzed using a new method, which allows one to
estimate the primary cosmic ray fluxes. The estimated
all-particle spectrum is higher and flatter than the one
obtained from direct measurements but is consistent with EAS
array measurements. The spectral indexes of the fitted
energy spectrum are 2.56[Formula presented]0.05 for [Formula
presented]500 TeV and 2.9[Formula presented]0.3 for [Formula
presented]5000 TeV with a gradual change at intermediate
energies. The average mass number shows little dependence on
the primary energy below 1000 TeV, with a value of
10.1[Formula presented]2.5 at 100 TeV. At higher energies
the best fit average mass shows a mild increase with energy,
even though no definite conclusion can be reached taking
into account errors. The fitted spectra cover a range from
[Formula presented] 50 TeV up to several thousand TeV. ©
1997 The American Physical Society.},
Doi = {10.1103/PhysRevD.56.1418},
Key = {Ambrosio97b}
}
@booklet{Ambrosio97c,
Author = {Ambrosio, M and Antolini, R and Auriemma, G and Baker, R and Baldini, A and Barbarino, GC and Barish, BC and Battistoni, G and Bellotti, R and Bemporad, C and Bernardini, P and Bilokon, H and Bisi, V and Bloise, C and Bosio, T and Bower, C and Bussino, S and Cafagna, F and Calicchio, M and Campana, D and Carboni, M and Castellano, M and Cecchini, S and Cei, F and Chiarella, V and Corona, A and Coutu, S and de Benedictis, L and de
Cataldo, G and Dekhissi, H and de Marzo, C and de Mitri, I and de
Vincenzi, M and di Credico, A and Erriquez, O and Fantini, R and Favuzzi, C and Forti, C and Fusco, P and Giacomelli, G and Giannini, G and Giglietto, N and Goretti, M and Grassi, M and Green, P and Grillo, A and Guarino, F and Guarnaccia, P and Gustavino, C and Habig, A and Hanson,
K and Hawthorne, A and Heinz, R and Hong, JT and Iarocci, E and Katsavounidis, E and Kearns, E and Kyriazopoulou, S and Lamanna, E and Lane, C and Levin, DS and Lipari, P and Liu, G and Liu, R and Longley, NP and Longo, MJ and Ludlam, G and Maaroufi, F and Mancarella, G and Mandrioli,
G and Margiotta-Neri, A and Marini, A and Martello, D and Marzari-Chiesa, A and Mazziotta, MN and Michael, DG and Mikheyev, S and Miller, L and Monacelli, P and Montaruli, T and Monteno, M and Mufson,
S and Musser, J and Nicoló, D and Nolty, R and Okada, C and Orth, C and Osteria, G and Paganini, S and Palamara, O and Parlati, S and Patera, V and Patrizii, L and Pazzi, R and Peck, CW and Petrera, S and Pignatano, ND and Pistilli, P and Popa, V and Rainó, A},
Title = {Seasonal variations in the underground muon intensity as
seen by MACRO},
Journal = {Astroparticle Physics},
Volume = {7},
Number = {1-2},
Pages = {109-124},
Publisher = {Elsevier BV},
Year = {1997},
Month = {January},
ISSN = {0927-6505},
url = {http://dx.doi.org/10.1016/S0927-6505(97)00011-X},
Abstract = {Using 5.33 × 106 single muons collected in 1.46 × 104 live
hours by MACRO during the period 1991-1994, we have searched
for a correlation between variations in the underground muon
rate, Νμ, and seasonal temperature variations in the
atmosphere. These correlations are found to be present with
high statistical significance. Analysis of the relatively
complete December 1992-December 1994 subset of the data
yields a value for the temperature coefficient, αΤ =
(Τ/Νμ)(∂Nu;μ/∂Tau;) = 0.83 ± 0.13. Analysis of the
total data set gives consistent results. We have compared
this result with the hypothesis that the muons observed in
MACRO come from pion decays alone. Although our result is
consistent with the 'pion only' hypothesis, a discussion of
the sensitivity of our data sample to the kaon component of
the cascades leading to observed muons underground will also
be presented. © 1997 Elsevier Science B.V.},
Doi = {10.1016/S0927-6505(97)00011-X},
Key = {Ambrosio97c}
}
@booklet{Ambrosio97e,
Author = {Ambrosio, M and Antolini, R and Auriemma, G and Baker, R and Baldini, A and Barbarino, GC and Barish, BC and Battistoni, G and Bellotti, R and Bemporad, C and Bernardini, P and Bilokon, H and Bisi, V and Bloise, C and Bosio, T and Bower, C and Bussino, S and Cafagna, R and Calicchio, M and Campana, D and Carboni, M and Castellano, M and Cecchini, S and Cei, F and Chiarella, V and Corona, A and Coutu, S and De Cataldo and G and Dekhissi,
H and De Marzo and C and De Mitri and I and De Vincenzi and M and Di Credico and A and Erriquez, O and Fantini, R and Favuzzi, C and Forti, C and Fusco, P and Giacomelli, G and Giannini, G and Giglietto, N and Goretti, M and Grassi, M and Green, P and Grillo, A and Guarino, F and Guarnaccia, P and Gustavino, C and Habig, A and Hanson, K and Hawthorne, A and Heinz, R and Hong, JT and Iarocci, E and Katsavounidis, E and Kearns, E and Kyriazopoulou, S and Lamanna, E and Lane, C and Levin, DS and Lipari, P and Liu, G and Liu, R and Longley, NP and Longo, MJ and Ludlam, G and Mancarella, G and Mandrioli, G and Margiotta-Neri, A and Marini, A and Martello, D and Marzari-Chiesa, A and Mazziotta, MN and Michael, DG and Mikheyev, S and Miller, L and Monacelli, P and Montaruli, T and Monteno,
M and Mufson, S and Musser, J and Nicoló, D and Nolty, R and Okada, C and Orth, C and Osteria, G and Palamara, O and Parlati, S and Patera, V and Patrizii, L and Pazzi, R and Peck, CW and Petrera, S and Pignatano, ND and Pistilli, P and Popa, V and Rainó, A and Reynoldson, J and Ronga, F and Rubizzo, U and Sanzgiri, A and Sartogo, F and Satriano, C and Satta, L and Scapparone, E and Scholberg, K and Sciubba, A and Serra-Lugaresi, P and Severi, M and Sinev, V and Sitta, M and Spinelli, P and Spinetti, M and Spurio, M and Steinberg, R and Stone, JL and Sulak, LR and Surdo, A and Tarlé, G and Togo, V and Valente, V and Walter, CW and Webb,
R},
Title = {The performance of MACRO liquid scintillator in the search
for magnetic monopoles with 10−3 < β <
1},
Journal = {Astroparticle Physics},
Volume = {6},
Number = {2},
Pages = {113-128},
Publisher = {Elsevier BV},
Year = {1997},
Month = {February},
ISSN = {0927-6505},
url = {http://gateway.webofknowledge.com/gateway/Gateway.cgi?GWVersion=2&SrcApp=PARTNER_APP&SrcAuth=LinksAMR&KeyUT=WOS:A1997WJ60800001&DestLinkType=FullRecord&DestApp=ALL_WOS&UsrCustomerID=47d3190e77e5a3a53558812f597b0b92},
Doi = {10.1016/s0927-6505(96)00048-5},
Key = {Ambrosio97e}
}
@booklet{Ambrosio97d,
Author = {Ambrosio, M and Antolini, R and Auriemma, G and Baker, R and Baldini, A and Barbarino, GC and Barish, BC and Battistoni, G and Bellotti, R and Bemporad, C and Bernardini, P and Bilokon, H and Bisi, V and Bloise, C and Bosio, T and Bower, C and Bussino, S and Cafagna, F and Calicchio, M and Campana, D and Carboni, M and Castellano, M and Cecchini, S and Cei, F and Chiarella, V and Corona, A and Coutu, S and De Cataldo and G and Dekhissi,
H and De Marzo and C and De Mitri and I and De Vincenzi and M and Di Credico and A and Erriquez, O and Fantini, R and Favuzzi, C and Forti, C and Fusco, P and Giacomelli, G and Giannini, G and Giglietto, N and Goretti, M and Grassi, M and Grillo, A and Guarino, F and Guarnaccia, P and Gustavino,
C and Habig, A and Hanson, K and Hawthorne, A and Heinz, R and Hong, JT and Iarocci, E and Katsavounidis, E and Kearns, E and Kyriazopoulou, S and Lamanna, E and Lane, C and Levin, DS and Lipari, P and Longley, NP and Longo, MJ and Mancarella, G and Mandrioli, G and Margiotta-Neri, A and Marini, A and Martello, D and Marzari-Chiesa, A and Mazziotta, MN and Michael, DG and Mikheyev, S and Miller, L and Monacelli, P and Montaruli, T and Monteno, M and Mufson, S and Musser, J and Nicoló, D and Nolty, R and Okada, C and Orth, C and Osteria, G and Palamara, O and Parlati, S and Patera, V and Patrizii, L and Pazzi, R and Peck, CW and Petrera, S and Pistilli, P and Popa, V and Rainó, A and Reynoldson, J and Ronga, F and Rubizzo, U and Sanzgiri, A and Sartogo, F and Satriano, C and Satta, L and Scapparone, E and Scholberg, K and Sciubba, A and Serra-Lugaresi, P and Severi, M and Sitta, M and Spinelli, P and Spinetti, M and Spurio, M and Steinberg, R and Stone, JL and Sulak, LR and Surdo, A and Tarlé, G and Togo, V and Valente, V and Walter, CW and Webb,
R},
Title = {High energy cosmic ray physics with the MACRO experiment at
Gran Sasso},
Journal = {Nuclear Physics B - Proceedings Supplements},
Volume = {52},
Number = {3},
Pages = {172-175},
Publisher = {Elsevier BV},
Year = {1997},
Month = {February},
ISSN = {0550-3213},
url = {http://gateway.webofknowledge.com/gateway/Gateway.cgi?GWVersion=2&SrcApp=PARTNER_APP&SrcAuth=LinksAMR&KeyUT=WOS:A1997WW40500032&DestLinkType=FullRecord&DestApp=ALL_WOS&UsrCustomerID=47d3190e77e5a3a53558812f597b0b92},
Doi = {10.1016/s0920-5632(96)00869-9},
Key = {Ambrosio97d}
}
@booklet{Ambrosio97,
Author = {Ambrosio, M and Antolini, R and Auriemma, G and Baker, R and Baldini, A and Barbarino, GC and Barish, BC and Battistoni, G and Bellotti, R and Bemporad, C and Bernardini, P and Bilokon, H and Bisi, V and Bloise, C and Bosio, T and Bower, C and Bussino, S and Cafagna, F and Calicchio, M and Campana, D and Carboni, M and Castellano, M and Cecchini, S and Cei, F and Chiarella, V and Corona, A and Coutu, S and de Cataldo, G and Dekhissi,
H and de Marzo, C and de Mitri, I and de Vincenzi, M and di Credico, A and Erriquez, O and Fantini, R and Favuzzi, C and Forti, C and Fusco, P and Giacomelli, G and Giannini, G and Giglietto, N and Goretti, M and Grassi, M and Gray, L and Green, P and Grillo, A and Guarino, F and Guarnaccia, P and Gustavino, C and Habig, A and Hanson, K and Hawthorne,
A and Heinz, R and Hong, JT and Iarocci, E and Katsavounidis, E and Kearns,
E and Kyriazopoulou, S and Lamanna, E and Lane, C and Levin, DS and Lipari,
P and Liu, G and Liu, R and Longley, NP and Longo, MJ and Ludlam, G and Mancarella, G and Mandrioli, G and Margiotta Neri and A and Marini, A and Martello, D and Marzari-Chiesa, A and Mazziotta, MN and Michael, DG and Mikheyev, S and Miller, L and Monacelli, P and Montaruli, T and Monteno,
M and Mufson, S and Musser, J and Nicoló, D and Nolty, R and Okada, C and Orth, C and Osteria, G and Palamara, O and Parlati, S and Patera, V and Patrizii, L and Pazzi, R and Peck, CW and Petrera, S and Pignatano, ND and Pistilli, P and Popa, V and Rainó, A and Reynoldson, J and Ronga,
F},
Title = {Magnetic monopole search with the MACRO detector at Gran
Sasso},
Journal = {Physics Letters, Section B: Nuclear, Elementary Particle and
High-Energy Physics},
Volume = {406},
Number = {3},
Pages = {249-255},
Publisher = {Elsevier BV},
Year = {1997},
Month = {August},
ISSN = {0370-2693},
url = {http://dx.doi.org/10.1016/S0370-2693(97)00684-9},
Abstract = {In this letter we present the results of the search for
massive magnetic monopoles in the penetrating cosmic ray
radiation using the various subdetectors of the MACRO
apparatus, during the period 1989-1995. Flux limits are
given for the β = v/c range 4 × 10-5 < β < 1; for 10-4 <
β < 10-1 the limits are below the Parker bound, ∼ 10-15
cm-2s-1sr-1. © 1997 Published by Elsevier Science
B.V.},
Doi = {10.1016/S0370-2693(97)00684-9},
Key = {Ambrosio97}
}
@article{fds248726,
Author = {Fukuda, Y and Hayakawa, T and Ichihara, E and Inoue, K and Ishihara, K and Ishino, H and Itow, Y and Kajita, T and Kameda, J and Kasuga, S and Kobayashi, K and Kobayashi, Y and Koshio, Y and Martens, K and Miura, M and Nakahata, M and Nakayama, S and Okada, A and Oketa, M and Okumura, K and Ota, M and Sakurai, N and Shiozawa, M and Suzuki, Y and Takeuchi, Y and Totsuka, Y and Yamada, S and Earl, M and Habig, A and Hong, JT and Kearns,
E and Kim, SB and Masuzawa, M and Messier, MD and Scholberg, K and Stone,
JL and Sulak, LR and Walter, CW and Goldhaber, M and Barszczak, T and Gajewski, W and Halverson, PG and Hsu, J and Kropp, WR and Price, LR and Reines, F and Sobel, HW and Vagins, MR and Ganezer, KS and Keig, WE and Ellsworth, RW and Tasaka, S and Flanagan, JW and Kibayashi, A and Learned, JG and Matsuno, S and Stenger, V and Takemori, D and Ishii, T and Kanzaki, J and Kobayashi, T and Nakamura, K and Nishikawa, K and Oyama,
Y and Sakai, A and Sakuda, M and Sasaki, O and Echigo, S and Kohama, M and Suzuki, AT and Haines, TJ and Blaufuss, E and Sanford, R and Svoboda, R and Chen, ML and Conner, Z and Goodman, JA and Sullivan, GW and Mori, M and Goebel, F and Hill, J and Jung, CK and Mauger, C and McGrew, C and Sharkey,
E and Viren, B and Yanagisawa, C and Doki, W and Ishizuka, T and Kitaguchi,
Y and Koga, H and Miyano, K and Okazawa, H and Saji, C and Takahata, M and Kusano, A and Nagashima, Y and Takita, M and Yamaguchi, T and Yoshida,
M and Etoh, M and Fujita, K and Hasegawa, A and Hasegawa, T and Hatakeyama,
S and Iwamoto, T and Kinebuchi, T and Koga, M and Maruyama, T and Ogawa, H and Saito, M and Suzuki, A and Tsushima, F and Koshiba, M and Nemoto, M and Nishijima, K and Futagami, T and Hayato, Y and Kanaya, Y and Kaneyuki,
K and Watanabe, Y and Kielczewska, D and Doyle, R and George, J and Stachyra, A and Wai, L and Wilkes, J and Young, K},
Title = {Measurement of a small atmospheric νμ/νe
ratio},
Journal = {Physics Letters, Section B: Nuclear, Elementary Particle and
High-Energy Physics},
Volume = {433},
Number = {1-2},
Pages = {9-18},
Year = {1998},
ISSN = {0370-2693},
Abstract = {From an exposure of 25.5 kiloton-years of the
Super-Kamiokande detector, 900 muon-like and 983
electron-like single-ring atmospheric neutrino interactions
were detected with momentum pe > 100 MeV/c, pμ > 200
MeV/c, and with visible energy less than 1.33 GeV. Using a
detailed Monte Carlo simulation, the ratio
(μ/e)DATA/(μ/e)MC was measured to be 0.61 ± 0.03(stat.)
± 0.05(sys.), consistent with previous results from the
Kamiokande, IMB and Soudan-2 experiments, and smaller than
expected from theoretical models of atmospheric neutrino
production. © 1998 Published by Elsevier Science B.V. All
rights reserved.},
Key = {fds248726}
}
@article{fds248725,
Author = {Giglietto, N and Ambrosio, M and Antolini, R and Auriemma, G and Baker,
R and Baldini, A and Barbarino, GC and Barish, BC and Battistoni, G and Bellotti, R and Bemporad, C and Bernardini, P and Bilokon, H and Bisi,
V and Bloise, C and Bosio, T and Bower, C and Bussino, S and Cafagna, F and Calicchio, M and Campana, D and Carboni, M and Castellano, M and Cecchini, S and Cei, F and Chiarella, V and Corona, A and Coutu, S and de
Benedictis, L and de Cataldo, G and Dekhissi, H and de Marzo, C and de
Mitri, I and de Vincenzi, M and di Credico, A and Erriquez, O and Fantini, R and Favuzzi, C and Forti, C and Fusco, P and Giacomelli, G and Giannini, G and Goretti, M and Grassi, M and Green, P and Grillo, A and Guarino, F and Guarnaccia, P and Gustavino, C and Habig, A and Hanson,
K and Hawthorne, A and Heinz, R and Hong, JT and Iarocci, E and Katsavounidis, E and Kearns, E and Kyriazopoulou, S and Lamanna, E and Lane, C and Levin, DS and Lipari, P and Liu, G and Liu, R and Longley, NP and Longo, MJ and Ludlam, G and Maaroufi, F and Mancarella, G and Mandrioli,
G and Margiotta-Neri, A and Marini, A and Martello, D and Marzari-Chiesa, A and Mazziotta, MN and Michael, DG and Mikheyev, S and Miller, L and Monacelli, P and Montaruli, T and Monteno, M and Mufson,
S and Musser, J and Nicoló, D and Nolty, R and Okada, C and Orth, C and Osteria, G and Palamara, O and Parlati, S and Patera, V and Patrizii, L and Pazzi, R and Peck, CW and Petrera, S and Pignatano, ND and Pistilli, P and Popa, V and Rainó, A and Reynoldson, J},
Title = {Performance of the MACRO detector at Gran Sasso: Moon shadow
and seasonal variations},
Journal = {Nuclear Physics B - Proceedings Supplements},
Volume = {61},
Number = {3 SUPPL.},
Pages = {180-184},
Publisher = {Elsevier BV},
Year = {1998},
Month = {January},
ISSN = {0920-5632},
url = {http://dx.doi.org/10.1016/S0920-5632(97)00559-8},
Abstract = {The MACRO underground detector at Gran Sasso has recorded
about 30 million muon events in the period 1989-1995. We
have analyzed these data to look for time variations and to
study the pointing capabilities of the apparatus in the
search for astrophysical point sources. We have observed a
3% seasonal variation of the high energy muon rate, due to
atmospheric temperature variations, in agreement with
theoretical predictions. We report also the detection of the
moon shadowing effect with a statistical significance of 3.7
σ. The results obtained straighten the possibility that a
"muon astronomy" using underground experiments is
possible.},
Doi = {10.1016/S0920-5632(97)00559-8},
Key = {fds248725}
}
@booklet{Ambrosio98b,
Author = {Ambrosio, M and Antolini, R and Auriemma, G and Baker, R and Baldini, A and Barbarino, GC and Barish, BC and Battistoni, G and Bellotti, R and Bemporad, C and Bernardini, P and Bilokon, H and Bisi, V and Bloise, C and Bower, C and Bussino, S and Cafagna, F and Calicchio, M and Campana, D and Carboni, M and Castellano, M and Cecchini, S and Cei, F and Celio, P and Chiarella, V and Corona, A and Coutu, S and de Benedictis, L and de
Cataldo, G and Dekhissi, H and de Marzo, C and de Mitri, I and de
Vincenzi, M and di Credico, A and Erriquez, O and Favuzzi, C and Forti,
C and Fusco, P and Giacomelli, G and Giannini, G and Giglietto, N and Grassi, M and Gray, L and Grillo, A and Guarino, F and Guarnaccia, P and Gustavino, C and Habig, A and Hanson, K and Hawthorne, A and Heinz, R and Hong, JT and Iarocci, E and Katsavounidis, E and Kearns, E and Kyriazopoulou, S and Lamanna, E and Lane, C and Levin, DS and Lipari, P and Liu, R and Longley, NP and Longo, MJ and Ludlam, G and Maaroufi, F and Mancarella, G and Mandrioli, G and Manzoor, S and Margiotta Neri and A and Marini, A and Martello, D and Marzari-Chiesa, A and Mazziotta, MN and Mazzotta, C and Michael, DG and Mikheyev, S and Miller, L and Monacelli,
P and Montaruli, T and Monteno, M and Mufson, S and Musser, J and Nicoló,
D and Nolty, R and Okada, C and Orth, C and Osteria, G and Palamara, O and Parlati, S and Patera, V and Patrizii, L and Pazzi, R and Peck, CW and Petrera, S and Pistilli, P and Popa, V and Rainó, A and Reynoldson, J and Ronga, F and Rubizzo, U},
Title = {Real time supernova neutrino burst detection with
MACRO},
Journal = {Astroparticle Physics},
Volume = {8},
Number = {3},
Pages = {123-133},
Publisher = {Elsevier BV},
Year = {1998},
Month = {January},
ISSN = {0927-6505},
url = {http://dx.doi.org/10.1016/S0927-6505(97)00032-7},
Abstract = {The MACRO experiment has been running as a supernova
neutrino detector since 1989 and is sensitive to the whole
galaxy since the beginning of 1992. A galactic supernova
would produce some hundreds of v̄e events in the detector.
We describe our stellar gravitational collapse online
monitors and alarm system, and present the results of a
search for neutrino bursts from supernovae during a period
of 1.5 yr. © 1998 Elsevier Science B.V.},
Doi = {10.1016/S0927-6505(97)00032-7},
Key = {Ambrosio98b}
}
@booklet{Fukuda98b,
Author = {Fukuda, Y and Hayakawa, T and Ichihara, E and Inoue, K and Ishihara, K and Ishino, H and Itow, Y and Kajita, T and Kameda, J and Kasuga, S and Kobayashi, K and Kobayashi, Y and Koshio, Y and Miura, M and Nakahata,
M and Nakayama, S and Okada, A and Okumura, K and Sakurai, N and Shiozawa,
M and Suzuki, Y and Takeuchi, Y and Totsuka, Y and Yamada, S and Earl, M and Habig, A and Kearns, E and Messier, MD and Scholberg, K and Stone, JL and Sulak, LR and Walter, CW and Goldhaber, M and Barszczxak, T and Casper,
D and Gajewski, W and Halverson, PG and Hsu, J and Kropp, WR and Price, LR and Reines, F and Smy, M and Sobel, HW and Vagins, MR and Ganezer, KS and Keig,
WE and Ellsworth, RW and Tasaka, S and Flanagan, JW and Kibayashi, A and Learned, JG and Matsuno, S and Stenger, VJ and Takemori, D and Ishii, T and Kanzaki, J and Kobayashi, T and Mine, S and Nakamura, K and Nishikawa,
K and Oyama, Y and Sakai, A and Sakuda, M and Sasaki, O and Echigo, S and Kohama, M and Suzuki, AT and Haines, TJ and Blaufuss, E and Kim, BK and Sanford, R and Svoboda, R and Chen, ML and Conner, Z and Goodman, JA and Sullivan, GW and Hill, J and Jung, CK and Martens, K and Mauger, C and Mc
Grew, C and Sharkey, E and Viren, B and Yanagisawa, C and Doki, W and Miyano, K and Okazawa, H and Saji, C and Takahata, M and Nagashima, Y and Takita, M and Yamaguchi, T and Yoshida, M and Kim, SB and Etoh, M and Fujita, K and Hasegawa, A and Hasegawa, T and Hatakeyama, S and Iwamoto,
T},
Title = {Evidence for oscillation of atmospheric neutrinos},
Journal = {Physical Review Letters},
Volume = {81},
Number = {8},
Pages = {1562-1567},
Publisher = {American Physical Society (APS)},
Year = {1998},
Month = {January},
ISSN = {0031-9007},
url = {http://dx.doi.org/10.1103/PhysRevLett.81.1562},
Abstract = {We present an analysis of atmospheric neutrino data from a
33.0 kton yr (535-day) exposure of the Super-Kamiokande
detector. The data exhibit a zenith angle dependent deficit
of muon neutrinos which is inconsistent with expectations
based on calculations of the atmospheric neutrino flux.
Experimental biases and uncertainties in the prediction of
neutrino fluxes and cross sections are unable to explain our
observation. The data are consistent, however, with
two-flavor νμ↔ντ oscillations with sin22θ>0.82 and
5×10−4<Δm2<6×10−3eV2 at 90% confidence level. © 1998
The American Physical Society.},
Doi = {10.1103/PhysRevLett.81.1562},
Key = {Fukuda98b}
}
@booklet{Shiozawa98,
Author = {Shiozawa, M and Viren, B and Fukuda, Y and Hayakawa, T and Ichihara, E and Inoue, K and Ishihara, K and Ishino, H and Itow, Y and Kajita, T and Kameda, J and Kasuga, S and Kobayashi, K and Kobayashi, Y and Koshio, Y and Miura, M and Nakahata, M and Nakayama, S and Okada, A and Oketa, M and Okumura, K and Ota, M and Sakurai, N and Suzuki, Y and Takeuchi, Y and Totsuka, Y and Yamada, S and Earl, M and Habig, A and Kearns, E and Messier, MD and Scholberg, K and Stone, JL and Sulak, LR and Walter, CW and Goldhaber, M and Barszczak, T and Gajewski, W and Halverson, PG and Hsu,
J and Kropp, WR and Price, LR and Reines, F and Sobel, HW and Vagins, MR and Ganezer, KS and Keig, WE and Ellsworth, RW and Tasaka, S and Flanagan,
JW and Kibayashi, A and Learned, JG and Matsuno, S and Stenger, V and Takemori, D and Ishii, T and Kanzaki, J and Kobayashi, T and Nakamura,
K and Nishikawa, K and Oyama, Y and Sakai, A and Sakuda, M and Sasaki, O and Echigo, S and Kohama, M and Suzuki, AT and Haines, TJ and Blaufuss, E and Sanford, R and Svoboda, R and Chen, ML and Conner, Z and Goodman, JA and Sullivan, GW and Mori, M and Hill, J and Jung, CK and Martens, K and Mauger, C and Mc Grew and C and Sharkey, E and Yanagisawa, C and Doki, W and Ishizuka, T and Kitaguchi, Y and Koga, H and Miyano, K and Okazawa, H and Saji, C and Takahata, M and Kusano, A and Nagashima, Y and Takita, M and Yamaguchi, T and Yoshida, M and Kim, SB and Etoh, M and Fujita, K and Hasegawa, A},
Title = {Search for proton decay via p→e+π0
in a large water cherenkov detector},
Journal = {Physical Review Letters},
Volume = {81},
Number = {16},
Pages = {3319-3323},
Publisher = {American Physical Society (APS)},
Year = {1998},
Month = {January},
ISSN = {0031-9007},
url = {http://dx.doi.org/10.1103/PhysRevLett.81.3319},
Abstract = {We have searched for proton decay via p→e+π0 using data
from a 25.5ktonyr exposure of the Super-Kamiokande detector.
We find no candidate events with an expected background
induced by atmospheric neutrinos of 0.1 events. From these
data, we set a lower limit on the partial lifetime of the
proton τ/Bp→e+π0 to be 1.6×1033years at a 90%
confidence level. © 1998 The American Physical
Society.},
Doi = {10.1103/PhysRevLett.81.3319},
Key = {Shiozawa98}
}
@booklet{Ambrosio98a,
Author = {Ambrosio, M and Antolini, R and Aramo, C and Auriemma, G and Baldini, A and Barbarino, GC and Barish, BC and Battistoni, G and Bellotti, R and Bemporad, C and Bernardini, P and Bilokon, H and Bisi, V and Bloise, C and Bower, C and Bussino, S and Cafagna, F and Calicchio, M and Campana, D and Carboni, M and Castellano, M and Cecchini, S and Cei, F and Chiarella,
V and Coutu, S and Cunti, G and de Benedictis, L and de Cataldo, G and Dekhissi, H and de Marzo, C and de Mitri, I and de Vincenzi, M and di
Credico, A and Erriquez, O and Favuzzi, C and Forti, C and Fusco, P and Giacomelli, G and Giannini, G and Giglietto, N and Grassi, M and Gray,
L and Grillo, A and Guarino, F and Guarnaccia, P and Gustavino, C and Habig, A and Hanson, K and Hawthorne, A and Heinz, R and Iarocci, E and Katsavounidis, E and Kearns, E and Kyriazopoulou, S and Lamanna, E and Lane, C and Levin, DS and Lipari, P and Longley, NP and Longo, MJ and Maaroufi, F and Mancarella, G and Mandrioli, G and Manzoor, S and Margiotta Neri and A and Marini, A and Martello, D and Marzari-Chiesa,
A and Mazziotta, MN and Mazzotta, C and Michael, DG and Mikheyev, S and Miller, L and Monacelli, P and Montaruli, T and Monteno, M and Mufson,
S and Musser, J and Nicoló, D and Nolty, R and Okada, C and Orth, C and Osteria, G and Palamara, O and Patera, V and Patrizii, L and Pazzi, R and Peck, CW and Petrera, S and Pistilli, P and Popa, V and Pugliese, V and Rainó, A and Reynoldson, J and Ronga, F and Rubizzo, U and Sanzgiri, A and Satriano, C and Satta, L and Scapparone, E},
Title = {The observation of up-going charged particles produced by
high energy muons in underground detectors},
Journal = {Astroparticle Physics},
Volume = {9},
Number = {2},
Pages = {105-117},
Publisher = {Elsevier BV},
Year = {1998},
Month = {January},
ISSN = {0927-6505},
url = {http://dx.doi.org/10.1016/S0927-6505(98)00010-3},
Abstract = {An experimental study of the production of up-going charged
particles in inelastic interactions of down-going
underground muons is reported, using data obtained from the
MACRO detector at the Gran Sasso Laboratory. In a sample of
12.2 x 106 single muons, corresponding to a detector
lifetime of 1.55y, 243 events are observed having an
up-going particle associated with a down-going muon. These
events are analysed to determine the range and emission
angle distributions of the up-going particle, corrected for
detection and reconstruction efficiency. Measurements of the
muon neutrino flux by underground detectors are often based
on the observation of through-going and stopping muons
produced in νμ interactions in the rock below the
detector. Up-going particles produced by an undetected
down-going muon are a potential background source in these
measurements. The implications of this background for
neutrino studies using MACRO are discussed. © 1998 Elsevier
Science B.V.},
Doi = {10.1016/S0927-6505(98)00010-3},
Key = {Ambrosio98a}
}
@booklet{Fukuda98c,
Author = {Fukuda, Y and Hayakawa, T and Ichihara, E and Inoue, K and Ishihara, K and Ishino, H and Itow, Y and Kajita, T and Kameda, J and Kasuga, S and Kobayashi, K and Kobayashi, Y and Koshio, Y and Martens, K and Miura, M and Nakahata, M and Nakayama, S and Okada, A and Oketa, M and Okumura, K and Ota, M and Sakurai, N and Shiozawa, M and Suzuki, Y and Takeuchi, Y and Totsuka, Y and Yamada, S and Earl, M and Habig, A and Hong, JT and Kearns,
E and Kim, SB and Masuzawa, M and Messier, MD and Scholberg, K and Stone,
JL and Sulak, LR and Walter, CW and Goldhaber, M and Barszczak, T and Gajewski, W and Halverson, PG and Hsu, J and Kropp, WR and Price, LR and Reines, F and Sobel, HW and Vagins, MR and Ganezer, KS and Keig, WE and Ellsworth, RW and Tasaka, S and Flanagan, JW and Kibayashi, A and Learned, JG and Matsuno, S and Stenger, V and Takemori, D and Ishii, T and Kanzaki, J and Kobayashi, T and Nakamura, K and Nishikawa, K and Oyama,
Y and Sakai, A and Sakuda, M and Sasaki, O and Echigo, S and Kohama, M and Suzuki, AT and Haines, TJ and Blaufuss, E and Sanford, R and Svoboda, R and Chen, ML and Conner, Z and Goodman, JA and Sullivan, GW and Mori, M and Hill, J and Jung, CK and Mauger, C and Mc Grew and C and Sharkey, E and Viren,
B and Yanagisawa, C and Doki, W and Ishizuka, T and Kitaguchi, Y and Koga,
H and Miyano, K and Okazawa, H and Saji, C and Takahata, M and Kusano, A and Nagashima, Y and Takita, M and Yamaguchi, T and Yoshida, M and Etoh,
M},
Title = {Measurements of the solar neutrino flux from
super-kamiokande’s first 300 days},
Journal = {Physical Review Letters},
Volume = {81},
Number = {6},
Pages = {1158-1162},
Publisher = {American Physical Society (APS)},
Year = {1998},
Month = {January},
ISSN = {0031-9007},
url = {http://dx.doi.org/10.1103/PhysRevLett.81.1158},
Abstract = {The first results of the solar neutrino flux measurement
from Super-Kamiokande are presented. The results shown here
are obtained from data taken between 31 May 1996, and 23
June 1997. Using our measurement of recoil electrons with
energies above 6.5 MeV, we infer the total flux of 8B solar
neutrinos to be 2.42±0.06(stat)+0.10-0.07(syst)×106cm-2s-1.
This result is consistent with the Kamiokande measurement
and is 36% of the flux predicted by the BP95 solar model.
The flux is also measured in 1.5 month subsets and shown to
be consistent with a constant rate. © 1998 The American
Physical Society.},
Doi = {10.1103/PhysRevLett.81.1158},
Key = {Fukuda98c}
}
@article{fds345331,
Author = {Mazziotta, MN},
Title = {Performance of the transition radiation detector of the
MACRO experiment},
Journal = {NUCLEAR PHYSICS B},
Pages = {289-294},
Publisher = {ELSEVIER SCIENCE BV},
Year = {1998},
Month = {February},
Key = {fds345331}
}
@article{fds326732,
Author = {Astbury, A and Aubert, B and Augé, E and Baisin, L and Barreiro, F and Battistoni, G and Bazan, A and Baze, JM and Beaudoin, G and Beaugiraud,
B and Berset, JC and Boniface, J and Boos, E and Breton, D and Camin, DV and Canton, B and Cavalli, D and Chase, R and Chekhtman, A and Chevalley,
JL and Chmeissani, M and Chollet, JC and Citterio, M and Colas, J and Collot, J and Costa, G and Cousinou, MC and Cozzi, L and Dargent, P and David, J and Davis, RA and Delagnes, E and de LaTaille, C and Del Peso,
J and Depommier, P and de Saintignon, P and Dinkespiller, B and Eek, LO and Etienne, F and Eynard, G and Fassnacht, P and Fayard, L and Fedyakin, N and Fernandez, E and Ferrari, A and Fouchez, D and Fournier, D and Garcia,
J and Garrido, L and Genat, JF and Gianotti, F and Gildemeister, O and Gingrich, DM and Gonzales, J and Gordon, HA and Gosset, L and Greenious,
G and Hervas, L and Hostachy, JY and Hrisoho, A and Imbault, D and Jacquier, Y and Jézéquel, S and Keeler, R and Kitching, P and Labarga,
L and Lavocat, P and Le Dortz and O and Lefebvre, M and Leflour, T and León-Florián, E and Leroy, C and Linossier, O and Lissauer, D and Lottin, JP and Lund-Jensen, B and Ma, H and Mahout, G and Makowiecki, D and Mandelli, L and Mansoulié, B and Marin, CP and Martin, L and Martinez,
M and Mazzanti, M and Merkel, B and Meyer, JP and Miotto, A and Monnier, E and Nagy, E and Nessi, M and Nicoleau, S and Nikolic, I and Noppe, JM and Olivetto, C and Olsen, B and Padilla, C and Parrour, G and Perini, L and Petroff, P and Pinfold, JL and Poggioli, L and Puzo, P and Radeka, V and Rahm, DC and Renardy, JF and Rescia, S and Resconi, S and Richer, JP and Richter, W and Robertson, S and Rodning, NL and Romero, P and Roy, P and Sala, P and Sauvage, G and Savoy-Navarro, A and Schaffer, A and Scheel,
C and Schwemling, P and Schwindling, J and Seguin-Moreau, N and Serin,
L and Simion, S and Söderqvist, J and Stephani, D and Taguet, JP and Takai, H and Teiger, J and Thion, J and Tisserand, V and Tisserant, S and VanDenPlas, D and Veillet, JJ and Vichou, I and Vuillemin, V and Walter,
C and White, J and Wingerter-Seez, I and Zhautykov, BO and Zitoun, R and Zolnierowski, YP},
Title = {Test beam results of a stereo preshower integrated in the
liquid argon accordion calorimeter},
Journal = {Nuclear Instruments and Methods in Physics Research Section
A: Accelerators, Spectrometers, Detectors and Associated
Equipment},
Volume = {411},
Number = {2-3},
Pages = {313-329},
Publisher = {Elsevier BV},
Year = {1998},
Month = {July},
url = {http://dx.doi.org/10.1016/s0168-9002(98)00342-8},
Doi = {10.1016/s0168-9002(98)00342-8},
Key = {fds326732}
}
@booklet{Fukuda98d,
Author = {Fukuda, Y and Hayakawa, T and Ichihara, E and Inoue, K and Ishihara, K and Ishino, H and Itow, Y and Kajita, T and Kameda, J and Kasuga, S and Kobayashi, K and Kobayashi, Y and Koshio, Y and Martens, K and Miura, M and Nakahata, M and Nakayama, S and Okada, A and Oketa, M and Okumura, K and Ota, M and Sakurai, N and Shiozawa, M and Suzuki, Y and Takeuchi, Y and Totsuka, Y and Yamada, S and Earl, M and Habig, A and Hong, JT and Kearns,
E and Kim, SB and Masuzawa, M and Messier, MD and Scholberg, K and Stone,
JL and Sulak, LR and Walter, CW and Goldhaber, M and Barszczak, T and Gajewski, W and Halverson, PG and Hsu, J and Kropp, WR and Price, LR and Reines, F and Sobel, HW and Vagins, MR and Ganezer, KS and Keig, WE and Ellsworth, RW and Tasaka, S and Flanagan, JW and Kibayashi, A and Learned, JG and Matsuno, S and Stenger, V and Takemori, D and Ishii, T and Kanzaki, J and Kobayashi, T and Nakamura, K and Nishikawa, K and Oyama,
Y and Sakai, A and Sakuda, M and Sasaki, O and Echigo, S and Kohama, M and Suzuki, AT and Haines, TJ and Blaufuss, E and Sanford, R and Svoboda, R and Chen, ML and Conner, Z and Goodman, JA and Sullivan, GW and Mori, M and Goebel, F and Hill, J and Jung, CK and Mauger, C and McGrew, C and Sharkey,
E and Viren, B and Yanagisawa, C and Doki, W and Ishizuka, T and Kitaguchi,
Y and Koga, H and Miyano, K and Okazawa, H and Saji, C and Takahata, M and Kusano, A and Nagashima, Y and Takita, M and Yamaguchi, T and Yoshida,
M},
Title = {Measurement of a small atmospheric νμ/νe
ratio},
Journal = {Physics Letters, Section B: Nuclear, Elementary Particle and
High-Energy Physics},
Volume = {433},
Number = {1-2},
Pages = {9-18},
Publisher = {Elsevier BV},
Year = {1998},
Month = {August},
ISSN = {0370-2693},
url = {http://gateway.webofknowledge.com/gateway/Gateway.cgi?GWVersion=2&SrcApp=PARTNER_APP&SrcAuth=LinksAMR&KeyUT=WOS:000075193300002&DestLinkType=FullRecord&DestApp=ALL_WOS&UsrCustomerID=47d3190e77e5a3a53558812f597b0b92},
Abstract = {From an exposure of 25.5 kiloton-years of the
Super-Kamiokande detector, 900 muon-like and 983
electron-like single-ring atmospheric neutrino interactions
were detected with momentum pe > 100 MeV/c, pμ > 200 MeV/c,
and with visible energy less than 1.33 GeV. Using a detailed
Monte Carlo simulation, the ratio (μ/e)DATA/(μ/e)MC was
measured to be 0.61 ± 0.03(stat.) ± 0.05(sys.), consistent
with previous results from the Kamiokande, IMB and Soudan-2
experiments, and smaller than expected from theoretical
models of atmospheric neutrino production. © 1998 Published
by Elsevier Science B.V. All rights reserved.},
Doi = {10.1016/S0370-2693(98)00476-6},
Key = {Fukuda98d}
}
@booklet{Ambrosio98,
Author = {Ambrosio, M and Antolini, R and Aramo, C and Auriemma, G and Baldini, A and Barbarino, GC and Barish, BC and Battistoni, G and Bellotti, R and Bemporad, C and Bernardini, P and Bilokon, H and Bisi, V and Bloise, C and Bower, C and Bussino, S and Cafagna, F and Calicchio, M and Campana, D and Carboni, M and Castellano, M and Cecchini, S and Cei, F and Chiarella,
V and Choudhary, BC and Coutu, S and de Benedictis, L and de Cataldo, G and Dekhissi, H and de Marzo, C and de Mitri, I and Derkaoui, J and de
Vincenzi, M and di Credico, A and Erriquez, O and Favuzzi, C and Forti,
C and Fusco, P and Giacomelli, G and Giannini, G and Giglietto, N and Giorgini, M and Grassi, M and Gray, L and Grillo, A and Guarino, F and Guarnaccia, P and Gustavino, C and Habig, A and Hanson, K and Hawthorne,
A and Heinz, R and Huang, Y and Iarocci, E and Katsavounidis, E and Katsavounidis, I and Kearns, E and Kim, H and Kyriazopoulou, S and Lamanna, E and Lane, C and Levin, DS and Lipari, P and Longley, NP and Longo, MJ and Maaroufi, F and Mancarella, G and Mandrioli, G and Manzoor, S and Margiotta Neri and A and Marini, A and Martello, D and Marzari-Chiesa, A and Mazziotta, MN and Mazzotta, C and Michael, DG and Mikheyev, S and Miller, L and Monacelli, P and Montaruli, T and Monteno,
M and Mufson, S and Musser, J and Nicolo, D and Nolty, R and Okada, C and Orth, C and Osteria, G and Ouchrif, M and Palamara, O and Patera, V and Patrizii, L and Pazzi, R and Peck, CW and Petrera, S and Pistilli, P and Popa, V and Pugliese, V and Raino, A and Reynoldson,
J},
Title = {Measurement of the atmospheric neutrino-induced upgoing muon
flux using MACRO},
Journal = {Physics Letters, Section B: Nuclear, Elementary Particle and
High-Energy Physics},
Volume = {434},
Number = {3-4},
Pages = {451-457},
Publisher = {Elsevier BV},
Year = {1998},
Month = {August},
ISSN = {0370-2693},
url = {http://dx.doi.org/10.1016/S0370-2693(98)00885-5},
Abstract = {We present a measurement of the flux of neutrino-induced
upgoing muons (< Eν > ∼ 100 GeV) using the MACRO
detector. The ratio of the number of observed to expected
events integrated over all zenith angles is 0.74 ± 0.036
(stat) ± 0.046 (systematic) ± 0.13 (theoretical). The
observed zenith distribution for -1.0 ≤ cosθ ≤ -0.1
does not fit well with the no oscillation expectation,
giving a maximum probability for χ2 of 0.1%. The acceptance
of the detector has been extensively studied using downgoing
muons, independent analyses and Monte Carlo simulations. The
other systematic uncertainties cannot be the source of the
discrepancies between the data and expectations. We have
investigated whether the observed number of events and the
shape of the zenith distribution can be explained by a
neutrino oscillation hypothesis. Fitting either the flux or
zenith distribution independently yields mixing parameters
of sin22θ = 1.0 and Δm2 of a few times 10-3 eV2. However,
the observed zenith distribution does not fit well with any
expectations, giving a maximum probability for χ2 of 5% for
the best oscillation hypothesis, and the combined
probability for the shape and number of events is 17%. We
conclude that these data favor a neutrino oscillation
hypothesis, but with unexplained structure in the zenith
distribution not easily explained by either the statistics
or systematics of the experiment. © 1998 Published by
Elsevier Science B.V. All rights reserved.},
Doi = {10.1016/S0370-2693(98)00885-5},
Key = {Ambrosio98}
}
@booklet{Fukuda98a,
Author = {Fukuda, Y and Hayakawa, T and Ichihara, E and Inoue, K and Ishihara, K and Ishino, H and Itow, Y and Kajita, T and Kameda, J and Kasuga, S and Kobayashi, K and Kobayashi, Y and Koshio, Y and Martens, K and Miura, M and Nakahata, M and Nakayama, S and Okada, A and Oketa, M and Okumura, K and Ota, M and Sakurai, N and Shiozawa, M and Suzuki, Y and Takeuchi, Y and Totsuka, Y and Yamada, S and Earl, M and Habig, A and Kearns, E and Kim,
SB and Messier, MD and Scholberg, K and Stone, JL and Sulak, LR and Walter,
CW and Goldhaber, M and Barszczak, T and Gajewski, W and Halverson, PG and Hsu, J and Kropp, WR and Price, LR and Reines, F and Sobel, HW and Vagins,
MR and Ganezer, KS and Keig, WE and Ellsworth, RW and Tasaka, S and Flanagan, JW and Kibayashi, A and Learned, JG and Matsuno, S and Stenger, V and Takemori, D and Ishii, T and Kanzaki, J and Kobayashi, T and Nakamura, K and Nishikawa, K and Oyama, Y and Sakai, A and Sakuda, M and Sasaki, O and Echigo, S and Kohama, M and Suzuki, AT and Haines, TJ and Blaufuss, E and Conner, Z and Goodman, JA and Sullivan, GW and Mori, M and Hill, J and Jung, CK and Mauger, C and McGrew, C and Sharkey, E and Viren,
B and Yanagisawa, C and Doki, W and Ishizuka, T and Kitaguchi, Y and Koga,
H and Miyano, K and Okazawa, H and Saji, C and Takahata, M and Kusano, A and Nagashima, Y and Takita, M and Yamaguchi, T and Yoshida, M and Etoh, M and Fujita, K and Hasegawa, A and Hasegawa, T and Hatakeyama, S and Iwamoto,
T},
Title = {Study of the atmospheric neutrino flux in the multi-GeV
energy range},
Journal = {Physics Letters, Section B: Nuclear, Elementary Particle and
High-Energy Physics},
Volume = {436},
Number = {1-2},
Pages = {33-41},
Publisher = {Elsevier BV},
Year = {1998},
Month = {September},
ISSN = {0370-2693},
url = {http://dx.doi.org/10.1016/S0370-2693(98)00876-4},
Abstract = {The flavor ratio of the atmospheric neutrino flux and its
zenith angle dependence have been studied in the multi-GeV
energy range using an exposure of 25.5 kiloton-years of the
Super-Kamiokande detector. By comparing the data to a
detailed Monte Carlo simulation, the ratio
(μ/e)DATA/(μ/e)MC was measured to be 0.66 ± 0.06(stat.)
± 0.08(sys.). In addition, a strong distortion in the shape
of the μ-like event zenith angle distribution was observed.
The ratio of the number of upward to downward μ-like events
was found to be 0.52+0.070.06(stat.) ± 0.01(sys.), with an
expected value of 0.98 ± 0.03(stat.) ± 0.02(sys.), while
the same ratio for the e-like events was consistent with
unity. © 1998 Elsevier Science B.V. All rights
reserved.},
Doi = {10.1016/S0370-2693(98)00876-4},
Key = {Fukuda98a}
}
@booklet{Fukuda98,
Author = {Fukuda, Y and Hayakawa, T and Ichihara, E and Inoue, K and Ishihara, K and Ishino, H and Itow, Y and Kajita, T and Kameda, J and Kasuga, S and Kobayashi, K and Kobayashi, Y and Koshio, Y and Martens, K and Miura, M and Nakahata, M and Nakayama, S and Okada, A and Oketa, M and Okumura, K and Ota, M and Sakurai, N and Shiozawa, M and Suzuki, Y and Takeuchi, Y and Totsuka, Y and Yamada, S and Earl, M and Habig, A and Hong, JT and Kearns,
E and Kim, SB and Masuzawa, M and Messier, MD and Scholberg, K and Stone,
JL and Sulak, LR and Walter, CW and Goldhaber, M and Barszczak, T and Gajewski, W and Halverson, PG and Hsu, J and Kropp, WR and Price, LR and Reines, F and Sobel, HW and Vagins, MR and Ganezer, KS and Keig, WE and Ellsworth, RW and Tasaka, S and Flanagan, JW and Kibayashi, A and Learned, JG and Matsuno, S and Stenger, V and Takemori, D and Ishii, T and Kanzaki, J and Kobayashi, T and Nakamura, K and Nishikawa, K and Oyama,
Y and Sakai, A and Sakuda, M and Sasaki, O and Echigo, S and Kohama, M and Suzuki, AT and Haines, TJ and Blaufuss, E and Sanford, R and Svoboda, R and Chen, ML and Conner, Z and Goodman, JA and Sullivan, GW and Mori, M and Hill, J and Jung, CK and Mauger, C and McGrew, C and Sharkey, E and Viren,
B and Yanagisawa, C and Doki, W and Ishizuka, T and Kitaguchi, Y and Koga,
H and Miyano, K and Okazawa, H and Saji, C and Takahata, M and Kusano, A and Nagashima, Y and Takita, M and Yamaguchi, T and Yoshida, M and Etoh, M and Fujita, K and Hasegawa, A and Hasegawa, T and Hatakeyama, S and Iwamoto,
T and Kinebuchi, T and Koga, M and Maruyama, T and Ogawa, H and Suzuki, A and Tsushima, F and Koshiba, M and Nemoto, M and Nishijima, K and Futagami,
T and Hayato, Y and Kanaya, Y and Kaneyuki, K and Watanabe, Y and Kielczewska, D and Doyle, R and George, J and Stachyra, A and Wai, L and Wilkes, J and Young, K},
Title = {Erratum: Measurements of the Solar Neutrino Flux from
Super-Kamiokande's First 300 Days [Phys. Rev. Lett. 81, 1158
(1998)]},
Journal = {Physical Review Letters},
Volume = {81},
Number = {19},
Pages = {4279-4279},
Publisher = {American Physical Society (APS)},
Year = {1998},
Month = {November},
ISSN = {0031-9007},
url = {http://gateway.webofknowledge.com/gateway/Gateway.cgi?GWVersion=2&SrcApp=PARTNER_APP&SrcAuth=LinksAMR&KeyUT=WOS:000077011000068&DestLinkType=FullRecord&DestApp=ALL_WOS&UsrCustomerID=47d3190e77e5a3a53558812f597b0b92},
Doi = {10.1103/physrevlett.81.4279},
Key = {Fukuda98}
}
@booklet{Hayato99,
Author = {Hayato, Y and Earl, M and Fukuda, Y and Hayakawa, T and Inoue, K and Ishihara, K and Ishino, H and Itow, Y and Kajita, T and Kameda, J and Kasuga, S and Kobayashi, K and Kobayashi, Y and Koshio, Y and Miura, M and Nakahata, M and Nakayama, S and Obayashi, Y and Okada, A and Okumura, K and Sakurai, N and Shiozawa, M and Suzuki, Y and Takeuchi, H and Takeuchi,
Y and Totsuka, Y and Yamada, S and Habig, A and Kearns, E and Messier, MD and Scholberg, K and Stone, JL and Sulak, LR and Walter, CW and Goldhaber,
M and Barszczak, T and Casper, D and Gajewski, W and Kropp, WR and Mine, S and Price, LR and Smy, M and Sobel, HW and Vagins, MR and Ganezer, KS and Keig,
WE and Ellsworth, RW and Tasaka, S and Kibayashi, A and Learned, JG and Matsuno, S and Stenger, VJ and Takemori, D and Ishii, T and Kanzaki, J and Kobayashi, T and Nakamura, K and Nishikawa, K and Oyama, Y and Sakai, A and Sakuda, M and Sasaki, O and Echigo, S and Kohama, M and Suzuki, AT and Haines, TJ and Blaufuss, E and Kim, BK and Sanford, R and Svoboda, R and Chen, ML and Goodman, JA and Sullivan, GW and Hill, J and Jung, CK and Martens, K and Mauger, C and Mc Grew and C and Sharkey, E and Viren, B and Yanagisawa, C and Doki, W and Kirisawa, M and Inaba, S and Miyano, K and Okazawa, H and Saji, C and Takahashi, M and Takahata, M and Higuchi, K and Nagashima, Y and Takita, M and Yamaguchi, T and Yoshida, M and Kim, SB and Etoh, M and Hasegawa, A and Hasegawa, T and Hatakeyama, S and Iwamoto,
T},
Title = {Search for proton decay through p → ¯νK+ in a
large water cherenkov detector},
Journal = {Physical Review Letters},
Volume = {83},
Number = {8},
Pages = {1529-1533},
Publisher = {American Physical Society (APS)},
Year = {1999},
Month = {January},
url = {http://dx.doi.org/10.1103/PhysRevLett.83.1529},
Abstract = {We present results of a search for proton decays, p →
¯νK+, using data from a 33kt?yr exposure of the
Super-Kamiokande detector. Two decay modes of the kaon, K+
→ µ+νµ and K+ → π+π0, were studied. The data were
consistent with the background expected from atmospheric
neutrinos; therefore a lower limit on the partial lifetime
of the proton τ/B(p → ¯νK+) was found to be 6.7 × 1032
years at 90% confidence level. © 1999 The American Physical
Society.},
Doi = {10.1103/PhysRevLett.83.1529},
Key = {Hayato99}
}
@booklet{Ambrosio99d,
Author = {Ambrosio, M and Antolini, R and Aramo, C and Auriemma, G and Baldini, A and Barbarino, GC and Barish, BC and Battistoni, G and Bellotti, R and Bemporad, C and Bernardini, P and Bilokon, H and Bisi, V and Bloise, C and Bower, C and Bussino, S and Cafagna, F and Calicchio, M and Campana, D and Carboni, M and Castellano, M and Cecchini, S and Cei, F and Chiarella,
V and Choudhary, BC and Coutu, S and de Benedictis, L and Dc Cataldo and G and Dekhissi, H and de Marzo, C and de Mitri, I and Derkaoui, J and de
Vincenzi, M and Di Credico and A and Erriquez, O and Favuzzi, C and Forti,
C and Fusco, P and Giacomelli, G and Giannini, G and Giglietto, N and Giorgini, M and Grassi, M and Gray, L and Grillo, A and Guarino, F and Guarnaccia, P and Gustavino, C and Habig, A and Hanson, K and Heinz, R and Huang, Y and Iarocci, E and Katsavounidis, E and Kearns, E and Kim, H and Kyriazopoulou, S and Lamanna, E and Lane, C and Levin, DS and Lipari, P and Longley, NP and Longo, MJ and Maaroufi, F and Mancarella, G and Mandrioli, G and Manzoor, S and Neri, AM and Marini, A and Martello, D and Marzari-Chiesa, A and Mazziotta, MN and Mazzotta, C and Michael, DG and Mikheyev, S and Miller, L and Monacelli, P and Montarali, T and Monteno,
M and Mufson, S and Musser, J and Nicoló, D and Orth, C and Osteria, G and Ouchrif, M and Palamara, O and Patera, V and Patrizii, L and Pazzi, R and Peck, CW and Petrera, S and Pistilli, P and Popa, V and Pugliese, V and Rainò, A and Reynoldson, J and Ronga, F and Rubizzo, U and Satriano, C and Satta, L},
Title = {Measurement of the energy spectrum of underground muons at
Gran Sasso with a transition radiation detector},
Journal = {Astroparticle Physics},
Volume = {10},
Number = {1},
Pages = {11-20},
Publisher = {Elsevier BV},
Year = {1999},
Month = {January},
ISSN = {0927-6505},
url = {http://dx.doi.org/10.1016/S0927-6505(98)00037-1},
Abstract = {We have measured directly the residual energy of cosmic ray
muons crossing the MACRO detector at the Gran Sasso
Laboratory. For this measurement we have used a transition
radiation detector consisting of three identical modules,
each of about 12m2 area, operating in the energy region from
100 GeV to 1 TeV. The results presented here were obtained
with the first module collecting data for more than two
years. The average single muon energy is found to be 320 ±
4 (stat.) ± 11 (syst.) GeV in the rock depth range
3000-6500 hg/cm2. The results are in agreement with
calculations of the energy loss of muons in the rock above
the detector. © 1999 Elsevier Science B.V.},
Doi = {10.1016/S0927-6505(98)00037-1},
Key = {Ambrosio99d}
}
@booklet{Fukuda99b,
Author = {Fukuda, Y and Hayakawa, T and Ichihara, E and Inoue, K and Ishihara, K and Ishino, H and Itow, Y and Kajita, T and Kameda, J and Kasuga, S and Kobayashi, K and Kobayashi, Y and Koshio, Y and Miura, M and Nakahata,
M and Nakayama, S and Okada, A and Okumura, K and Sakurai, N and Shiozawa,
M and Suzuki, Y and Takeuchi, Y and Totsuka, Y and Yamada, S and Earl, M and Habig, A and Kearns, E and Messier, MD and Scholberg, K and Stone, JL and Sulak, LR and Walter, CW and Goldhaber, M and Barszczak, T and Casper,
D and Gajewski, W and Kropp, WR and Price, LR and Reines, F and Smy, M and Sobel, HW and Vagins, MR and Haines, TJ and Kielczewska, D and Ganezer,
KS and Keig, WE and Ellsworth, RW and Tasaka, S and Flanagan, JW and Kibayashi, A and Learned, JG and Matsuno, S and Stenger, VJ and Takemori, D and Ishii, T and Kanzaki, J and Kobayashi, T and Mine, S and Nakamura, K and Nishikawa, K and Oyama, Y and Sakai, A and Sakuda, M and Sasaki, O and Echigo, S and Kohama, M and Suzuki, AT and Blaufuss, E and Kim, BK and Sanford, R and Svoboda, R and Chen, ML and Goodman, JA and Sullivan, GW and Hill, J and Jung, CK and Martens, K and Mauger, C and Mc
Grew, C and Sharkey, E and Viren, B and Yanagisawa, C and Doki, W and Miyano, K and Okazawa, H and Saji, C and Takahata, M and Nagashima, Y and Takita, M and Yamaguchi, T and Yoshida, M and Kim, SB and Etoh, M and Fujita, K and Hasegawa, A and Hasegawa, T and Hatakeyama, S and Iwamoto,
T and Koga, M},
Title = {Measurement of the flux and zenith-angle distribution of
upward throughgoing muons by super-kamiokande},
Journal = {Physical Review Letters},
Volume = {82},
Number = {13},
Pages = {2644-2648},
Publisher = {American Physical Society (APS)},
Year = {1999},
Month = {January},
url = {http://dx.doi.org/10.1103/PhysRevLett.82.2644},
Abstract = {A total of 614 upward throughgoing muons of minimum energy
1.6 GeV are observed by Super-Kamiokande during 537 detector
live days. The measured muon flux is [1.74±0.07(stat)±0.02(sys)]×10-13cm-2s-1sr-1
compared to an expected flux of [1.97±0.44(theor)]×10-13cm-2s-1sr-1.
The absolute measured flux is in agreement with the
prediction within the errors. However, the zenith-angle
dependence of the observed upward throughgoing muon flux
does not agree with no-oscillation predictions. The observed
distortion in shape is consistent with the vμ⟷vτ
oscillation hypothesis with sin22θ> 0.4 and
1×10-3Δm2<1×10-1eV2 at 90% confidence level. © 2000 The
American Physical Society.},
Doi = {10.1103/PhysRevLett.82.2644},
Key = {Fukuda99b}
}
@booklet{Fukuda99c,
Author = {Fukuda, Y and Hayakawa, T and Ichihara, E and Inoue, K and Ishihara, K and Ishino, H and Itow, Y and Kajita, T and Kameda, J and Kasuga, S and Kobayashi, K and Kobayashi, Y and Koshio, Y and Miura, M and Nakahata,
M and Nakayama, S and Okada, A and Okumura, K and Sakurai, N and Shiozawa,
M and Suzuki, Y and Takeuchi, Y and Totsuka, Y and Yamada, S and Earl, M and Habig, A and Kerns, E and Messier, MD and Scholberg, K and Stone, JL and Sulak, LR and Walter, CW and Goldhaber, M and Barszczak, T and Casper,
D and Gajewski, W and Halverson, PG and Hsu, J and Kropp, WR and Price, LR and Reines, F and Smy, M and Sobel, HW and Vagins, MR and Ganezer, KS and Keig,
WE and Ellsworth, RW and Tasaka, S and Flanagan, JW and Kibayashi, A and Learned, JG and Matsuno, S and Stenger, VJ and Takemori, D and Ishii, T and Kanzaki, J and Kobayashi, T and Mine, S and Nakamura, K and Nishikawa,
K and Oyama, Y and Sakai, A and Sakuda, M and Sasaki, O and Echigo, S and Kohama, M and Suzuki, AT and Haines, TJ and Blaufuss, E and Kim, BK and Sanford, R and Svoboda, R and Chen, ML and Conner, Z and Goodman, JA and Sullivan, GW and Hill, J and Jung, CK and Martens, K and Mauger, C and Mc
Grew, C and Sharkey, E and Viren, B and Yanagisawa, C and Doki, W and Miyano, K and Okazawa, H and Saji, C and Takahata, M and Nagashima, Y and Takita, M and Yamaguchi, T and Yoshida, M and Kim, SB and Etoh, M and Fujita, K and Hasegawa, A and Hasagawa, T and Hatakeyama, S and Iwamoto,
T},
Title = {Constraints on neutrino oscillation parameters from the
measurement of day-night solar neutrino fluxes at
super-kamiokande},
Journal = {Physical Review Letters},
Volume = {82},
Number = {9},
Pages = {1810-1814},
Publisher = {American Physical Society (APS)},
Year = {1999},
Month = {January},
ISSN = {0031-9007},
url = {http://dx.doi.org/10.1103/PhysRevLett.82.1810},
Abstract = {A search for day-night variations in the solar neutrino flux
resulting from neutrino oscillations has been carried out
using the 504 day sample of solar neutrino data obtained at
Super-Kamiokande. The absence of a significant day-night
variation has set an absolute flux independent exclusion
region in the two neutrino oscillation parameter space. ©
1999 The American Physical Society.},
Doi = {10.1103/PhysRevLett.82.1810},
Key = {Fukuda99c}
}
@booklet{Takeuchi99,
Author = {Takeuchi, Y and Okumura, K and Kajita, T and Tasaka, S and Nemoto, M and Fukuda, Y and Okazawa, H and Hayakawa, T and Ishihara, K and Ishino, H and Itow, Y and Kameda, J and Kasuga, S and Kobayashi, K and Kobayashi, Y and Koshio, Y and Miura, M and Nakahata, M and Nakayama, S and Obayashi, Y and Okada, A and Sakurai, N and Shiozawa, M and Suzuki, Y and Takeuchi, H and Totsuka, Y and Yamada, S and Earl, M and Habig, A and Kearns, E and Messier, MD and Scholberg, K and Stone, JL and Sulak, LR and Walter, CW and Goldhaber, M and Barszczak, T and Casper, D and Gajewski, W and Kropp,
WR and Mine, S and Price, LR and Smy, M and Sobel, HW and Vagins, MR and Ganezer, KS and Keig, WE and Ellsworth, RW and Kibayashi, A and Learned,
JG and Matsuno, S and Stenger, VJ and Takemori, D and Ishii, T and Kanzaki,
J and Kobayashi, T and Nakamura, K and Nishikawa, K and Oyama, Y and Sakai,
A and Sakuda, M and Sasaki, C and Echigo, S and Kohama, M and Suzuki, AT and Haines, TJ and Blaufuss, E and Kim, BK and Sanford, R and Svoboda, R and Chen, ML and Goodman, JA and Sullivan, GW and Hill, J and Jung, CK and Martens, K and Mauger, C and McGrew, C and Sharkey, E and Viren, B and Yanagisawa, C and Doki, W and Kirisawa, M and Inaba, S and Miyano, K and Saji, C and Takahashi, M and Takahata, M and Higuchi, K and Nagashima,
Y and Takita, M and Yamaguchi, T and Yoshida, M and Kim, SB and Etoh, M and Hasegawa, A and Hasegawa, T and Hatakeyama, S and Inoue,
K},
Title = {Measurement of radon concentrations at Super-Kamiokande},
Journal = {Physics Letters, Section B: Nuclear, Elementary Particle and
High-Energy Physics},
Volume = {452},
Number = {3-4},
Pages = {418-424},
Publisher = {Elsevier BV},
Year = {1999},
Month = {January},
ISSN = {0370-2693},
url = {http://dx.doi.org/10.1016/S0370-2693(99)00311-1},
Abstract = {Radioactivity from radon is a major background for observing
solar neutrinos at Super-Kamiokande. In this paper, we
describe the measurement of radon concentrations at
Super-Kamiokande, the method of radon reduction, and the
radon monitoring system. The measurement shows that the
current low-energy event rate between 5.0 MeV and 6.5 MeV
implies a radon concentration in the Super-Kamiokande water
of less than 1.4 mBq/m3. © 1999 Published by Elsevier
Science B.V. All rights reserved.},
Doi = {10.1016/S0370-2693(99)00311-1},
Key = {Takeuchi99}
}
@booklet{Fukuda99a,
Author = {Fukuda, Y and Hayakawa, T and Ichihara, E and Inoue, K and Ishihara, K and Ishino, H and Itow, Y and Kajita, T and Kameda, J and Kasuga, S and Kobayashi, K and Kobayashi, Y and Koshio, Y and Miura, M and Nakahata,
M and Nakayama, S and Okada, A and Okumura, K and Sakurai, N and Shiozawa,
M and Suzuki, Y and Takeuchi, Y and Totsuka, Y and Yamada, S and Earl, M and Habig, A and Kearns, E and Messier, MD and Scholberg, K and Stone, JL and Sulak, LR and Walter, CW and Goldhaber, M and Barszczak, T and Casper,
D and Gajewski, W and Halverson, PG and Hsu, J and Kropp, WR and Price, LR and Reines, F and Smy, M and Sobel, HW and Vagins, MR and Ganezer, KS and Keig,
WE and Ellsworth, RW and Tasaka, S and Flanagan, JW and Kibayashi, A and Learned, JG and Matsuno, S and Stenger, VJ and Takemori, D and Ishii, T and Kanzaki, J and Kobayashi, T and Mine, S and Nakamura, K and Nishikawa,
K and Oyama, Y and Sakai, A and Sakuda, M and Sasaki, O and Echigo, S and Kohama, M and Suzuki, AT and Haines, TJ and Blaufuss, E and Kim, BK and Sanford, R and Svoboda, R and Chen, ML and Conner, Z and Goodman, JA and Sullivan, GW and Hill, J and Jung, CK and Martens, K and Mauger, C and Mc
Grew, C and Sharkey, E and Viren, B and Yanagisawa, C and Doki, W and Miyano, K and Okazawa, H and Saji, C and Takahata, M and Nagashima, Y and Takita, M and Yamaguchi, T and Yoshida, M and Kim, SB and Etoh, M and Fujita, K and Hasegawa, A and Hasegawa, T and Hatakeyama, S and Iwamoto,
T},
Title = {Measurement of the solar neutrino energy spectrum using
neutrino-electron scattering},
Journal = {Physical Review Letters},
Volume = {82},
Number = {12},
Pages = {2430-2434},
Publisher = {American Physical Society (APS)},
Year = {1999},
Month = {January},
url = {http://dx.doi.org/10.1103/PhysRevLett.82.2430},
Abstract = {A measurement of the energy spectrum of recoil electrons
from solar neutrino scattering in the Super-Kamiokande
detector is presented. The results shown here were obtained
from 504 days of data taken between 31 May 1996 and 25 March
1998. The shape of the measured spectrum is compared with
the expectation for solar 8B neutrinos. The comparison takes
into account both kinematic and detector related effects in
the measurement process. The spectral shape comparison
between the observation and the expectation gives a χ2 of
25.3 with 15 degrees of freedom, corresponding to a 4.6%
confidence level. © 1998 The American Physical
Society.},
Doi = {10.1103/PhysRevLett.82.2430},
Key = {Fukuda99a}
}
@booklet{Futagami99,
Author = {Futagami, T and Fukuda, Y and Hayakawa, T and Inoue, K and Ishihara, K and Ishino, H and Itow, Y and Kajita, T and Kameda, J and Kasuga, S and Kobayashi, K and Kobayashi, Y and Koshio, Y and Miura, M and Nakahata,
M and Nakayama, S and Obayashi, Y and Okada, A and Okumura, K and Sakurai,
N and Shiozawa, M and Suzuki, Y and Takeuchi, H and Takeuchi, Y and Totsuka, Y and Yamada, S and Earl, M and Habig, A and Kearns, E and Messier, MD and Scholberg, K and Stone, JL and Sulak, LR and Walter, CW and Goldhaber, M and Barszczak, T and Casper, D and Gajewski, W and Kropp,
WR and Mine, S and Price, LR and Smy, M and Sobel, HW and Vagins, MR and Ganezer, KS and Keig, WE and Ellsworth, RW and Tasaka, S and Kibayashi,
A and Learned, JG and Matsuno, S and Stenger, VJ and Takemori, D and Ishii,
T and Kanzaki, J and Kobayashi, T and Nakamura, K and Nishikawa, K and Oyama, Y and Sakai, A and Sakuda, M and Sasaki, O and Echigo, S and Kohama,
M and Suzuki, AT and Haines, TJ and Blaufuss, E and Kim, BK and Sanford, R and Svoboda, R and Chen, ML and Goodman, JA and Sullivan, GW and Hill, J and Jung, CK and Martens, K and Mauger, C and Mc Grew and C and Sharkey, E and Viren, B and Yanagisawa, C and Doki, W and Kirisawa, M and Inaba, S and Miyano, K and Okazawa, H and Saji, C and Takahashi, M and Takahata, M and Higuchi, K and Nagashima, Y and Takita, M and Yamaguchi, T and Yoshida,
M and Kim, SB and Etoh, M and Hasegawa, A and Hasegawa, T and Hatakeyama,
S and Iwamoto, T},
Title = {Observation of the East-West anisotropy of the atmospheric
neutrino flux},
Journal = {Physical Review Letters},
Volume = {82},
Number = {26},
Pages = {5194-5197},
Publisher = {American Physical Society (APS)},
Year = {1999},
Month = {January},
ISSN = {0031-9007},
url = {http://gateway.webofknowledge.com/gateway/Gateway.cgi?GWVersion=2&SrcApp=PARTNER_APP&SrcAuth=LinksAMR&KeyUT=WOS:000081152700004&DestLinkType=FullRecord&DestApp=ALL_WOS&UsrCustomerID=47d3190e77e5a3a53558812f597b0b92},
Abstract = {The east-west anisotropy, caused by the deflection of
primary cosmic rays in the Earth's magnetic field, is
observed for the first time in the flux of atmospheric
neutrinos. Using a 45 kt yr exposure of the Super-Kamiokande
detector, 552 e-like and 633 μ-like horizontally going
events are selected in the momentum range between 400 and
3000 MeV/c. The azimuthal distributions of e-like and
μ-like events agree with the expectation from atmospheric
neutrino flux calculations, verifying that the flux of
atmospheric neutrinos in the GeV energy range is reasonably
well modeled by calculations that account for the
geomagnetic field. © 1999 The American Physical
Society.},
Doi = {10.1103/PhysRevLett.82.5194},
Key = {Futagami99}
}
@booklet{Ambrosio99b,
Author = {Ambrosio, M and Antolini, R and Aramo, C and Auriemma, G and Baldini, A and Barbarino, GC and Barish, BC and Battistoni, G and Bellotti, R and Bemporad, C and Bernardini, P and Bilokon, H and Bisi, V and Bloise, C and Bower, C and Bussino, S and Cafagna, F and Calicchio, M and Campana, D and Carboni, M and Castellano, M and Cecchini, S and Cei, F and Chiarella,
V and Coutu, S and de Benedictis, L and de Cataldo, G and Dekhissi, H and de Marzo, C and de Mitri, I and de Vincenzi, M and di Credico, A and Erriquez, O and Favuzzi, C and Forti, C and Fusco, R and Giacomelli, G and Giannini, G and Giglietto, N and Grassi, M and Gray, L and Grillo, A and Guarino, F and Guarnaccia, P and Gustavino, C and Habig, A and Hanson,
K and Hawthorne, A and Heinz, R and Iarocci, E and Katsavounidis, E and Kearns, E and Kvriazopoulou, S and Lamanna, E and Lane, C and Levin, DS and Lipari, P and Longley, NP and Longo, MJ and Maaroufi, F and Mancarella,
G and Mandrioli, G and Manzoor, S and Margiotta Neri and A and Marini, A and Martello, D and Marzari-Chiesa, A and Mazziotta, MN and Mazzotta, C and Michael, DG and Mikheyev, S and Miller, L and Monacelli, P and Montaruli, T and Monteno, M and Mufson, S and Musser, J and Nicoló, D and Nolty, R and Okada, C and Orth, C and Osteria, G and Palamara, O and Patera, V and Patrizii, L and Pazzi, R and Peck, CW and Petrera, S and Pistilli, P and Popa, V and Rainó, A and Rastelli, A and Reynoldson, J and Ronga, F and Rubizzo, U and Sanzgiri, A and Satriano, C and Satta, L and Scapparone, E and Scholberg, K},
Title = {Relevance of the hadronic interaction model in the
interpretation of multiple muon data as detected with the
MACRO experiment},
Journal = {Nuclear Physics B - Proceedings Supplements},
Volume = {75},
Number = {1-2},
Pages = {265-268},
Publisher = {Elsevier BV},
Year = {1999},
Month = {January},
ISSN = {0920-5632},
url = {http://dx.doi.org/10.1016/s0920-5632(99)00261-3},
Abstract = {With the aim of discussing the effect of the possible
sources of systematic uncertainties in simulation models,
the analysis of multiple muon events from the MACRO
experiment at Gran Sasso is reviewed. In particular, the
predictions from different currently available hadronic
interaction models are compared.},
Doi = {10.1016/s0920-5632(99)00261-3},
Key = {Ambrosio99b}
}
@booklet{Ambrosio99c,
Author = {Ambrosio, and M, and others},
Title = {Observation of the shadowing of cosmic rays by the Moon
using a deep underground detector},
Journal = {Physical Review D},
Volume = {5901},
Number = {1},
Pages = {art. no.-012003},
Year = {1999},
Month = {January},
Abstract = {Using data collected by the MACRO experiment during the
years 1989-1996, we show evidence for the shadow of the Moon
in the underground cosmic ray flux with a significance of
3.6σ. This detection of the shadowing effect is the first
by an underground detector. A maximum-likelihood analysis is
used to determine that the angular resolution of the
apparatus is 0.9°±0.3°. These results demonstrate
MACRO'S capabilities as a muon telescope by confirming its
absolute pointing ability and quantifying its angular
resolution. ©1998 The American Physical
Society.},
Key = {Ambrosio99c}
}
@booklet{Fukuda99,
Author = {Fukuda, Y and Ishihara, K and Itow, Y and Kajita, T and Kameda, J and Kasuga, S and Kobayashi, K and Kobayashi, Y and Koshio, Y and Miura, M and Nakahata, M and Nakayama, S and Obayashi, Y and Okada, A and Okumura, K and Sakurai, N and Shiozawa, M and Suzuki, Y and Takeuchi, H and Takeuchi,
Y and Totsuka, Y and Yamada, S and Earl, M and Habig, A and Kearns, E and Messier, MD and Scholberg, K and Stone, JL and Sulak, LR and Walter, CW and Goldhaber, M and Barszczak, T and Casper, D and Gajewski, W and Kropp,
WR and Mine, S and Price, LR and Smy, M and Sobel, HW and Vagins, MR and Ganezer, KS and Keig, WE and Ellsworth, RW and Tasaka, S and Kibayashi,
A and Learned, JG and Matsuno, S and Stenger, VJ and Takemori, D and Ishii,
T and Ishino, H and Kobayashi, T and Nakamura, K and Oyama, Y and Sakai, A and Sakuda, M and Sasaki, O and Echigo, S and Kohama, M and Suzuki, AT and Inagaki, T and Nishikawa, K and Haines, TJ and Blaufuss, E and Kim, BK and Sanford, R and Svoboda, R and Chen, ML and Goodman, JA and Sullivan, GW and Hill, J and Jung, CK and Martens, K and Mauger, C and McGrew, C and Sharkey, E and Viren, B and Yanagisawa, C and Doki, W and Kirisawa, M and Inaba, S and Miyano, K and Okazawa, H and Saji, C and Takahashi, M and Takahata, M and Higuchi, K and Nagashima, Y and Takita, M and Yamaguchi,
T and Yoshida, M and Kim, SB and Etoh, M and Hasegawa, A and Hasegawa, T and Hatakeyama, S and Inoue, K and Iwamoto, T and Koga, M and Maruyama,
T},
Title = {Neutrino-induced upward stopping muons in
Super-Kamiokande},
Journal = {Physics Letters, Section B: Nuclear, Elementary Particle and
High-Energy Physics},
Volume = {467},
Number = {3-4},
Pages = {185-193},
Publisher = {Elsevier BV},
Year = {1999},
Month = {January},
ISSN = {0370-2693},
url = {http://dx.doi.org/10.1016/S0370-2693(99)01188-0},
Abstract = {A total of 137 upward stopping muons of minimum energy 1.6
GeV are observed by Super-Kamiokande during 516 detector
live days. The measured muon flux is 0.39 ± 0.04(stat.) ±
0.02(syst.) × 10-13 cm-2s-1sr-1 compared to an expected
flux of 0.73 ± 0.16(theo.) × 10-13 cm-2s-1sr-1. Using our
previously-published measurement of the upward through-going
muon flux, we calculate the stopping/through-going flux
ratio ℛ, which has less theoretical uncertainty. The
measured value of ℛ = 0.22 ± 0.02(stat.) ± 0.01(syst.)
is significantly smaller than the value 0.37-0.04+0.05(theo.)
expected using the best theoretical information (the
probability that the measured ℛ is a statistical
fluctuation below the expected value is 0.39%). A
simultaneous fitting to zenith angle distributions of upward
stopping and through-going muons gives a result which is
consistent with the hypothesis of neutrino oscillations with
the parameters sin22θ > 0.7 and 1.5 × 10-3 < Δm2 < 1.5 ×
10-2 eV2 at 90% confidence level, providing a confirmation
of the observation of neutrino oscillations by
Super-Kamiokande using the contained atmospheric neutrino
events. © 1999 Published by Elsevier Science B.V. All
rights reserved.},
Doi = {10.1016/S0370-2693(99)01188-0},
Key = {Fukuda99}
}
@article{fds326731,
Author = {Battistoni, G},
Title = {Experimental study of hadronic interaction models using
coincident data from EAS-TOP and MACRO},
Journal = {Nuclear Physics B - Proceedings Supplements},
Volume = {70},
Number = {1-3},
Pages = {483-485},
Publisher = {Elsevier BV},
Year = {1999},
Month = {January},
url = {http://dx.doi.org/10.1016/s0920-5632(98)00477-0},
Doi = {10.1016/s0920-5632(98)00477-0},
Key = {fds326731}
}
@article{fds304626,
Author = {Ambrosio, M and Antolini, R and Aramo, C and Auriemma, G and Baldini, A and Barbarino, GC and Barish, BC and Battistoni, G and Bellotti, R and Bemporad, C and Bernardini, P and Bilokon, H and Bisi, V and Bloise, C and Bower, C and Bussino, S and Cafagna, F and Calicchio, M and Campana, D and Carboni, M and Castellano, M and Cecchini, S and Cei, F and Chiarella,
V and Choudhary, BC and Coutu, S and Benedictis, L and Cataldo, G and Dekhissi, H and Marzo, C and Mitri, I and Derkaoui, J and Vincenzi, M and Credico, A and Erriquez, O and Favuzzi, C and Forti, C and Fusco, P and Giacomelli, G and Giannini, G and Giglietto, N and Giorgini, M and Grassi, M and Gray, L and Grillo, A and Guarino, F and Guarnaccia, P and Gustavino, C and Habig, A and Hanson, K and Heinz, R and Huang, Y and Iarocci, E and Katsavounidis, E and Kearns, E and Kim, H and Kyriazopoulou, S and Lamanna, E and Lane, C and Levin, DS and Lipari, P and Longley, NP and Longo, MJ and Maaroufi, F and Mancarella, G and Mandrioli, G and Manzoor, S and Neri, AM and Marini, A and Martello, D and Marzari-Chiesa, A and Mazziotta, MN and Mazzotta, C and Michael, DG and Mikheyev, S and Miller, L and Monacelli, P and Montaruli, T and Monteno,
M and Mufson, S and Musser, J and Nicoló, D and Orth, C and Osteria, G and Ouchrif, M and Palamara, O and Patera, V and Patrizii, L and Pazzi, R and Peck, CW and Petrera, S and Pistilli, P and Popa, V and Pugliese, V and Rainò, A and Reynoldson, J and Ronga, F and Rubizzo, U and Satriano, C and Satta, L},
Title = {Observation of the shadowing of cosmic rays by the Moon
using a deep underground detector},
Journal = {Physical Review D - Particles, Fields, Gravitation and
Cosmology},
Volume = {59},
Number = {1},
Pages = {1-7},
Publisher = {American Physical Society (APS)},
Year = {1999},
Month = {January},
url = {http://dx.doi.org/10.1103/PhysRevD.59.012003},
Abstract = {Using data collected by the MACRO experiment during the
years 1989–1996, we show evidence for the shadow of the
Moon in the underground cosmic ray flux with a significance
of 3.6σ. This detection of the shadowing effect is the
first by an underground detector. A maximum-likelihood
analysis is used to determine that the angular resolution of
the apparatus is [Formula Presented] These results
demonstrate MACRO’s capabilities as a muon telescope by
confirming its absolute pointing ability and quantifying its
angular resolution. © 1998 The American Physical
Society.},
Doi = {10.1103/PhysRevD.59.012003},
Key = {fds304626}
}
@article{fds304628,
Author = {Ambrosio, M and Antolini, R and Aramo, C and Auriemma, G and Baldini, A and Barbarino, GC and Barish, BC and Battistoni, G and Bellotti, R and Bemporad, C and Bernardini, E and Bernardini, P and Bilokon, H and Bisi,
V and Bloise, C and Bower, C and Bussino, S and Cafagna, F and Calicchio,
M and Campana, D and Carboni, M and Castellano, M and Cecchini, S and Cei,
F and Chiarella, V and Choudhary, BC and Coutu, S and De Benedictis and L and De Cataldo and G and Dekhissi, H and De Marzo and C and De Mitri and I and Derkaoui, J and De Vincenzi and M and Di Credico and A and Diehl, E and Erriquez, O and Favuzzi, C and Forti, C and Fusco, P and Giacomelli, G and Giannini, G and Giglietto, N and Giorgini, M and Grassi, M and Gray, L and Grillo, A and Guarino, F and Guarnaccia, P and Gustavino, C and Habig,
A and Hanson, K and Heinz, R and Huang, Y and Iarocci, E and Katsavounidis,
E and Katsavounidis, I and Kearns, E and Kim, H and Kyriazopoulou, S and Lamanna, E and Lane, C and Lari, T and Levin, DS and Lipari, P and Longley,
NP and Longo, MJ and Maaroufi, F and Mancarella, G and Mandrioli, G and Manzoor, S and Margiotta Neri and A and Marini, A and Martello, D and Marzari-Chiesa, A and Mazziotta, MN and Mazzotta, C and Michael, DG and Mikheyev, S and Miller, L and Monacelli, P and Montaruli, T and Monteno,
M and Mufson, S and Musser, J and Nicoló, D and Orth, C and Osteria, G and Ouchrif, M and Palamara, O and Patera, V and Patrizii, L and Pazzi, R and Peck, CW and Petrera, S and Pistilli, P and Popa, V and Rainò, A and Rastelli, A and Reynoldson, J},
Title = {Limits on dark matter WIMPs using upward-going muons in the
MACRO detector},
Journal = {Physical Review D - Particles, Fields, Gravitation and
Cosmology},
Volume = {60},
Number = {8},
Pages = {1-10},
Publisher = {American Physical Society (APS)},
Year = {1999},
Month = {January},
url = {http://dx.doi.org/10.1103/PhysRevD.60.082002},
Abstract = {We perform an indirect search for weakly interacting massive
particles (WIMPs) using the MACRO detector to look for
neutrino-induced upward-going muons resulting from the
annihilation of WIMPs trapped in the Sun and Earth. The
search is conducted in various angular cones centered on the
Sun and Earth to accommodate a range of WIMP masses. No
significant excess over the background from atmospheric
neutrinos is seen. We set experimental flux limits on the
upward-going muon fluxes from the Sun and the Earth. These
limits are used to constrain neutralino particle parameters
from supersymmetric theory, including those suggested by
recent results from DAMA-NaI. © 1999 The American Physical
Society.},
Doi = {10.1103/PhysRevD.60.082002},
Key = {fds304628}
}
@article{fds304627,
Author = {Ambrosio, M and Antolini, R and Aramo, C and Auriemma, G and Baldini, A and Barbarino, GC and Barish, BC and Battistoni, G and Bellotti, R and Bemporad, C and Bernardini, E and Bernardini, P and Bilokon, H and Bisi,
V and Bloise, C and Bower, C and Bussino, S and Cafagna, F and Calicchio,
M and Campana, D and Carboni, M and Castellano, M and Cecchini, S and Cei,
F and Chiarella, V and Choudhary, BC and Coutu, S and De Cataldo and G and Dekhissi, H and De Marzo and C and De Mitri and I and Derkaoui, J and De
Vincenzi, M and Di Credico and A and Erriquez, O and Favuzzi, C and Forti,
C and Fusco, P and Giacomelli, G and Giannini, G and Giglietto, N and Giorgini, M and Grassi, M and Gray, L and Grillo, A and Guarino, F and Gustavino, C and Habig, A and Hanson, K and Heinz, R and Huang, Y and Iarocci, E and Katsavounidis, E and Katsavounidis, I and Kearns, E and Kim, H and Kyriazopoulou, S and Lamanna, E and Lane, C and Lari, T and Levin, DS and Lipari, P and Longley, NP and Longo, MJ and Loparco, F and Maaroufi, F and Mancarella, G and Mandrioli, G and Manzoor, S and Margiotta Neri and A and Marini, A and Martello, D and Marzari-Chiesa,
A and Mazziotta, MN and Mazzotta, C and Michael, DG and Mikheyev, S and Miller, L and Monacelli, P and Montaruli, T and Monteno, M and Mufson,
S and Musser, J and Nicoló, D and Orth, C and Osteria, G and Ouchrif, M and Palamara, O and Patera, V and Patrizii, L and Pazzi, R and Peck, CW and Petrera, S and Pistilli, P and Popa, V and Rainò, A and Rastelli, A and Reynoldson, J and Ronga, F and Rubizzo, U},
Title = {High statistics measurement of the underground muon pair
separation at Gran Sasso},
Journal = {Physical Review D - Particles, Fields, Gravitation and
Cosmology},
Volume = {60},
Number = {3},
Pages = {1-13},
Publisher = {American Physical Society (APS)},
Year = {1999},
Month = {January},
url = {http://dx.doi.org/10.1103/PhysRevD.60.032001},
Abstract = {We present a measurement of the underground decoherence
function using multi-muon events observed in the MACRO
detector at Gran Sasso at an average depth of (Formula
presented) Muon pair separations up to 70 m have been
measured, corresponding to parent mesons with (Formula
presented)–(Formula presented) Improved selection criteria
are used to reduce detector effects mainly in the low
distance separation region of muon pairs. Special care is
given to a new unfolding procedure designed to minimize
systematic errors in the numerical algorithm. The accuracy
of the measurement is such that the possible contribution of
rare processes, such as (Formula presented) can be
experimentally studied. The measured decoherence function is
compared with the predictions of the hadronic interaction
model of the HEMAS Monte Carlo code. Good agreement is
obtained. We interpret this agreement to indicate that no
anomalous (Formula presented) components in soft
hadron-nucleus and nucleus-nucleus collisions are required
by the MACRO experimental data. Preliminary comparisons with
other Monte Carlo codes point out that the uncertainties
associated with the hadronic interaction model may be as
large as 20%, depending on the energy. MACRO data can be
used as a benchmark for future work on the discrimination of
shower models in the primary energy region around and below
the knee of the spectrum. © 1999 The American Physical
Society.},
Doi = {10.1103/PhysRevD.60.032001},
Key = {fds304627}
}
@article{fds337394,
Author = {Battistoni, G},
Title = {Study of photonuclear interaction of muons in rock with the
MACRO experiment},
Journal = {VULCANO WORKSHOP 1998 - FRONTIER OBJECTS IN ASTROPHYSICS AND
PARTICLE PHYSICS},
Volume = {65},
Pages = {419-427},
Publisher = {SOC ITALIANA FISICA},
Editor = {Giovannelli, F and Mannocchi, G},
Year = {1999},
Month = {January},
ISBN = {88-7794-214-2},
Key = {fds337394}
}
@booklet{Nakahata99,
Author = {Nakahata, M and Fukuda, Y and Hayakawa, T and Ichihara, E and Inoue, K and Ishihara, K and Ishino, H and Itow, Y and Kajita, T and Kameda, J and Kasuga, S and Kobayashi, K and Kobayashi, Y and Koshio, Y and Martens,
K and Miura, M and Nakayama, S and Okada, A and Okumura, K and Sakurai, N and Shiozawa, M and Suzuki, Y and Takeuchi, Y and Totsuka, Y and Yamada, S and Earl, M and Habig, A and Kearns, E and Messier, MD and Scholberg, K and Stone, JL and Sulak, LR and Walter, CW and Goldhaber, M and Barszczak,
T and Casper, D and Gajewski, W and Halverson, PG and Hsu, J and Kropp, WR and Price, LR and Reines, F and Smy, M and Sobel, HW and Vagins, MR and Ganezer, KS and Keig, WE and Ellsworth, RW and Tasaka, S and Flanagan,
JW and Kibayashi, A and Learned, JG and Matsuno, S and Stenger, VJ and Takemori, D and Ishii, T and Kanzaki, J and Kobayashi, T and Mine, S and Nakamura, K and Nishikawa, K and Oyama, Y and Sakai, A and Sakuda, M and Sasaki, O and Echigo, S and Kohama, M and Suzuki, AT and Haines, TJ and Blaufuss, E and Kim, BK and Sanford, R and Svoboda, R and Chen, ML and Conner, Z and Goodman, JA and Sullivan, GW and Hill, J and Jung, CK and Mauger, C and McGrew, C and Sharkey, E and Viren, B and Yanagisawa, C and Doki, W and Miyano, K and Okazawa, H and Saji, C and Takahata, M and Nagashima, Y and Takita, M and Yamaguchi, T and Yoshida, M and Kim, SB and Etoh, M and Fujita, K and Hasegawa, A and Hasegawa, T and Hatakeyama,
S},
Title = {Calibration of Super-Kamiokande using an electron
LINAC},
Journal = {Nuclear Instruments and Methods in Physics Research, Section
A: Accelerators, Spectrometers, Detectors and Associated
Equipment},
Volume = {421},
Number = {1-2},
Pages = {113-129},
Publisher = {Elsevier BV},
Year = {1999},
Month = {January},
ISSN = {0168-9002},
url = {http://dx.doi.org/10.1016/S0168-9002(98)01200-5},
Abstract = {In order to calibrate the Super-Kamiokande experiment for
solar neutrino measurements, a linear accelerator (LINAC)
for electrons was installed at the detector. LINAC data were
taken at various positions in the detector volume, tracking
the detector response in the variables relevant to solar
neutrino analysis. In particular, the absolute energy scale
is now known with less than 1% uncertainty. © 1999 Elsevier
Science B.V. All rights reserved.},
Doi = {10.1016/S0168-9002(98)01200-5},
Key = {Nakahata99}
}
@booklet{Ambrosio99,
Author = {Ambrosio, and M, and others},
Title = {Limits on dark matter WIMPs using upward-going muons in the
MACRO detector},
Journal = {Physical Review D},
Volume = {6008},
Number = {8},
Pages = {art. no.-082002},
Year = {1999},
Month = {October},
Abstract = {We perform an indirect search for weakly interacting massive
particles (WIMPs) using the MACRO detector to look for
neutrino-induced upward-going muons resulting from the
annihilation of WIMPs trapped in the Sun and Earth. The
search is conducted in various angular cones centered on the
Sun and Earth to accommodate a range of WIMP masses. No
significant excess over the background from atmospheric
neutrinos is seen. We set experimental flux limits on the
upward-going muon fluxes from the Sun and the Earth. These
limits are used to constrain neutralino particle parameters
from supersymmetric theory, including those suggested by
recent results from DAMA-NaI. ©1999 The American Physical
Society.},
Key = {Ambrosio99}
}
@article{fds248732,
Author = {Ambrosio, M and Antolini, R and Auriemma, G and Bakari, D and Baldini,
A and Barbarino, GC and Barish, BC and Battistoni, G and Bellotti, R and Bemporad, C and Bernardini, P and Bilokon, H and Bisi, V and Bloise, C and Bower, C and Brigida, M and Bussino, S and Cafagna, F and Calicchio, M and Campana, D and Carboni, M and Cecchini, S and Cei, F and Chiarella, V and Choudhary, BC and Coutu, S and Cataldo, GD and Dekhissi, H and Marzo,
CD and Mitri, ID and Derkaoui, J and Vincenzi, MD and Credico, AD and Erriquez, O and Favuzzi, C and Forti, C and Fusco, P and Giacomelli, G and Giannini, G and Giglietto, N and Giorgini, M and Grassi, M and Gray, L and Grillo, A and Guarino, F and Gustavino, C and Habig, A and Hanson, K and Heinz, R and Iarocci, E and Katsavounidis, E and Katsavounidis, I and Kearns, E and Kim, H and Kyriazopoulou, S and Lamanna, E and Lane, C and Levin, DS and Lipari, P and Longley, NP and Longo, MJ and Loparco, F and Maaroufi, F and Mancarella, G and Mandrioli, G and Margiotta, A and Marini, A and Martello, D and Marzari-Chiesa, A and Mazziotta, MN and Michael, DG and Mikheyev, S and Miller, L and Monacelli, P and Montaruli, T and Monteno, M and Mufson, S and Musser, J and Nicolò, D and Nolty, R and Orth, C and Okada, C and Osteria, G and Ouchrif, M and Palamara, O and Patera, V and Patrizii, L and Pazzi, R and Peck, CW and Perrone, L and Petrera, S and Pistilli, P and Popa, V and Rainò, A and Reynoldson, J and Ronga, F and Satriano, C and Satta, L and Scapparone,
E and Scholberg, K and Sciubba, A and Serra, P and Sioli, M and Sitta, M and Spinelli, P and Spinetti, M and Spurio, M and Steinberg, R and Stone,
JL and Sulak, LR and Surdo, A and Tarlè, G and Togo, V and Vakili, M and Vilela, E and Walter, CW and Webb, R},
Title = {Search for lightly ionizing particles with the MACRO
detector},
Journal = {Physical Review D - Particles, Fields, Gravitation and
Cosmology},
Volume = {62},
Number = {5},
Pages = {1-9},
Year = {2000},
ISSN = {0556-2821},
Abstract = {A search for lightly ionizing particles has been performed
with the MACRO detector. This search was sensitive to
particles with charges between 1/5 e and close to the charge
of an electron, with β between approximately 0.25 and 1.0.
Unlike previous searches both single track events and tracks
buried within high multiplicity muon showers were examined.
In a period of approximately one year no candidates were
observed. Assuming an isotropic flux, for the single track
sample this corresponds to a 90% C.L. upper flux limit Φ
≤9.2×10-15 cm-2 s-1 sr-1. ©2000 The American Physical
Society.},
Key = {fds248732}
}
@article{Ambrosio:1999gj,
Author = {Ambrosio et al., M},
Title = {Nuclearite search with the MACRO detector at Gran
Sasso},
Journal = {The European Physical Journal C},
Volume = {13},
Number = {3},
Pages = {453-453},
Publisher = {Springer Science and Business Media LLC},
Year = {2000},
ISSN = {1434-6044},
url = {http://gateway.webofknowledge.com/gateway/Gateway.cgi?GWVersion=2&SrcApp=PARTNER_APP&SrcAuth=LinksAMR&KeyUT=WOS:000086888100006&DestLinkType=FullRecord&DestApp=ALL_WOS&UsrCustomerID=47d3190e77e5a3a53558812f597b0b92},
Abstract = {http://arxiv.org/abs/hep-ex/9904031},
Doi = {10.1007/s100520050708},
Key = {Ambrosio:1999gj}
}
@article{fds248731,
Author = {Patrizii, L and Ambrosio, M and Antolini, R and Aramo, C and Auriemma,
G and Bakari, D and Baldini, A and Barbarino, GC and Barish, BC and Battistoni, G and Bellotti, R and Bemporad, C and Bernardini, P and Bilokon, H and Bisi, V and Bloise, C and Bower, C and Bussino, S and Cafagna, F and Calicchio, M and Campana, D and Carboni, M and Castellano, M and Cecchini, S and Cei, F and Chiarella, V and Choudhary,
BC and Coutu, S and de Benedicts, L and de Cataldo, G and Dekhissi, H and de Marzo, C and de Mitri, I and Derkaoui, J and de Vincenzi, M and di
Credico, A and Erriquez, O and Favuzzi, C and Forti, C and Fusco, P and Giacomelli, G and Giannini, G and Giglietto, N and Giorgini, M and Grassi, M and Gray, L and Grillo, A and Guarino, F and Guarnaccia, P and Gustavino, C and Habig, A and Hanson, K and Heinz, R and Huang, Y and Iarocci, E and Katsavounidis, E and Katsavounidis, I and Kearns, E and Kim, H and Kyriazopoulou, S and Lamanna, E and Lane, C and Lari, T and Levin, DS and Lipari, P and Longley, NP and Longo, MJ and Maaroufi, F and Mancarella, G and Mandrioli, G and Manzoor, S and Margiotta, A and Marini, A and Martello, D and Marzari-Chiesa, A and Mazziotta, MN and Michael, DG and Mikheyev, S and Miller, L and Monacelli, P and Montaruli, T and Monteno, M and Mufson, S and Musser, J and Nicoló, D and Orth, C and Osteria, G and Ouchrif, M and Palamara, O and Patera, V and Pazzi, R and Peck, CW and Perrone, L and Petrera, S and Pistilli, P and Popa, V and Pugliese, V and Rainò, A and Ftastelli,
A},
Title = {Search for massive rare particles with the MACRO detector at
Gran Sasso},
Journal = {Nuclear Physics B - Proceedings Supplements},
Volume = {85},
Number = {1-3},
Pages = {221-226},
Publisher = {Elsevier BV},
Year = {2000},
Month = {January},
ISSN = {0920-5632},
url = {http://dx.doi.org/10.1016/S0920-5632(00)00510-7},
Abstract = {Searches for massive penetrating particles in the cosmic
radiation have been performed with the MACRO detector.
Scintillators, streamer tubes (instrumented with specialized
electronics) and nuclear track detectors have been used to
search for signatures coming from magnetic monopoles (MMs);
the scintillator and the nuclear track subdetectors were
also used for searches for other rare particles
(nuclearites, charged Q-balls). Based on no observation of
such signals, we establish stringent flux limits, for MMs as
slow as a few 10-5 c.},
Doi = {10.1016/S0920-5632(00)00510-7},
Key = {fds248731}
}
@article{Ambrosio:2000ja,
Author = {Ambrosio, M and Antolini, R and Auriemma, G and Bakari, D and Baldini,
A and Barbarino, GC and Barish, BC and Battistoni, G and Bellotti, R and Bemporad, C and Bernardini, P and Bilokon, H and Bisi, V and Bloise, C and Bower, C and Brigida, M and Bussino, S and Cafagna, F and Calicchio, M and Campana, D and Carboni, M and Cecchini, S and Cei, F and Chiarella, V and Choudhary, BC and Coutu, S and De Cataldo and G and Dekhissi, H and De
Marzo, C and De Mitri and I and Derkaoui, J and De Vincenzi and M and Di
Credico, A and Erriquez, O and Favuzzi, C and Forti, C and Fusco, P and Giacomelli, G and Giannini, G and Giglietto, N and Giorgini, M and Grassi, M and Gray, L and Grillo, A and Guarino, F and Gustavino, C and Habig, A and Hanson, K and Heinz, R and Iarocci, E and Katsavounidis, E and Katsavounidis, I and Kearns, E and Kim, H and Kyriazopoulou, S and Lamanna, E and Lane, C and Levin, DS and Lipari, P and Longley, NP and Longo, MJ and Loparco, F and Maaroufi, F and Mancarella, G and Mandrioli, G and Margiotta, A and Marini, A and Martello, D and Marzari-Chiesa, A and Mazziotta, MN and Michael, DG and Mikheyev, S and Miller, L and Monacelli, P and Montaruli, T and Monteno, M and Mufson,
S and Musser, J and Nicolòm, D and Nolty, R and Orth, C and Osteria, G and Ouchrif, M and Palamara, O and Patera, V and Patrizii, L and Pazzi, R and Peck, CW and Perrone, L and Petrera, S and Pistilli, P and Popa, V and Rainòa, A and Reynoldson, J and Ronga, F and Satriano, C and Satta, L and Scapparone, E and Scholberg, K and Sciubba, A},
Title = {Low energy atmospheric muon neutrinos in
MACRO},
Journal = {Physics Letters, Section B: Nuclear, Elementary Particle and
High-Energy Physics},
Volume = {478},
Number = {1-3},
Pages = {5-13},
Publisher = {Elsevier BV},
Year = {2000},
Month = {April},
ISSN = {0370-2693},
url = {http://gateway.webofknowledge.com/gateway/Gateway.cgi?GWVersion=2&SrcApp=PARTNER_APP&SrcAuth=LinksAMR&KeyUT=WOS:000086540600002&DestLinkType=FullRecord&DestApp=ALL_WOS&UsrCustomerID=47d3190e77e5a3a53558812f597b0b92},
Abstract = {We present the measurement of two event samples induced by
atmospheric v(μ) of average energy Ē(ν) ~ 4 GeV. In the
first sample, a neutrino interacts inside the MACRO detector
producing an upward-going muon leaving the apparatus. The
ratio of the number of observed to expected events is 0.57
± 0.05(stat) ± 0.06(syst) ± 0.14(theor) with an angular
distribution similar to that expected from the Bartol
atmospheric neutrino flux. The second is a mixed sample of
internally produced downward-going muons and externally
produced upward-going muons stopping inside the detector.
These two subsamples are selected by topological criteria;
the lack of timing information makes it impossible to
distinguish stopping from downgoing muons. The ratio of the
number of observed to expected events is 0.71 ± 0.05(stat)
± 0.07(syst) ± 0.18(theor). The observed deficits in each
subsample is in agreement with neutrino oscillations,
although the significance is reduced by the large
theoretical errors. However, the ratio of the two samples
causes a large cancellation of theoretical and of some
systematic errors. With the ratio, we rule out the
no-oscillation hypothesis at 95% c.1. Furthermore, the ratio
tests the pathlength dependence of possible oscillations.
The data of both samples and their ratio favor maximal
mixing and Δm2 ~ 10-3-10-2 eV2. These parameters are in
agreement with our results from upward throughgoing muons,
induced by v(μ) of much higher energies. (C) 2000 Elsevier
Science B.V.},
Doi = {10.1016/S0370-2693(00)00267-7},
Key = {Ambrosio:2000ja}
}
@article{fds326730,
Author = {Akhmadaliev, S and Albiol, F and Amaral, P and Ambrosini, G and Amorim,
A and Anderson, K and Andrieux, ML and Aubert, B and Augé, E and Badaud,
F and Baisin, L and Barreiro, F and Battistoni, G and Bazan, A and Bazizi,
K and Bee, C and Belorgey, J and Belymam, A and Benchekroun, D and Berglund, S and Berset, JC and Blanchot, G and Bogush, A and Bohm, C and Boldea, V and Bonivento, W and Borgeaud, P and Borisov, O and Bosman, M and Bouhemaid, N and Breton, D and Brette, P and Bromberg, C and Budagov, J and Burdin, S and Caloba, L and Camarena, F and Camin, DV and Canton, B and Caprini, M and Carvalho, J and Casado, P and Cases, R and Castillo, MV and Cavalli, D and Cavalli-Sforza, M and Cavasinni, V and Chadelas, R and Chalifour, M and Chekhtman, L and Chevalley, JL and Chirikov-Zorin,
I and Chlachidze, G and Chollet, JC and Citterio, M and Cleland, WE and Clement, C and Cobal, M and Cogswell, F and Colas, J and Collot, J and Cologna, S and Constantinescu, S and Costa, G and Costanzo, D and Coulon, JP and Crouau, M and Dargent, P and Daudon, F and David, M and Davidek, T and Dawson, J and De, K and Delagnes, E and de la Taille, C and Del Peso and J and Del Prete and T and de Saintignon, P and di Girolamo, B and Dinkespiller, B and Dita, S and Djama, F and Dodd, J and Dolejsi, J and Dolezal, Z and Downing, R and Dugne, JJ and Duval, PY and Dzahini, D and Efthymiopoulos, I and Errede, D and Errede, S and Etienne, F and Evans,
H and Eynard, G and Farida, F and Fassnacht, P and Fedyakin, N and de
Fernandez Troconiz and J and Ferrari, A},
Title = {Results from a new combined test of an electromagnetic
liquid argon calorimeter with a hadronic scintillating-tile
calorimeter},
Journal = {Nuclear Instruments and Methods in Physics Research, Section
A: Accelerators, Spectrometers, Detectors and Associated
Equipment},
Volume = {449},
Number = {3},
Pages = {461-477},
Publisher = {Elsevier BV},
Year = {2000},
Month = {July},
url = {http://dx.doi.org/10.1016/S0168-9002(00)00153-4},
Abstract = {A new combined test of an electromagnetic liquid argon
accordion calorimeter and a hadronic scintillating-tile
calorimeter was carried out at the CERN SPS. These devices
are prototypes of the barrel calorimeter of the future ATLAS
experiment at the LHC. The energy resolution of pions in the
energy range from 10 to 300 GeV at an incident angle θ of
about 12° is well described by the expression σ/E = ((41.9
± 1.6)%/√E + (1.8 ± 0.1)%)⊕(1.8 ± 0.1)/E, where E is
in GeV. The response to electrons and muons was evaluated.
Shower profiles, shower leakage and the angular resolution
of hadronic showers were also studied. Results are compared
with those from the previous beam test.},
Doi = {10.1016/S0168-9002(00)00153-4},
Key = {fds326730}
}
@article{Suzuki:2000nj,
Author = {Suzuki, A and Park, H and Aoki, S and Echigo, S and Fujii, K and Hara, T and Iwashita, T and Kitamura, M and Kohama, M and Kume, G and Onchi, M and Otaki, T and Sato, K and Takatsuki, M and Takenaka, K and Tanaka, Y and Tashiro, K and Inagaki, T and Kato, I and Mukai, S and Nakaya, T and Nishikawa, K and Sasao, N and Shima, A and Yokoyama, H and Chikamatsu,
T and Hayato, Y and Ishida, T and Ishii, T and Ishino, H and Jeon, EJ and Kobayashi, T and Lee, SB and Nakamura, K and Oyama, Y and Sakai, A and Sakuda, M and Tumakov, V and Fukuda, S and Fukuda, Y and Ishizuka, M and Itow, Y and Kajita, T and Kameda, J and Kaneyuki, K and Kobayashi, K and Kobayashi, Y and Koshio, Y and Miura, M and Moriyama, S and Nakahata, M and Nakayama, S and Obayashi, Y and Okada, A and Sakurai, N and Shiozawa, M and Suzuki, Y and Takeuchi, H and Takeuchi, Y and Totsuka, Y and Toshito, T and Yamada, S and Miyano, K and Nakamura, M and Tamura, N and Nakano, I and Yoshida, M and Kadowaki, T and Kishi, S and Maruyama, T and Etoh, M and Nishijima, K and Bhang, HC and Khang, BH and Kim, BJ and Kim, HI and Kim,
JH and Kim, SB and So, H and Yoo, JH and Choi, JH and Jang, HI and Jang, JS and Kim, JY and Lim, IT and Pac, MY and Kearns, E and Scholberg, K and Stone,
JL and Sulak, LR and Walter, CW and Casper, D and Gajewski, W and Kropp, W and Mine, S and Sobel, H and Vagins, M and Matsuno, S and Hill,
J},
Title = {Design, construction, and operation of SciFi tracking
detector for K2K experiment},
Journal = {Nuclear Instruments and Methods in Physics Research, Section
A: Accelerators, Spectrometers, Detectors and Associated
Equipment},
Volume = {453},
Number = {1-2},
Pages = {165-176},
Publisher = {Elsevier BV},
Year = {2000},
Month = {October},
ISSN = {0168-9002},
url = {http://arxiv.org/pdf/hep-ex/0004024},
Abstract = {We describe the construction and performance of a
scintillating fiber detector used in the near detector for
the K2K (KEK to Kamioka, KEK E362) long baseline neutrino
oscillation experiment. The detector uses 3.7 m long and
0.692 mm diameter scintillating fiber coupled to
image-intensifier tubes (IIT), and a CCD camera readout
system. Fiber sheet production and detector construction
began in 1997, and the detector was commissioned in March
1999. Results from the first K2K runs confirm good initial
performance: position resolution is estimated to be about
0.8 mm, and track finding efficiency is 98±2% for long
tracks (i.e., those which intersect more than 5 fiber
planes). The hit efficiency was estimated to be 92±2% using
cosmic-ray muons, after noise reduction at the offline
stage. The possibility of using the detector for particle
identification is also discussed.},
Doi = {10.1016/S0168-9002(00)00624-0},
Key = {Suzuki:2000nj}
}
@article{Fukuda:2000np,
Author = {Fukuda, S and Fukuda, Y and Ishitsuka, M and Kajita, T and Kameda, J and Kaneyuki, K and Kobayashi, K and Koshio, Y and Miura, M and Moriyama, S and Nakahata, M and Nakayama, S and Obayashi, Y and Okada, A and Okumura, K and Sakurai, N and Shiozawa, M and Suzuki, Y and Takeuchi, H and Takeuchi,
Y and Toshito, T and Totsuka, Y and Yamada, S and Earl, M and Habig, A and Kearns, E and Messier, MD and Scholberg, K and Stone, JL and Sulak, LR and Walter, CW and Goldhaber, M and Barszczak, T and Casper, D and Gajewski,
W and Kropp, WR and Mine, S and Price, LR and Smy, M and Sobel, HW and Vagins,
MR and Ganezer, KS and Keig, WE and Ellsworth, RW and Tasaka, S and Kibayashi, A and Learned, JG and Matsuno, S and Takemori,
D},
Title = {Tau neutrinos favored over sterile neutrinos in atmospheric
muon neutrino oscillations.},
Journal = {Physical review letters},
Volume = {85},
Number = {19},
Pages = {3999-4003},
Year = {2000},
Month = {November},
ISSN = {0031-9007},
url = {http://www.ncbi.nlm.nih.gov/pubmed/11056609},
Abstract = {The previously published atmospheric neutrino data did not
distinguish whether muon neutrinos were oscillating into tau
neutrinos or sterile neutrinos, as both hypotheses fit the
data. Using data recorded in 1100 live days of the
Super-Kamiokande detector, we use three complementary data
samples to study the difference in zenith angle distribution
due to neutral currents and matter effects. We find no
evidence favoring sterile neutrinos, and reject the
hypothesis at the 99% confidence level. On the other hand,
we find that oscillation between muon and tau neutrinos
suffices to explain all the results in hand.},
Doi = {10.1103/physrevlett.85.3999},
Key = {Fukuda:2000np}
}
@article{Ambrosio:2000kh,
Author = {Ambrosio, M and Antolini, R and Auriemma, G and Bakari, D and Baldini,
A and Barbarino, GC and Barish, BC and Battistoni, G and Bellotti, R and Bemporad, C and Bernardini, P and Bilokon, H and Bisi, V and Bloise, C and Bower, C and Brigida, M and Bussino, S and Cafagna, F and Calicchio, M and Campana, D and Carboni, M and Cecchini, S and Cei, F and Chiarella, V and Choudhary, BC and Coutu, S and De Cataldo and G and Dekhissi, H and De
Marzo, C and De Mitri and I and Derkaoui, J and De Vincenzi and M and Di
Credico, A and Erriquez, O and Favuzzi, C and Forti, C and Fusco, P and Giacomelli, G and Giannini, G and Giglietto, N and Giorgini, M and Grassi, M and Gray, L and Grillo, A and Guarino, F and Gustavino, C and Habig, A and Hanson, K and Heinz, R and Iarocci, E and Katsavounidis, E and Katsavounidis, I and Kearns, E and Kim, H and Kyriazopoulou, S and Lamanna, E and Lane, C and Levin, DS and Lipari, P and Longley, NP and Longo, MJ and Loparco, F and Maaroufi, F and Mancarella, G and Mandrioli, G and Margiotta, A and Marini, A and Martello, D and Marzari-Chiesa, A and Mazziotta, MN and Michael, DG and Mikheyev, S and Miller, L and Monacelli, P and Montaruli, T and Monteno, M and Mufson,
S and Musser, J and Nicolo, D and Nolty, R and Orth, C and Okada, C and Osteria, G and Ouchrif, M and Palamara, O and Patera, V and Patrizii, L and Pazzi, R and Peck, CW and Perrone, L and Petrera, S and Pistilli, P and Popa, V and Raino, A and Reynoldson, J and Ronga, F and Satriano, C and Satta, L and Scapparone, E},
Title = {Search for lightly ionizing particles with the MACRO
detector},
Journal = {Physical Review D},
Volume = {62},
Number = {5},
Pages = {9},
Publisher = {American Physical Society (APS)},
Year = {2000},
Month = {December},
ISSN = {0556-2821},
url = {http://gateway.webofknowledge.com/gateway/Gateway.cgi?GWVersion=2&SrcApp=PARTNER_APP&SrcAuth=LinksAMR&KeyUT=WOS:000089022500007&DestLinkType=FullRecord&DestApp=ALL_WOS&UsrCustomerID=47d3190e77e5a3a53558812f597b0b92},
Abstract = {A search for lightly ionizing particles has been performed
with the MACRO detector. This search was sensitive to
particles with charges between 1/5 e and close to the charge
of an electron, with β between approximately 0.25 and 1.0.
Unlike previous searches both single track events and tracks
buried within high multiplicity muon showers were examined.
In a period of approximately one year no candidates were
observed. Assuming an isotropic flux, for the single track
sample this corresponds to a 90% C.L. upper flux limit Φ
≤9.2×10-15 cm-2 s-1sr-1. © 2000 The American Physical
Society.},
Doi = {10.1103/PhysRevD.62.052003},
Key = {Ambrosio:2000kh}
}
@article{fds248733,
Author = {Blaufuss, E and Guillian, G and Fukuda, Y and Fukuda, S and Ishitsuka,
M and Itow, Y and Kajita, T and Kameda, J and Kaneyuki, K and Kobayashi, K and Kobayashi, Y and Koshio, Y and Miura, M and Moriyama, S and Nakahata, M and Nakayama, S and Obayashi, Y and Okada, A and Okumura, K and Sakurai, N and Shiozawa, M and Suzuki, Y and Takeuchi, H and Takeuchi, Y and Toshito,
T and Totsuka, Y and Yamada, S and Earl, M and Habig, A and Kearns, E and Messier, MD and Scholberg, K and Stone, JL and Sulak, LR and Walter, CW and Goldhaber, M and Barszczak, T and Casper, D and Gajewski, W and Kropp,
WR and Mine, S and Price, LR and Smy, M and Sobel, HW and Vagins, MR and Ganezer, KS and Keig, WE and Ellsworth, RW and Tasaka, S and Kibayashi,
A and Learned, JG and Matsuno, S and Takemori, D and Hayato, Y and Ishii,
T and Kobayashi, T and Nakamura, K and Oyama, Y and Sakai, A and Sakuda, M and Sasaki, O and Echigo, S and Kohama, M and Suzuki, AT and Inagaki, T and Nishikawa, K and Haines, TJ and Kim, BK and Sanford, R and Svoboda, R and Chen, ML and Goodman, JA and Sullivan, GW and Hill, J and Jung, CK and Martens, K and Malek, M and Mauger, C and McGrew, C and Sharkey, E and Viren, B and Yanagisawa, C and Kirisawa, M and Inaba, S and Mitsuda, C and Miyano, K and Okazawa, H and Saji, C and Takahashi, M and Takahata, M and Nagashima, Y and Nitta, K and Takita, M and Yoshida, M and Kim, SB and Etoh, M and Gando, Y and Hasegawa, T and Inoue, K},
Title = {16N as a calibration source for
Super-Kamiokande},
Journal = {Nuclear Instruments and Methods in Physics Research, Section
A: Accelerators, Spectrometers, Detectors and Associated
Equipment},
Volume = {458},
Number = {3},
Pages = {638-649},
Publisher = {Elsevier BV},
Year = {2001},
ISSN = {0168-9002},
url = {http://dx.doi.org/10.1016/S0168-9002(00)00900-1},
Abstract = {The decay of 16N is used to cross check the absolute energy
scale calibration for solar neutrinos established by the
electron linear accelerator (LINAC). A deuterium-tritium
neutron generator was employed to create 16N via the (n,p)
reaction on 16O in the water of the detector. This technique
is isotropic and has different systematic uncertainties than
the LINAC. The results from this high-statistics data sample
agree with the absolute energy scale of the LINAC to better
than 1%. A natural source of 16N from the capture of μ- on
16O, which is collected as a background to the solar
neutrino analysis, is also discussed.},
Doi = {10.1016/S0168-9002(00)00900-1},
Key = {fds248733}
}
@article{Ambrosio:2000yx,
Author = {Ambrosio, M and Antolini, R and Auriemma, G and Bakari, D and Baldini,
A and Barbarino, GC and Barish, BC and Battistoni, G and Bellotti, R and Bemporad, C and Bernardini, P and Bilokon, H and Bisi, V and Bloise, C and Bower, C and Brigida, M and Bussino, S and Cafagna, F and Calicchio, M and Campana, D and Carboni, M and Cecchini, S and Cei, F and Chiarella, V and Choudhary, BC and Coutu, S and de Cataldo, G and Dekhissi, H and de
Marzo, C and de Mitri, I and Derkaoui, J and de Vincenzi, M and di
Credico, A and Erriquez, O and Favuzzi, C and Forti, C and Fusco, P and Giacomelli, G and Giannini, G and Giglietto, N and Giorgini, M and Grassi, M and Gray, L and Grillo, A and Guarino, F and Gustavino, C and Habig, A and Hanson, K and Heinz, R and Iarocci, E and Katsavounidis, E and Katsavounidis, I and Kearns, E and Kim, H and Kyriazopoulou, S and Lamanna, E and Lane, C and Levin, DS and Lipari, P and Longley, NP and Longo, MJ and Loparco, F and Maaroufi, F and Mancarella, G and Mandrioli, G and Manzoor, S and Margiotta, A and Marini, A and Martello,
D and Marzari-Chiesa, A and Mazziotta, MN and Michael, DG and Mikheyev,
S and Miller, L and Monacelli, P and Montaruli, T and Monteno, M and Mufson, S and Musser, J and Nicolo, D and Nolty, R and Okada, C and Orth,
C and Osteria, G and Ouchrif, M and Palamara, O and Patera, V and Patrizii,
L and Pazzi, R and Peck, CW and Perrone, L and Petrera, S and Pistilli, P and Popa, V and Raino, A and Reynoldson, J and Ronga, F and Satriano, C and Satta, L and Scapparone, E},
Title = {Neutrino astronomy with the macro detector},
Journal = {Astrophysical Journal},
Volume = {546},
Number = {2 PART 1},
Pages = {1038-1054},
Publisher = {IOP Publishing},
Year = {2001},
Month = {January},
ISSN = {0004-637X},
url = {http://arxiv.org/pdf/astro-ph/0002492},
Abstract = {High-energy gamma-ray astronomy is now a well-established
field, and several sources have been discovered in the
region from a few giga-electron volts up to several
tera-electron volts. If sources involving hadronic processes
exist, the production of photons would be accompanied by
neutrinos too. Other possible neutrino sources could be
related to the annihilation of weakly interacting, massive
particles (WIMPs) at the center of galaxies with black
holes. We present the results of a search for pointlike
sources using 1100 upward-going muons produced by neutrino
interactions in the rock below and inside the Monopole
Astrophysics and Cosmic Ray Observatory (MACRO) detector in
the underground Gran Sasso Laboratory. These data show no
evidence of a possible neutrino pointlike source or of
possible correlations between gamma-ray bursts and
neutrinos. They have been used to set flux upper limits for
candidate pointlike sources which are in the range
10-14-10-15 cm-2 s-1.},
Doi = {10.1086/318281},
Key = {Ambrosio:2000yx}
}
@article{Blaufuss:2000tp,
Author = {Blaufuss, E and Guillian, G and Fukuda, Y and Fukuda, S and Ishitsuka,
M and Itow, Y and Kajita, T and Kameda, J and Kaneyuki, K and Kobayashi, K and Kobayashi, Y and Koshio, Y and Miura, M and Moriyama, S and Nakahata, M and Nakayama, S and Obayashi, Y and Okada, A and Okumura, K and Sakurai, N and Shiozawa, M and Suzuki, Y and Takeuchi, B and Takeuchi, Y and Toshito,
T and Totsuka, Y and Yamada, S and Earl, M and Habig, A and Kearns, E and Messier, MD and Scholberg, K and Stone, JL and Sulak, LR and Walter, CW and Goldhaber, M and Barszczak, T and Casper, D and Gajewski, W and Kropp,
WR and Mine, S and Price, LR and Smy, M and Sobel, HW and Vagins, MR and Ganezer, KS and Keig, WE and Ellsworth, RW and Tasaka, S and Kibayashi,
A and Learned, JG and Matsuno, S and Takemori, D and Hayato, Y and Ishii,
T and Kobayashi, T and Nakamura, K and Oyama, Y and Sakai, A and Sakuda, M and Sasaki, O and Echigo, S and Kohama, M and Suzuki, AT and Inagaki, T and Nishikawa, K and Haines, TJ and Kim, BK and Sanford, R and Svoboda, R and Chen, ML and Goodman, JA and Sullivan, GW and Hill, J and Jung, CK and Martens, K and Malek, M and Mauger, C and McGrew, C and Sharkey, E and Viren, B and Yanagisawa, C and Kirisawa, M and Inaba, S and Mitsuda, C and Miyano, K and Okazawa, H and Saji, C and Takahashi, M and Takahata, M and Nagashima, Y and Nitta, K and Takita, M and Yoshida, M and Kim, SB and Etoh, M and Gando, Y and Hasegawa, T and Inoue, K and Ishihara, K and Maruyama, T and Shirai, J and Suzuki, A and Koshiba, M and Hatakeyama,
Y and Ichikawa, Y and Koike, M and Nishijima, K and Fujiyasu, H and Ishino,
H and Morii, M and Watanabe, Y and Golebiewska, U and Kielczewska, D and Boyd, SC and Stachyra, AL and Wilkes, RJ and Young,
KK},
Title = {N-16 as a calibration source for Super-Kamiokande},
Journal = {NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION
A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED
EQUIPMENT},
Volume = {458},
Number = {3},
Pages = {638-649},
Publisher = {ELSEVIER SCIENCE BV},
Year = {2001},
Month = {February},
ISSN = {0168-9002},
url = {http://gateway.webofknowledge.com/gateway/Gateway.cgi?GWVersion=2&SrcApp=PARTNER_APP&SrcAuth=LinksAMR&KeyUT=WOS:000167040900004&DestLinkType=FullRecord&DestApp=ALL_WOS&UsrCustomerID=47d3190e77e5a3a53558812f597b0b92},
Abstract = {http://arxiv.org/abs/hep-ex/0005014},
Key = {Blaufuss:2000tp}
}
@article{fds318500,
Author = {Bhatnagar, P and Glasheen, BM and Bains, SK and Long, SL and Minocha, R and Walter, C and Minocha, SC},
Title = {Transgenic manipulation of the metabolism of polyamines in
poplar cells.},
Journal = {Plant physiology},
Volume = {125},
Number = {4},
Pages = {2139-2153},
Year = {2001},
Month = {April},
url = {http://dx.doi.org/10.1104/pp.125.4.2139},
Abstract = {The metabolism of polyamines (putrescine, spermidine, and
spermine) has become the target of genetic manipulation
because of their significance in plant development and
possibly stress tolerance. We studied the polyamine
metabolism in non-transgenic (NT) and transgenic cells of
poplar (Populus nigra x maximowiczii) expressing a mouse Orn
decarboxylase (odc) cDNA. The transgenic cells showed
elevated levels of mouse ODC enzyme activity, severalfold
higher amounts of putrescine, a small increase in
spermidine, and a small reduction in spermine as compared
with NT cells. The conversion of labeled ornithine (Orn)
into putrescine was significantly higher in the transgenic
than the NT cells. Whereas exogenously supplied Orn caused
an increase in cellular putrescine in both cell lines,
arginine at high concentrations was inhibitory to putrescine
accumulation. The addition of urea and glutamine had no
effect on polyamines in either of the cell lines. Inhibition
of glutamine synthetase by methionine sulfoximine led to a
substantial reduction in putrescine and spermidine in both
cell lines. The results show that: (a) Transgenic expression
of a heterologous odc gene can be used to modulate
putrescine metabolism in plant cells, (b) accumulation of
putrescine in high amounts does not affect the native
arginine decarboxylase activity, (c) Orn biosynthesis occurs
primarily from glutamine/glutamate and not from catabolic
breakdown of arginine, (d) Orn biosynthesis may become a
limiting factor for putrescine production in the odc
transgenic cells, and (e) assimilation of nitrogen into
glutamine keeps pace with an increased demand for its use
for putrescine production.},
Doi = {10.1104/pp.125.4.2139},
Key = {fds318500}
}
@article{Fukuda:2001nk,
Author = {Fukuda, S and Fukuda, Y and Ishitsuka, M and Itow, Y and Kajita, T and Kameda, J and Kaneyuki, K and Kobayashi, K and Koshio, Y and Miura, M and Moriyama, S and Nakahata, M and Nakayama, S and Okada, A and Sakurai, N and Shiozawa, M and Suzuki, Y and Takeuchi, H and Takeuchi, Y and Toshito,
T and Totsuka, Y and Yamada, S and Desai, S and Earl, M and Kearns, E and Messier, MD and Scholberg, K and Stone, JL and Sulak, LR and Walter, CW and Goldhaber, M and Barszczak, T and Casper, D and Gajewski, W and Kropp,
WR and Mine, S and Liu, DW and Price, LR and Smy, MB and Sobel, HW and Vagins,
MR and Ganezer, KS and Keig, WE and Ellsworth, RW and Tasaka, S and Kibayashi, A and Learned, JG and Matsuno, S and Takemori, D and Hayato,
Y and Ishii, T and Kobayashi, T and Nakamura, K and Obayashi, Y and Oyama,
Y and Sakai, A and Sakuda, M and Kohama, M and Suzuki, AT and Inagaki, T and Nakaya, T and Nishikawa, K and Haines, TJ and Blaufuss, E and Dazeley,
S and Lee, KB and Svoboda, R and Goodman, JA and Guillian, G and Sullivan,
GW and Turcan, D and Habig, A and Hill, J and Jung, CK and Martens, K and Malek, M and Mauger, C and McGrew, C and Sharkey, E and Viren, B and Yanagisawa, C and Mitsuda, C and Miyano, K and Saji, C and Shibata, T and Kajiyama, Y and Nagashima, Y and Nitta, K and Takita, M and Yoshida, M and Kim, HI and Kim, SB and Yoo, J and Okazawa, H and Ishizuka, T and Etoh, M and Gando, Y and Hasegawa, T and Inoue, K and Ishihara, K and Maruyama, T and Shirai, J and Suzuki, A and Koshiba, M and Hatakeyama, Y and Ichikawa,
Y and Koike, M and Nishijima, K and Fujiyasu, H and Ishino, H and Morii, M and Watanabe, Y and Golebiewska, U and Kielczewska, D and Boyd, SC and Stachyra, AL and Wilkes, RJ and Young, KK and Super-Kamiokande
Collaboration},
Title = {Constraints on neutrino oscillations using 1258 days of
Super-Kamiokande solar neutrino data.},
Journal = {Physical review letters},
Volume = {86},
Number = {25},
Pages = {5656-5660},
Year = {2001},
Month = {June},
ISSN = {0031-9007},
url = {http://www.ncbi.nlm.nih.gov/pubmed/11415326},
Abstract = {We report the result of a search for neutrino oscillations
using precise measurements of the recoil electron energy
spectrum and zenith angle variations of the solar neutrino
flux from 1258 days of neutrino-electron scattering data in
Super-Kamiokande. The absence of significant zenith angle
variation and spectrum distortion places strong constraints
on neutrino mixing and mass difference in a flux-independent
way. Using the Super-Kamiokande flux measurement in
addition, two allowed regions at large mixing are
found.},
Doi = {10.1103/physrevlett.86.5656},
Key = {Fukuda:2001nk}
}
@article{Fukuda:2001nj,
Author = {Fukuda, S and Fukuda, Y and Ishitsuka, M and Itow, Y and Kajita, T and Kameda, J and Kaneyuki, K and Kobayashi, K and Koshio, Y and Miura, M and Moriyama, S and Nakahata, M and Nakayama, S and Okada, A and Sakurai, N and Shiozawa, M and Suzuki, Y and Takeuchi, H and Takeuchi, Y and Toshito,
T and Totsuka, Y and Yamada, S and Desai, S and Earl, M and Kearns, E and Messier, MD and Scholberg, K and Stone, JL and Sulak, LR and Walter, CW and Goldhaber, M and Barszczak, T and Casper, D and Gajewski, W and Kropp,
WR and Mine, S and Liu, DW and Price, LR and Smy, MB and Sobel, HW and Vagins,
MR and Ganezer, KS and Keig, WE and Ellsworth, RW and Tasaka, S and Kibayashi, A and Learned, JG and Matsuno, S and Takemori, D and Hayato,
Y and Ishii, T and Kobayashi, T and Nakamura, K and Obayashi, Y and Oyama,
Y and Sakai, A and Sakuda, M and Kohama, M and Suzuki, AT and Inagaki, T and Nakaya, T and Nishikawa, K and Haines, TJ and Blaufuss, E and Dazeley,
S and Lee, KB and Svoboda, R and Goodman, JA and Guillian, G and Sullivan,
GW and Turcan, D and Habig, A and Hill, J and Jung, CK and Martens, K and Malek, M and Mauger, C and McGrew, C and Sharkey, E and Viren, B and Yanagisawa, C and Mitsuda, C and Miyano, K and Saji, C and Shibata, T and Kajiyama, Y and Nagashima, Y and Nitta, K and Takita, M and Yoshida, M and Kim, HI and Kim, SB and Yoo, J and Okazawa, H and Ishizuka, T and Etoh, M and Gando, Y and Hasegawa, T and Inoue, K and Ishihara, K and Maruyama, T and Shirai, J and Suzuki, A and Koshiba, M and Hatakeyama, Y and Ichikawa,
Y and Koike, M and Nishijima, K and Fujiyasu, H and Ishino, H and Morii, M and Watanabe, Y and Golebiewska, U and Kielczewska, D and Boyd, SC and Stachyra, AL and Wilkes, RJ and Young, KK and Super-Kamiokande
Collaboration},
Title = {Solar 8B and hep neutrino measurements from 1258 days of
Super-Kamiokande data.},
Journal = {Physical review letters},
Volume = {86},
Number = {25},
Pages = {5651-5655},
Year = {2001},
Month = {June},
ISSN = {0031-9007},
url = {http://www.ncbi.nlm.nih.gov/pubmed/11415325},
Abstract = {Solar neutrino measurements from 1258 days of data from the
Super-Kamiokande detector are presented. The measurements
are based on recoil electrons in the energy range 5.0-20.0
MeV. The measured solar neutrino flux is
2.32+/-0.03(stat)+0.08-0.07(syst)x10(6) cm(-2) x s(-1),
which is 45.1+/-0.5(stat)+1.6-1.4(syst)% of that predicted
by the BP2000 SSM. The day vs night flux asymmetry
(Phi(n)-Phi(d))/Phi(average) is 0.033+/-0.022(stat)+0.013-0.012(syst).
The recoil electron energy spectrum is consistent with no
spectral distortion. For the hep neutrino flux, we set a 90%
C.L. upper limit of 40x10(3) cm(-2) x s(-1), which is 4.3
times the BP2000 SSM prediction.},
Doi = {10.1103/physrevlett.86.5651},
Key = {Fukuda:2001nj}
}
@article{Ahn:2001cq,
Author = {Ahn, SH and An, S and Aoki, S and Berns, HG and Bhang, HC and Boyd, S and Casper, D and Chikamatsu, T and Choi, JH and Echigo, S and Etoh, M and Fujii, K and Fukuda, S and Fukuda, Y and Gajewski, W and Golebiewska, U and Hara, T and Hasegawa, T and Hayato, Y and Hill, J and Hong, SJ and Ieiri,
M and Inada, T and Inagaki, T and Ishida, T and Ishii, H and Ishii, T and Ishino, H and Ishitsuka, M and Itow, Y and Iwashita, T and Jang, HI and Jang, JS and Jeon, EJ and Jeong, EM and Jung, CK and Kadowaki, T and Kajita, T and Kameda, J and Kaneyuki, K and Kato, I and Kato, Y and Kearns,
E and Kenmochi, S and Khang, BH and Kibayashi, A and Kielczewska, D and Kim, BJ and Kim, CO and Kim, HI and Kim, JH and Kim, JY and Kim, SB and Kishi,
S and Kitamura, M and Kobayashi, K and Kobayashi, T and Kobayashi, Y and Kohama, M and Koo, DG and Koshio, Y and Kropp, W and Kume, G and Kusano, E and Learned, JG and Lee, HK and Lee, JW and Lee, SB and Lim, IT and Lim, SH and Maesaka, H and Martens, K and Maruyama, T and Matsuno, S and Mauger, C and McGrew, C and Minakawa, M and Mine, S and Miura, M and Miyamoto, S and Miyano, K and Moriyama, S and Mukai, S and Nakahata, M and Nakamura, K and Nakamura, M and Nakano, I and Nakaya, T and Nakayama, S and Nakayoshi,
K and Nishijima, K and Nishikawa, K and Nishiyama, S and Noda, S and Noumi,
H and Obayashi, Y and Oh, JK and Okada, A and Onchi, M and Otaki,
T},
Title = {Detection of accelerator-produced neutrinos at a distance of
250 km},
Journal = {Physics Letters, Section B: Nuclear, Elementary Particle and
High-Energy Physics},
Volume = {511},
Number = {2-4},
Pages = {178-184},
Publisher = {Elsevier BV},
Year = {2001},
Month = {July},
ISSN = {0370-2693},
url = {http://gateway.webofknowledge.com/gateway/Gateway.cgi?GWVersion=2&SrcApp=PARTNER_APP&SrcAuth=LinksAMR&KeyUT=WOS:000169770800007&DestLinkType=FullRecord&DestApp=ALL_WOS&UsrCustomerID=47d3190e77e5a3a53558812f597b0b92},
Abstract = {The KEK to Kamioka long-baseline neutrino experiment (K2K)
has begun its investigation of neutrino oscillations
suggested by atmospheric neutrino observations. Twenty-eight
neutrino events have been detected in coincidence with the
expected arrival time of the beam in the 22.5 kt fiducial
volume of Super-Kamiokande, the far detector at 250 km
distance. The expectation is 37.8-3.8+3.5, derived using
measurements of neutrino interactions in a near detector and
extrapolation using a beam simulation validated by a
measurement of pion kinematics after production and
focusing. The background is of order 10-3 events. © 2001
Elsevier Science B.V.},
Doi = {10.1016/S0370-2693(01)00647-5},
Key = {Ahn:2001cq}
}
@article{Ambrosio:2001je,
Author = {Ambrosio, M and Antolini, R and Auriemma, G and Bakari, D and Baldini,
A and Barbarino, GC and Barish, BC and Battistoni, G and Becherini, Y and Bellotti, R and Bemporad, C and Bernardini, P and Bilokon, H and Bisi,
V and Bloise, C and Bower, C and Brigida, M and Bussino, S and Cafagna, F and Calicchio, M and Campana, D and Carboni, M and Caruso, R and Cecchini,
S and Cei, F and Chiarella, V and Choudhary, BC and Coutu, S and de
Cataldo, G and Dekhissi, H and de Marzo, C and de Mitri, I and Derkaoui,
J and de Vincenzi, M and di Credico, A and Erriquez, O and Favuzzi, C and Forti, C and Fusco, P and Giacomelli, G and Giannini, G and Giglietto,
N and Giorgini, M and Grassi, M and Gray, L and Grillo, A and Guarino, F and Gustavino, C and Habig, A and Hanson, K and Heinz, R and Iarocci, E and Katsavounidis, E and Katsavounidis, I and Kearns, E and Kim, H and Kyriazopoulou, S and Lamanna, E and Lane, C and Levin, DS and Lipari, P and Longley, NP and Longo, MJ and Loparco, F and Maaroufi, F and Mancarella,
G and Mandrioli, G and Margiotta, A and Marini, A and Martello, D and Marzari-Chiesa, A and Mazziotta, MN and Michael, DG and Mikheyev, S and Miller, L and Monacelli, P and Montaruli, T and Monteno, M and Mufson,
S and Musser, J and Nicolo, D and Nolty, R and Orth, C and Osteria, G and Palamara, O and Patera, V and Patrizii, L and Pazzi, R and Peck, CW and Perrone, L and Petrera, S and Pistilli, P and Popa, V and Raino, A and Reynoldson, J and Ronga, F and Rrhioua, A and Satriano, C and Scapparone, E and Scholberg, K},
Title = {Matter effects in upward-going muons and sterile neutrino
oscillations},
Journal = {Physics Letters, Section B: Nuclear, Elementary Particle and
High-Energy Physics},
Volume = {517},
Number = {1-2},
Pages = {59-66},
Publisher = {Elsevier BV},
Year = {2001},
Month = {September},
ISSN = {0370-2693},
url = {http://arxiv.org/pdf/hep-ex/0106049},
Abstract = {The angular distribution of upward-going muons produced by
atmospheric neutrinos in the rock below the MACRO detector
shows anomalies in good agreement with two flavor vμ →
vτ oscillations with maximum mixing and Δm2 around 0.0024
eV2. Exploiting the dependence of magnitude of the matter
effect on oscillation channel, and using a set of 809
upward-going muons observed in MACRO, we show that the two
flavor vμ → vs oscillation is disfavored with 99% C.L.
with respect to vμ → vτ. © 2001 Elsevier Science B.V.
All rights reserved.},
Doi = {10.1016/S0370-2693(01)00992-3},
Key = {Ambrosio:2001je}
}
@article{fds248833,
Author = {Walter, CW},
Title = {Nuclear Effects on QE Reconstruction in Low-Energy Neutrino
Long-Baseline Experiments.},
Journal = {Nuclear Physics B, Proceedings Supplements},
Year = {2002},
Key = {fds248833}
}
@article{Walter:2002sa,
Author = {Walter, CW},
Title = {Quasi-elastic events and nuclear effects with the K2K Sci-Fi
detector},
Journal = {Nuclear Physics B - Proceedings Supplements},
Volume = {111},
Number = {1-3},
Pages = {140-145},
Publisher = {Elsevier BV},
Year = {2002},
Month = {January},
url = {http://dx.doi.org/10.1016/s0920-5632(02)01784-x},
Abstract = {The near detector complex of the K2K long-baseline neutrino
experiment contains a scintillating fiber tracking detector.
It is capable of detecting not only the muon but also the
outgoing proton in neutrino-nucleon scattering. This allows
for the enhancement of quasi-elastic interactions in the
data sample. However, a proper modeling of the nuclear
re-interactions of the proton is necessary to achieve
reliable results.},
Doi = {10.1016/s0920-5632(02)01784-x},
Key = {Walter:2002sa}
}
@article{fds361717,
Author = {Giacomelli, G and Margiotta, A},
Title = {Status Report of the MACRO Experiment for the year
2001},
Year = {2002},
Month = {June},
Abstract = {In this 2001 status report of the MACRO experiment, results
are presented on atmospheric neutrinos and neutrino
oscillations, high energy neutrino astronomy, searches for
WIMPs, search for low energy stellar gravitational collapse
neutrinos, stringent upper limits on GUT magnetic monopoles,
nuclearites and lightly ionizing particles, high energy
downgoing muons, primary cosmic ray composition and
shadowing of primary cosmic rays by the Moon and the
Sun.},
Key = {fds361717}
}
@article{Ambrosio:2002mb,
Author = {Ambrosio, M and Antolini, R and Assiro, R and Auriemma, G and Bakari, D and Baldini, A and Barbarino, GC and Barbarito, E and Barish, BC and Battistoni, G and Becherini, Y and Bellotti, R and Bemporad, C and Bernardini, P and Bilokon, H and Bisi, V and Bloise, C and Bottazzi, E and Bower, C and Brigida, M and Bussino, S and Cafagna, F and Calicchio, M and Campana, D and Candela, A and Carboni, M and Cecchini, S and Cei, F and Ceres, A and Chiarella, V and Choudhary, BC and Coutu, S and Cozzi, M and Creti, P and De Cataldo and G and Degli Esposti and L and Dekhissi, H and De
Marzo, C and De Mitri and I and Derkaoui, J and De Vincenzi and M and Di
Credico, A and Di Ferdinando and D and Diotallevi, R and Erriquez, O and Favuzzi, C and Forti, C and Fusco, P and Gebhard, M and Giacomelli, G and Giacomelli, R and Giannini, G and Giglietto, N and Giorgini, M and Giuliani, R and Goretti, M and Grassi, M and Grau, H and Gray, L and Grillo, A and Guarino, F and Gustavino, C and Habig, A and Hanson, J and Hanson, K and Hawthorne, A and Heinz, R and Hong, JT and Iarocci, E and Katsavounidis, E and Katsavounidis, I and Kearns, E and Kim, H and Kyriazopoulou, S and Lamanna, E and Lane, C and Leone, A and Levin, DS and Lipari, P and Liu, G and Liu, R and Longley, NP and Longo, MJ and Loparco,
F and Maaroufi, F and Mancarella, G and Mandrioli, G and Manzoor, S and Marrelli, V and Margiotta, A and Marini, A and Martello, D and Marzari-Chiesa, A and Mazziotta, MN and Michael, DG and Mikheyev, S and Miller, L and Monacelli, P and Mongelli, M and Montaruli,
T},
Title = {The MACRO detector at Gran Sasso},
Journal = {Nuclear Instruments and Methods in Physics Research, Section
A: Accelerators, Spectrometers, Detectors and Associated
Equipment},
Volume = {486},
Number = {3},
Pages = {663-707},
Publisher = {Elsevier BV},
Year = {2002},
Month = {July},
ISSN = {0168-9002},
url = {http://gateway.webofknowledge.com/gateway/Gateway.cgi?GWVersion=2&SrcApp=PARTNER_APP&SrcAuth=LinksAMR&KeyUT=WOS:000176945400010&DestLinkType=FullRecord&DestApp=ALL_WOS&UsrCustomerID=47d3190e77e5a3a53558812f597b0b92},
Abstract = {MACRO was an experiment that ran in the Laboratori Nazionali
del Gran Sasso from 1988 to 2000. Its principal goal was to
observe magnetic monopoles or set significantly lower
experimental flux limits than had been previously available
in the velocity range from about β = 10-4 to unity. In
addition it made a variety of other observations. Examples
are: setting flux limits on other so far unobserved
particles such as nuclearites and lightly ionizing
particles, searching for WIMP annihilations in the Earth and
the Sun and for neutrino bursts from stellar collapses in or
near our Galaxy, and making measurements relevant to high
energy muon and neutrino astronomy and of the flux of
up-going muons as a function of nadir angle showing evidence
for neutrino oscillations. The apparatus consisted of three
principal types of detectors: liquid scintillator counters,
limited streamer tubes, and nuclear track etch detectors. In
addition, over part of its area it contained a transition
radiation detector. The general design philosophy emphasized
redundancy and complementarity. This paper describes the
technical aspects of the complete MACRO detector, its
operational performance, and the techniques used to
calibrate it and verify its proper operation. It supplements
a previously published paper which described the first
portion of the detector that was built and
operated.},
Doi = {10.1016/S0168-9002(01)02169-6},
Key = {Ambrosio:2002mb}
}
@article{fds326729,
Author = {De Mitri and I},
Title = {Search for massive rare particles with MACRO},
Journal = {Nuclear Physics B - Proceedings Supplements},
Volume = {110},
Pages = {186-188},
Publisher = {Elsevier BV},
Year = {2002},
Month = {July},
url = {http://dx.doi.org/10.1016/s0920-5632(02)01479-2},
Doi = {10.1016/s0920-5632(02)01479-2},
Key = {fds326729}
}
@article{Ambrosio:2001ai,
Author = {Ambrosio, M and Antolini, R and Auriemma, G and Bakari, D and Baldini,
A and Barbarino, GC and Barish, BC and Battistoni, G and Becherini, Y and Bellotti, R and Bemporad, C and Bernardini, P and Bilokon, H and Bloise,
C and Bower, C and Brigida, M and Bussino, S and Cafagna, F and Calicchio,
M and Campana, D and Carboni, M and Caruso, R and Cecchini, S and Cei, F and Chiarella, V and Choudhary, BC and Coutu, S and de Cataldo, G and Dekhissi, H and de Marzo, C and de Mitri, I and Derkaoui, J and de
Vincenzi, M and di Credico, A and Erriquez, O and Favuzzi, C and Forti,
C and Fusco, P and Giacomelli, G and Giannini, G and Giglietto, N and Giorgini, M and Grassi, M and Grillo, A and Guarino, F and Gustavino, C and Habig, A and Heinz, R and Iarocci, E and Katsavounidis, E and Katsavounidis, I and Kearns, E and Kim, H and Kyriazopoulou, S and Lamanna, E and Lane, C and Levin, DS and Lipari, P and Longley, NP and Longo, MJ and Loparco, F and Maaroufi, F and Mancarella, G and Mandrioli, G and Manzoor, S and Margiotta, A and Marini, A and Martello,
D and Marzari-Chiesa, A and Mazziotta, MN and Michael, DG and Monacelli,
P and Montaruli, T and Monteno, M and Mufson, S and Musser, J and Nicolò,
D and Nolty, R and Orth, C and Osteria, G and Palamara, O and Patera, V and Patrizii, L and Pazzi, R and Peck, CW and Perrone, L and Petrera, S and Popa, V and Reynoldson, J and Ronga, F and Rrhioua, A and Satriano, C and Scapparone, E and Scholberg, K and Sciubba, A and Serra, P and Sioli, M and Sirri, G and Sitta, M and Spinelli, P},
Title = {A combined analysis technique for the search for fast
magnetic monopoles with the MACRO detector},
Journal = {Astroparticle Physics},
Volume = {18},
Number = {1},
Pages = {27-41},
Publisher = {Elsevier BV},
Year = {2002},
Month = {July},
ISSN = {0927-6505},
url = {http://arxiv.org/pdf/hep-ex/0110083},
Abstract = {We describe a search method for fast moving (β = v/c > 5 ×
10-3) magnetic monopoles using simultaneously the
scintillator, streamer tube and track-etch subdetectors of
the MACRO apparatus. The first two subdetectors are used
primarily for the identification of candidates while the
track-etch one is used as the final tool for their rejection
or confirmation. Using this technique, a first sample of
more than two years of data has been analyzed without any
evidence of a magnetic monopole. We set a 90% CL upper limit
to the local monopole flux of 1.5 × 10-15 cm-2 s-1 sr-1 in
the velocity range 5 × 10-3 ≤ β ≤ 0.99 and for nucleon
decay catalysis cross-section smaller than ∼1 mb © 2002
Elsevier Science B.V. All rights reserved.},
Doi = {10.1016/S0927-6505(01)00183-9},
Key = {Ambrosio:2001ai}
}
@article{Fukuda:2002pe,
Author = {Fukuda, S and Fukuda, Y and Ishitsuka, M and Itow, Y and Kajita, T and Kameda, J and Kaneyuki, K and Kobayashi, K and Koshio, Y and Miura, M and Moriyama, S and Nakahata, M and Nakayama, S and Namba, T and Okada, A and Sakurai, N and Shiozawa, M and Suzuki, Y and Takeuchi, H and Takeuchi,
Y and Totsuka, Y and Yamada, S and Desai, S and Earl, M and Kearns, E and Messier, MD and Stone, JL and Sulak, LR and Walter, CW and Goldhaber, M and Barszczak, T and Casper, D and Gajewski, W and Kropp, WR and Mine, S and Liu, DW and Smy, MB and Sobel, HW and Vagins, MR and Gago, A and Ganezer,
KS and Keig, WE and Ellsworth, RW and Tasaka, S and Kibayashi, A and Learned, JG and Matsuno, S and Takemori, D and Hayato, Y and Ishii, T and Kobayashi, T and Maruyama, T and Nakamura, K and Obayashi, Y and Oyama,
Y and Sakuda, M and Yoshida, M and Kohama, M and Iwashita, T and Suzuki,
AT and Ichikawa, A and Inagaki, T and Kato, I and Nakaya, T and Nishikawa,
K and Haines, TJ and Dazeley, S and Hatakeyama, S and Svoboda, R and Blaufuss, E and Chen, ML and Goodman, JA and Guillian, G and Sullivan,
GW and Turčan, D and Scholberg, K and Habig, A and Ackermann, M and Hill,
J and Jung, CK and Malek, M and Martens, K and Mauger, C and McGrew, C and Sharkey, E and Viren, B and Yanagisawa, C and Toshito, T and Mitsuda, C and Miyano, K and Saji, C and Shibata, T and Kajiyama, Y and Nagashima, Y and Nitta, K and Takitat, M and Kim, HI and Kim, SB and Yoo, J and Okazawa,
H},
Title = {Determination of solar neutrino oscillation parameters using
1496 days of Super-Kamiokande-I data},
Journal = {Physics Letters, Section B: Nuclear, Elementary Particle and
High-Energy Physics},
Volume = {539},
Number = {3-4},
Pages = {179-187},
Publisher = {Elsevier BV},
Year = {2002},
Month = {July},
ISSN = {0370-2693},
url = {http://arxiv.org/pdf/hep-ex/0205075},
Abstract = {A number of different fits to solar neutrino mixing and mass
square difference were performed using 1496 days of
Super-Kamiokande-I's solar neutrino data. These data select
two allowed areas at large neutrino mixing when combined
with either the solar 8B flux prediction of the standard
solar model or the SNO interaction rate measurements. A
global fit combining SK data with the solar neutrino
interaction rates measured by Homestake, SNO, Gallex/GNO and
SAGE prefers a single allowed area, the Large Mixing Angle
solution, at the 98.9% confidence level. The mass square
difference Δm2 between the two mass eigenstates ranges from
about 3 to 19 × 10-5 eV2, while the mixing angle θ is in
the range of tan2θ ≈ 0.25-0.65. © 2002 Elsevier Science
B.V. All rights reserved.},
Doi = {10.1016/S0370-2693(02)02090-7},
Key = {Fukuda:2002pe}
}
@article{fds361716,
Author = {al, DAE},
Title = {Letter of Intent to build an Off-axis Detector to study numu
to nue oscillations with the NuMI Neutrino
Beam},
Year = {2002},
Month = {October},
Abstract = {The NuMI neutrino beam line and the MINOS experiment
represent a major investment of US High Energy Physics in
the area of neutrino physics. The forthcoming results could
decisively establish neutrino oscillations as the underlying
physics mechanism for the atmospheric $\numu$ deficit and
provide a precise measurement of the corresponding
oscillation parameters, $\dmsq23$ and $\sinsq2t23$.neutrino
sector may well be within our reach. The full potential of
the NuMI neutrino beam can be exploited by complementing the
MINOS detector, under construction, with a new detector(s)
placed at some off-axis position and collecting data in
parallel with MINOS. The first phase of the proposed program
includes a new detector, optimized for $\nue$ detection,
with a fiducial mass of the order of 20 kton and exposed to
neutrino and antineutrino beams. In a five year run its
sensitivity to the $\numutonue$ oscillations will be at
least a factor of ten beyond the current limit. The future
direction of the program will depend on the results of this
first phase, but it is very likely that it will be a
combination of a significant increase of the neutrino beam
intensity via an upgraded proton source and an increase of
the detector mass by a factor of five or so. Depending on
the circumstances, the goals of Phase II may be a further
increase of the sensitivity of a search for $\numutonue$
oscillations, or, perhaps, a measurement of the CP violating
phase $\delta$ in the lepton sector.},
Key = {fds361716}
}
@article{Fukuda:2002nf,
Author = {Fukuda, S and Fukuda, Y and Ishitsuka, M and Itow, Y and Kajita, T and Kameda, J and Kaneyuki, K and Kobayashi, K and Koshio, Y and Miura, M and Moriyama, S and Nakahata, M and Nakayama, S and Okada, A and Sakurai, N and Shiozawa, M and Suzuki, Y and Takeuchi, H and Takeuchi, Y and Toshito,
T and Totsuka, Y and Yamada, S and Desai, S and Kearns, E and Messier, MD and Stone, JL and Sulak, LR and Walter, CW and Wang, W and Goldhaber, M and Casper, D and Gajewski, W and Kropp, WR and Mine, S and Liu, DW and Smy,
MB and Sobel, HW and Vagins, MR and Ganezer, KS and Keig, WE and Ellsworth,
RW and Tasaka, S and Kibayashi, A and Learned, JG and Matsuno, S and Hayato, Y and Ichikawa, A and Ishii, T and Kobayashi, T and Maruyama, T and Nakamura, K and Obayashi, Y and Oyama, Y and Sakuda, M and Yoshida, M and Iwashita, T and Kohama, M and Suzuki, AT and Inagaki, T and Kato, I and Nakaya, T and Nishikawa, K and Haines, TJ and Dazeley, S and Svoboda, R and Blaufuss, E and Goodman, JA and Guillian, G and Sullivan, GW and Turcan,
D and Scholberg, K and Habig, A and Hill, J and Jung, CK and Martens, K and Malek, M and Mauger, C and McGrew, C and Sharkey, E and Viren, B and Yanagisawa, C and Mitsuda, C and Miyano, K and Saji, C and Shibata, T and Kajiyama, Y and Nagashima, Y and Nitta, K and Takita, M and Kim, HI and Kim, SB and Yoo, J and Okazawa, H and Ishizuka, T and Etoh, M and Gando, Y and Hasegawa, T and Inoue, K and Ishihara, K and Nishiyama,
I},
Title = {Search for neutrinos from gamma-ray bursts using
Super-Kamiokande},
Journal = {Astrophysical Journal},
Volume = {578},
Number = {1 I},
Pages = {317-324},
Publisher = {IOP Publishing},
Year = {2002},
Month = {October},
ISSN = {0004-637X},
url = {http://arxiv.org/pdf/astro-ph/0205304},
Abstract = {Using the Super-Kamiokande neutrino observatory, a search
was conducted for neutrinos produced in coincidence with
gamma-ray bursts observed by the Burst and Transient Source
Experiment detector. Super-Kamiokande data in the neutrino
energy range of 7 MeV ∼ 100 TeV were analyzed. For
gamma-ray bursts that occurred between 1996 April and 2000
May, no statistically significant signal in excess of the
background levels was detected. Implied upper limits on
associated gamma-ray burst neutrino production are
presented.},
Doi = {10.1086/342405},
Key = {Fukuda:2002nf}
}
@article{Ambrosio:2002du,
Author = {Ambrosio, M and Antolini, R and Auriemma, G and Bakari, D and Baldini,
A and Barbarino, GC and Barish, BC and Battistoni, G and Becherini, Y and Bellotti, R and Bemporad, C and Bernardini, P and Bilokon, H and Bloise,
C and Bower, C and Brigida, M and Bussino, S and Cafagna, F and Calicchio,
M and Campana, D and Candela, A and Carboni, M and Caruso, R and Cassese,
F and Cecchini, S and Cei, F and Chiarella, V and Choudhary, BC and Coutu,
S and Cozzi, M and De Cataldo and G and De Deo and M and Dekhissi, H and De
Marzo, C and De Mitri and I and Derkaoui, J and De Vincenzi and M and Di
Credico, A and Dincecco, M and Erriquez, O and Favuzzi, C and Forti, C and Fusco, P and Giacomelli, G and Giannini, G and Giglietto, N and Giorgini, M and Grassi, M and Gray, L and Grillo, A and Guarino, F and Gustavino, C and Habig, A and Hanson, K and Heinz, R and Iarocci, E and Katsavounidis, E and Katsavounidis, I and Kearns, E and Kim, H and Kyriazopoulou, S and Lamanna, E and Lane, C and Levin, DS and Lindozzi,
M and Lipari, P and Longley, NP and Longo, MJ and Loparco, F and Maaroufi,
F and Mancarella, G and Mandrioli, G and Margiotta, A and Marini, A and Martello, D and Marzari-Chiesa, A and Mazziotta, MN and Michael, DG and Monacelli, P and Montaruli, T and Monteno, M and Mufson, S and Musser,
J and Nicolo, D and Nolty, R and Orth, C and Osteria, G and Palamara, O and Patera, V and Patrizii, L and Pazzi, R and Peck, CW and Perronj, L and Petrera, S and Pistilli, P and Popa, V and Raino, A and Reynoldson, J and Ronga, F and Rrhioua, A},
Title = {Muon energy estimate through multiple scattering with the
MACRO detector},
Journal = {Nuclear Instruments and Methods in Physics Research, Section
A: Accelerators, Spectrometers, Detectors and Associated
Equipment},
Volume = {492},
Number = {3},
Pages = {376-386},
Publisher = {Elsevier BV},
Year = {2002},
Month = {October},
ISSN = {0168-9002},
url = {http://arxiv.org/pdf/physics/0203018},
Abstract = {Muon energy measurement represents an important issue for
any experiment addressing neutrino-induced up-going muon
studies. Since the neutrino oscillation probability depends
on the neutrino energy, a measurement of the muon energy
adds an important piece of information concerning the
neutrino system. We show in this paper how the MACRO limited
streamer tube system can be operated in drift mode by using
the TDCs included in the QTPs, an electronics designed for
magnetic monopole search. An improvement of the space
resolution is obtained, through an analysis of the multiple
scattering of muon tracks as they pass through our detector.
This information can be used further to obtain an estimate
of the energy of muons crossing the detector. Here we
present the results of two dedicated tests, performed at
CERN PS-T9 and SPS-X7 beam lines, to provide a full check of
the electronics and to exploit the feasibility of such a
multiple scattering analysis. We show that by using a neural
network approach, we are able to reconstruct the muon energy
for Eμ<40 GeV. The test beam data provide an absolute
energy calibration, which allows us to apply this method to
MACRO data. © 2002 Elsevier Science B.V. All rights
reserved.},
Doi = {10.1016/S0168-9002(02)01413-4},
Key = {Ambrosio:2002du}
}
@article{fds318499,
Author = {Ambrosio, M and Antolini, R and Auriemma, G and Bakari, D and Baldini,
A and Barbarino, GC and Barish, BC and Battistoni, G and Becherini, Y and Bellotti, R and Bemporad, C and Bernardini, P and Bilokon, H and Bloise,
C and Bower, C and Brigida, M and Bussino, S and Cafagna, F and Calicchio,
M and Campana, D and Carboni, M and Caruso, R and Cecchini, S and Cei, F and Chiarella, V and Chiarusi, T and Choudhary, BC and Coutu, S and Cozzi,
M and de Cataldo, G and Dekhissi, H and de Marzo, C and de Mitri, I and Derkaoui, J and de Vincenzi, M and Di Credico and A and Erriquez, O and Favuzzi, C and Forti, C and Fusco, P and Giacomelli, G and Giannini, G and Giglietto, N and Giorgini, M and Grassi, M and Grillo, A and Guarino, F and Gustavino, C and Habig, A and Hanson, K and Heinz, R and Iarocci, E and Katsavounidis, E and Katsavounidis, I and Kearns, E and Kim, H and Kyriazopoulou, S and Kumar, A and Lamanna, E and Lane, C and Levin, DS and Lipari, P and Longley, NP and Longo, MJ and Loparco, F and Maaroufi, F and Mancarella, G and Mandrioli, G and Manzoor, S and Margiotta, A and Marini, A and Martello, D and Marzari-Chiesa, A and Matteuzzi, D and Mazziotta, MN and Michael, DG and Monacelli, P and Montaruli, T and Monteno, M and Mufson, S and Musser, J and Nicolò, D and Nolty, R and Orth, C and Osteria, G and Palamara, O and Patera, V and Patrizii, L and Pazzi, R and Peck, CW and Perrone, L and Petrera, S and Pistilli, P and Popa, V and Rainò, A and Reynoldson, J and Ronga, F and Rrhioua, A and Satriano, C and Scapparone, E},
Title = {Final results of magnetic monopole searches with the MACRO
experiment: The MACRO collaboration},
Journal = {European Physical Journal C},
Volume = {25},
Number = {4},
Pages = {511-522},
Year = {2002},
Month = {November},
url = {http://dx.doi.org/10.1140/epjc/s2002-01046-9},
Abstract = {We present the final results obtained by the MACRO
experiment in the search for GUT magnetic monopoles in the
penetrating cosmic radiation, for the range 4 × 10-5 < β <
1. Several searches with all the MACRO sub-detectors (i.e.
scintillation counters, limited streamer tubes and nuclear
track detectors) were performed, both in stand alone and
combined ways. No candidates were detected and a 90%
Confidence Level (C.L.) upper limit to the local magnetic
monopole flux was set at the level of 1.4 × 10-16 cm-2 s-1
sr-1. This result is the first experimental limit obtained
in direct searches which is well below the Parker bound in
the whole β range in which GUT magnetic monopoles are
expected.},
Doi = {10.1140/epjc/s2002-01046-9},
Key = {fds318499}
}
@article{Ambrosio:2002qu,
Author = {Ambrosio, M and Antolini, R and Auriemma, G and Bakari, D and Baldini,
A and Barbarino, GC and Barish, BC and Battistoni, G and Becherini, Y and Bellotti, R and Bemporad, C and Bernardini, P and Bilokon, H and Bloise,
C and Bower, C and Brigida, M and Bussino, S and Cafagna, F and Calicchio,
M and Campana, D and Carboni, M and Caruso, R and Cecchini, S and Cei, F and Chiarella, V and Choudhary, BC and Coutu, S and Cozzi, M and de Cataldo,
G and Dekhissi, H and de Marzo, C and de Mitri, I and Derkaoui, J and de
Vincenzi, M and Di Credico and A and Erriquez, O and Favuzzi, C and Forti,
C and Fusco, P and Giacomelli, G and Giannini, G and Giglietto, N and Giorgini, M and Grassi, M and Grillo, A and Guarino, F and Gustavino, C and Habig, A and Hanson, K and Heinz, R and Iarocci, E and Katsavounidis, E and Katsavounidis, I and Kearns, E and Kim, H and Kyriazopoulou, S and Lamanna, E and Lane, C and Levin, DS and Lipari, P and Longley, NP and Longo, MJ and Loparco, F and Maaroufi, F and Mancarella, G and Mandrioli, G and Manzoor, S and Margiotta, A and Marini, A and Martello,
D and Marzari-Chiesa, A and Mazziotta, MN and Michael, DG and Monacelli,
P and Montaruli, T and Monteno, M and Mufson, S and Musser, J and Nicolò,
D and Nolty, R and Orth, C and Osteria, G and Palamara, O and Patera, V and Patrizii, L and Pazzi, R and Peck, CW and Perrone, L and Petrera, S and Pistilli, P and Popa, V and Rainò, A and Reynoldson, J and Ronga, F and Rrhioua, A and Satriano, C and Scapparone, E and Scholberg, K and Sciubba, A and Serra, P},
Title = {Search for nucleon decays induced by GUT magnetic monopoles
with the MACRO experiment},
Journal = {European Physical Journal C},
Volume = {26},
Number = {2},
Pages = {163-172},
Publisher = {Springer Nature},
Year = {2002},
Month = {December},
ISSN = {1434-6044},
url = {http://arxiv.org/pdf/hep-ex/0207024},
Abstract = {The interaction of a Grand Unification Magnetic Monopole
with a nucleon can lead to a barion-number violating process
in which the nucleon decays into a lepton and one or more
mesons (catalysis of nucleon decay). In this paper we report
an experimental study of the effects of a catalysis process
in the MACRO detector. Using a dedicated analysis we obtain
new magnetic monopole (MM) flux upper limits at the level of
∼ 3 · 10-16 cm-2 s-1 sr-1 for 1.1 · 10-4 ≤ |β| ≤ 5
· 10-3, based on the search for catalysis events in the
MACRO data. We also analyze the dependence of the MM flux
limit on the catalysis cross section.},
Doi = {10.1140/epjc/s2002-01045-x},
Key = {Ambrosio:2002qu}
}
@article{Ahn:2002up,
Author = {Ahn, MH and Aoki, S and Bhang, H and Boyd, S and Casper, D and Choi, JH and Fukuda, S and Fukuda, Y and Gajewski, W and Hara, T and Hasegawa, M and Hasegawa, T and Hayato, Y and Hill, J and Ichikawa, AK and Ikeda, A and Inagaki, T and Ishida, T and Ishii, T and Ishitsuka, M and Itow, Y and Iwashita, T and Jang, HI and Jang, JS and Jeon, EJ and Jung, CK and Kajita,
T and Kameda, J and Kaneyuki, K and Kato, I and Kearns, E and Kibayashi, A and Kielczewska, D and Kobayashi, K and Kim, BJ and Kim, CO and Kim, JY and Kim, SB and Kobayashi, T and Kohama, M and Koshio, Y and Kropp, WR and Learned, JG and Lim, SH and Lim, IT and Maesaka, H and Martens, K and Maruyama, T and Matsuno, S and Mauger, C and Mcgrew, C and Mine, S and Miura, M and Miyano, K and Moriyama, S and Nakahata, M and Nakamura, K and Nakano, I and Nakata, F and Nakaya, T and Nakayama, S and Namba, T and Nishikawa, K and Nishiyama, S and Noda, S and Obayashi, A and Okada, A and Ooyabu, T and Oyama, Y and Pac, MY and Park, H and Sakuda, M and Sakurai,
N and Sasao, N and Scholberg, K and Sharkey, E and Shiozawa, M and So, H and Sobel, HW and Stachyra, A and Stone, JL and Suga, Y and Sulak, LR and Suzuki, A and Suzuki, Y and Takeuchi, Y and Tamura, N and Toshito, T and Totsuka, Y and Vagins, MR and Walter, CW and Wilkes, RJ and Yamada, S and Yamamoto, S and Yanagisawa, C and Yokoyama, H and Yoo, J and Yoshida, M and Zalipska, J},
Title = {Indications of neutrino oscillation in a 250 km
long-baseline experiment},
Journal = {Physical Review Letters},
Volume = {90},
Number = {4},
Pages = {418011-418015},
Year = {2003},
ISSN = {0031-9007},
url = {http://www.ncbi.nlm.nih.gov/pubmed/12570410},
Abstract = {A study was performed on Kamioka long-baseline neutrino
oscillation experiment (K2K). The indications of neutrino
oscillation such as a reduction of flux together with a
distortion of the energy spectrum were observed in the
experiment. In Super Kamiokande (SK), 250 km from the
neutrino production point, fifty-six beam neutrino events
were observed. It was found that the probability that the
measurements at SK is explained by statistical fluctuation
without neutrino oscillation is less than
1%.},
Doi = {10.1103/physrevlett.90.041801},
Key = {Ahn:2002up}
}
@article{fds248716,
Author = {Walter, CW},
Title = {Recent results from the K2K experiment},
Journal = {Nuclear Physics B - Proceedings Supplements},
Volume = {123},
Pages = {260-266},
Booktitle = {Fundamental Interactions, Proceedings of the 17th Lake
Louise Winter Institute},
Publisher = {Elsevier BV},
Year = {2003},
Month = {January},
ISSN = {0920-5632},
url = {http://dx.doi.org/10.1016/S0920-5632(03)02186-8},
Abstract = {The K2K experiment has collected approximately half of its
allocated protons on target between June of 1999 and July of
2001. These proceedings give a short introduction to the
experiment and summarize some of the recent
results.},
Doi = {10.1016/S0920-5632(03)02186-8},
Key = {fds248716}
}
@article{fds248736,
Author = {Togo, V and Ambrosio, M and Antolini, R and Auriemma, G and Bakari, D and Baldini, A and Barbarino, GC and Barish, BC and Battistoni, G and Becherini, Y and Bellotti, R and Bemporad, C and Bernardini, P and Bilokon, H and Bloise, C and Bower, C and Brigida, M and Bussino, S and Cafagna, F and Calicchio, M and Campana, D and Carboni, M and Caruso, R and Cecchini, S and Cei, F and Chiarella, V and Chiarusi, T and Choudhary,
BC and Coutu, S and Cozzi, M and de Cataldo, G and Dekhissi, H and de
Marzo, C and de Mitri, I and Derkaoui, J and de Vincenzi, M and di
Credico, A and Erriquez, O and Favuzzi, C and Forti, C and Fusco, P and Giacomelli, G and Giannini, G and Giglietto, N and Giorgini, M and Grassi, M and Grillo, A and Guarino, F and Gustavino, C and Habig, A and Hanson, K and Heinz, R and Iarocci, E and Katsavounidis, E and Katsavounidis, I and Kearns, E and Kim, H and Kyriazopoulou, S and Kumar, A and Lamanna, E and Lane, C and Levin, DS and Lipari, P and Longley, NP and Longo, MJ and Loparco, F and Maaroufi, F and Mancarella,
G and Mandrioli, G and Manzoor, S and Margiotta, A and Marini, A and Martello, D and Marzari-Chiesa, A and Matteuzzi, D and Mazziotta, MN and Michael, DG and Monacelli, P and Montaruli, T and Monteno, M and Mufson,
S and Musser, J and Nicolò, D and Nolty, R and Orth, C and Osteria, G and Palamara, O and Patera, V and Patrizii, L and Pazzi, R and Peck, CW and Perrone, L and Petrera, S and Pistilli, P and Popa, V and Rainò, A and Reynoldson, J and Ronga, F and Rrhioua, A and Satriano,
C},
Title = {Calibrations of CR39 and Makrofol nuclear track detectors
and search for exotic particles},
Journal = {Nuclear Physics B - Proceedings Supplements},
Volume = {125},
Pages = {217-221},
Publisher = {Elsevier BV},
Year = {2003},
Month = {January},
ISSN = {0920-5632},
url = {http://dx.doi.org/10.1016/S0920-5632(03)90994-7},
Abstract = {We present the final results of the search for exotic
massive particles in the cosmic radiation performed with the
MACRO underground experiment. Magnetic monopoles and
nuclearites flux upper limits obtained with the CR39 nuclear
track subdetector, the scintillation and streamer tube
subdetectors are given. Searches at high altitude with the
SLIM experiment are in progress.},
Doi = {10.1016/S0920-5632(03)90994-7},
Key = {fds248736}
}
@article{Ambrosio:2002db,
Author = {Ambrosio, M and Antolini, R and Baldini, A and Barbarino, GC and Barish,
BC and Battistoni, G and Becherini, Y and Bellotti, R and Bemporad, C and Bernardini, P and Bilokon, H and Bower, C and Brigida, M and Bussino, S and Cafagna, F and Calicchio, M and Campana, D and Carboni, M and Caruso, R and Cecchini, S and Cei, F and Chiarella, V and Chiarusi, T and Choudhary,
BC and Coutu, S and Cozzi, M and De Cataldo and G and Dekhissi, H and De
Marzo, C and De Mitri and I and Derkaoui, J and De Vincenzi and M and Di
Credico, A and Erriquez, O and Favuzzi, C and Forti, C and Fusco, P and Giacomelli, G and Giannini, G and Giglietto, N and Giorgini, M and Grassi, M and Grillo, A and Gustavino, C and Habig, A and Hanson, K and Heinz, R and Katsavounidis, E and Katsavounidis, I and Kearns, E and Kim, H and Kyriazopoulou, S and Lamanna, E and Lane, C and Levin, DS and Lipari, P and Longley, NP and Longo, MJ and Loparco, F and Maaroufi, F and Mancarella, G and Mandrioli, G and Margiotta, A and Marini, A and Martello, D and Marzari-Chiesa, A and Mazziotta, MN and Michael, DG and Miller, L and Monacelli, P and Montaruli, T and Monteno, M and Mufson,
S and Musser, J and Nicolò, D and Nolty, R and Orth, C and Osteria, G and Palamara, O and Patrizii, L and Pazzi, R and Peck, CW and Perrone, L and Petrera, S and Popa, V and Rainò, A and Reynoldson, J and Ronga, F and Satriano, C and Scapparone, E and Scholberg, K and Serra, P and Sioli,
M and Sirri, G and Sitta, M and Spinelli, P and Spinetti, M and Spurio, M and Steinberg, R and Stone, JL},
Title = {Search for the sidereal and solar diurnal modulations in the
total MACRO muon data set},
Journal = {Physical Review D - Particles, Fields, Gravitation and
Cosmology},
Volume = {67},
Number = {4},
Pages = {042002},
Publisher = {American Physical Society (APS)},
Year = {2003},
Month = {January},
ISSN = {0556-2821},
url = {http://arxiv.org/pdf/astro-ph/0211119},
Abstract = {We have analyzed 44.3M single muons collected by MACRO from
1991 through 2000 in 2145 live days of operation. We have
searched for the solar diurnal, apparent sidereal, and
pseudosidereal modulation of the underground muon rate by
computing hourly deviations of the muon rate from 6 month
averages. We find evidence for statistically significant
modulations with the solar diurnal and the sidereal periods.
The amplitudes of these modulations are (Formula presented)
and are at the limit of the detector statistics. The
pseudosidereal modulation is not statistically significant.
The solar diurnal modulation is due to the daily atmospheric
temperature variations at 20 km, the altitude of primary
cosmic ray interactions with the atmosphere; MACRO is the
deepest experiment to report this result. The sidereal
modulation is in addition to the expected Compton-Getting
modulation due to solar system motion relative to the local
standard of rest; it represents motion of the solar system
with respect to the galactic cosmic rays toward the galactic
plane. © 2003 The American Physical Society.},
Doi = {10.1103/PhysRevD.67.042002},
Key = {Ambrosio:2002db}
}
@article{Ambrosio:2002ma,
Author = {Ambrosio, M and Antolini, R and Auriemma, G and Bakari, D and Baldini,
A and Barbarino, GC and Barish, BC and Battistoni, G and Becherini, Y and Bellotti, R and Bemporad, C and Bernardini, P and Bilokon, H and Bloise,
C and Bower, C and Brigida, M and Bussino, S and Cafagna, F and Calicchio,
M and Campana, D and Carboni, M and Caruso, R and Cecchini, S and Cei, F and Chiarella, V and Choudhary, BC and Coutu, S and Cozzi, M and de Cataldo,
G and Dekhissi, H and de Marzo, C and de Mitri, I and Derkaoui, J and de
Vincenzi, M and di Credico, A and Erriquez, O and Favuzzi, C and Forti,
C and Fusco, P and Giacomelli, G and Giannini, G and Giglietto, N and Giorgini, M and Grassi, M and Grillo, A and Guarino, F and Gustavino, C and Habig, A and Hanson, K and Heinz, R and Iarocci, E and Katsavounidis, E and Katsavounidis, I and Kearns, E and Kim, H and Kyriazopoulou, S and Lamanna, E and Lane, C and Levin, DS and Lipari, P and Longley, NP and Longo, MJ and Loparco, F and Maaroufi, F and Mancarella, G and Mandrioli, G and Margiotta, A and Marini, A and Martello, D and Marzari-Chiesa, A and Mazziotta, MN and Michael, DG and Monacelli, P and Montaruli, T and Monteno, M and Mufson, S and Musser, J and Nicolò, D and Nolty, R and Orth, C and Osteria, G and Palamara, O and Patera, V and Patrizii, L and Pazzi, R and Peck, CW and Perrone, L and Petrera, S and Pistilli, P and Popa, V and Rainò, A and Reynoldson, J and Ronga, F and Rrhioua, A and Satriano, C and Scapparone, E and Scholberg, K and Sciubba, A and Serra, P and Sioli, M},
Title = {Search for diffuse neutrino flux from astrophysical sources
with MACRO},
Journal = {Astroparticle Physics},
Volume = {19},
Number = {1},
Pages = {1-13},
Publisher = {Elsevier BV},
Year = {2003},
Month = {January},
ISSN = {0927-6505},
url = {http://arxiv.org/pdf/astro-ph/0203181},
Abstract = {Many galactic and extragalactic astrophysical sources are
currently considered promising candidates as high-energy
neutrino emitters. Astrophysical neutrinos can be detected
as upward-going muons produced in charged-current
interactions with the medium surrounding the detector. The
expected neutrino fluxes from various models start to
dominate on the atmospheric neutrino background at neutrino
energies above some tens of TeV. We present the results of a
search for an excess of high-energy upward-going muons among
the sample of data collected by MACRO during ∼5.8 years of
effective running time. No significant evidence for this
signal was found. As a consequence, an upper limit on the
flux of upward-going muons from high-energy neutrinos was
set at the level of 1.7 × 10 -14 cm -2 s -1 sr -1 . The
corresponding upper limit for the diffuse neutrino flux was
evaluated assuming a neutrino power law spectrum. Our result
was compared with theoretical predictions and upper limits
from other experiments. © 2002 Elsevier Science B.V. All
rights reserved.},
Doi = {10.1016/S0927-6505(02)00190-1},
Key = {Ambrosio:2002ma}
}
@article{Ambrosio:2002wr,
Author = {Ambrosio, M and Antolini, R and Auriemma, G and Bakari, D and Baldini,
A and Barbarino, GC and Barish, BC and Battistoni, G and Becherini, Y and Bellotti, R and Bemporad, C and Bernardini, P and Bilokon, H and Bloise,
C and Bower, C and Brigida, M and Bussino, S and Cafagna, F and Calicchio,
M and Campana, D and Carboni, M and Caruso, R and Cecchini, S and Cei, F and Chiarella, V and Choudhary, BC and Coutu, S and Cozzi, M and de Cataldo,
G and Dekhissi, H and de Marzo, C and de Mitri, I and Derkaoui, J and de
Vincenzi, M and di Credico, A and Erriquez, O and Favuzzi, C and Forti,
C and Fusco, P and Giacomelli, G and Giannini, G and Giglietto, N and Giorgini, M and Grassi, M and Grillo, A and Guarino, F and Gustavino, C and Habig, A and Hanson, K and Heinz, R and Iarocci, E and Katsavounidis, E and Katsavounidis, I and Kearns, E and Kim, H and Kyriazopoulou, S and Lamanna, E and Lane, C and Levin, DS and Lipari, P and Longley, NP and Longo, MJ and Loparco, F and Maaroufi, F and Mancarella, G and Mandrioli, G and Margiotta, A and Marini, A and Martello, D and Marzari-Chiesa, A and Mazziotta, MN and Michael, DG and Monacelli, P and Montaruli, T and Monteno, M and Mufson, S and Musser, J and Nicolò, D and Nolty, R and Orth, C and Osteria, G and Palamara, O and Patera, V and Patrizii, L and Pazzi, R and Peck, CW and Perrone, L and Petrera, S and Pistilli, P and Popa, V and Rainò, A and Reynoldson, J and Ronga, F and Rrhioua, A and Satriano, C and Scapparone, E and Scholberg, K and Sciubba, A and Serra, P and Sioli, M},
Title = {Search for cosmic ray sources using muons detected by the
MACRO experiment},
Journal = {Astroparticle Physics},
Volume = {18},
Number = {6},
Pages = {615-627},
Publisher = {Elsevier BV},
Year = {2003},
Month = {January},
ISSN = {0927-6505},
url = {http://arxiv.org/pdf/hep-ph/0204188},
Abstract = {The MACRO underground detector at Gran Sasso Laboratory
recorded 60 million secondary cosmic ray muons from February
1989 until December 2000. Different techniques were used to
analyze this sample in search for density excesses from
astrophysical point-like sources. No evidence for DC
excesses for any source in an all-sky survey is reported. In
addition, searches for muon excess correlated with the known
binary periods of Cygnus X-3 and Hercules X-1, and searches
for statistically significant bursting episodes from known
γ-ray sources are also proved negative. © 2002 Elsevier
Science B.V. All rights reserved.},
Doi = {10.1016/S0927-6505(02)00164-0},
Key = {Ambrosio:2002wr}
}
@article{Yoo:2003rc,
Author = {Yoo, J and Ashie, Y and Fukuda, S and Fukuda, Y and Ishihara, K and Itow,
Y and Koshio, Y and Minamino, A and Miura, M and Moriyama, S and Nakahata,
M and Namba, T and Nambu, R and Obayashi, Y and Sakurai, N and Shiozawa, M and Suzuki, Y and Takeuchi, H and Takeuchi, Y and Yamada, S and Ishitsuka,
M and Kajita, T and Kaneyuki, K and Nakayama, S and Okada, A and Ooyabu, T and Saji, C and Desai, S and Earl, M and Kearns, E and Messier, MD and Stone,
JL and Sulak, LR and Walter, CW and Goldhaber, M and Barszczak, T and Casper, D and Gajewski, W and Kropp, WR and Mine, S and Liu, DW and Smy,
MB and Sobel, HW and Vagins, MR and Gago, A and Ganezer, KS and Hill, J and Keig, WE and Kim, JY and Lim, IT and Ellsworth, RW and Tasaka, S and Kibayashi, A and Learned, JG and Matsuno, S and Takemori, D and Hayato,
Y and Ichikawa, AK and Ishii, T and Kameda, J and Kobayashi, T and Maruyama, T and Nakamura, K and Nitta, K and Oyama, Y and Sakuda, M and Totsuka, Y and Yoshida, M and Kohama, M and Iwashita, T and Suzuki, AT and Inagaki, T and Kato, I and Nakaya, T and Nishikawa, K and Haines, TJ and Dazeley, S and Hatakeyama, S and Svoboda, R and Blaufuss, E and Chen,
ML and Goodman, JA and Guillian, G and Sullivan, GW and Turcan, D and Scholberg, K and Habig, A and Ackermann, M and Jung, CK and Kalo, T and Kobayashi, K and Martens, K and Malek, M and Mauger, C and McGrew, C and Sharkey, E and Viren, B and Yanagisawa, C and Toshito,
T},
Title = {Search for periodic modulations of the solar neutrino flux
in Super-Kamiokande-I},
Journal = {Physical Review D},
Volume = {68},
Number = {9},
Pages = {092002},
Publisher = {American Physical Society (APS)},
Year = {2003},
Month = {January},
ISSN = {0556-2821},
url = {http://arxiv.org/pdf/hep-ex/0307070},
Abstract = {A search for periodic modulations of the solar neutrino flux
was performed using the Super-Kamiokande-I data taken from
31 May 1996 to 15 July 2001. The detector's capability of
measuring the exact time of events, combined with a
relatively high yield of solar neutrino events, allows a
search for short-time variations in the observed flux. We
employed the Lomb test to look for periodic modulations of
the observed solar neutrino flux. The obtained periodogram
is consistent with statistical fluctuation and no
significant periodicity was found. © 2003 The American
Physical Society.},
Doi = {10.1103/PhysRevD.68.092002},
Key = {Yoo:2003rc}
}
@article{Kim:2002pa,
Author = {Kim, BJ and Iwashita, T and Ishida, T and Jeon, EJ and Yokoyama, H and Aoki, S and Berns, HG and Bhang, HC and Boyd, S and Fujii, K and Hara, T and Hayato, Y and Hill, J and Ishii, T and Ishino, H and Jung, CK and Kearns,
E and Kim, HI and Kim, JH and Kim, JY and Kim, SB and Kobayashi, T and Kume,
G and Matsuno, S and Mine, S and Nakamura, K and Nakamura, M and Nishikawa,
K and Onchi, M and Otaki, T and Oyama, Y and Park, H and Sakuda, M and Sato,
K and Scholberg, K and Sharkey, E and Stone, JL and Suzuki, A and Takenaka,
K and Tamura, N and Tanaka, Y and Takatsuki, M and Walter, CW and Wilkes,
J and Yoo, J and Yoshida, M},
Title = {Tracking performance of the scintillating fiber detector in
the K2K experiment},
Journal = {Nuclear Instruments and Methods in Physics Research, Section
A: Accelerators, Spectrometers, Detectors and Associated
Equipment},
Volume = {497},
Number = {2-3},
Pages = {450-466},
Publisher = {Elsevier BV},
Year = {2003},
Month = {February},
ISSN = {0168-9002},
url = {http://arxiv.org/pdf/hep-ex/0206041},
Abstract = {Tracking performance of the scintillating fiber detector
(SciFi) in the K2K experiment was studied. SciFi was used to
reconstruct charged particles produced in neutrino
interactions in the near detector. The track reconstruction
algorithm and the performance of SciFi was also described
after three years of operation.},
Doi = {10.1016/S0168-9002(02)01980-0},
Key = {Kim:2002pa}
}
@article{Malek:2002ns,
Author = {Malek, M and Morii, M and Fukuda, S and Fukuda, Y and Ishitsuka, M and Itow, Y and Kajita, T and Kameda, J and Kaneyuki, K and Kobayashi, K and Koshio, Y and Miura, M and Moriyama, S and Nakahata, M and Nakayama, S and Namba, T and Okada, A and Ooyabu, T and Saji, C and Sakurai, N and Shiozawa, M and Suzuki, Y and Takeuchi, H and Takeuchi, Y and Totsuka,
Y and Yamada, S and Desai, S and Earl, M and Kearns, E and Messier, MD and Stone, JL and Sulak, LR and Walter, CW and Goldhaber, M and Barszczak,
T and Casper, D and Gajewski, W and Kropp, WR and Mine, S and Liu, DW and Smy,
MB and Sobel, HW and Vagins, MR and Gago, A and Ganezer, KS and Keig, WE and Ellsworth, RW and Tasaka, S and Kibayashi, A and Learned, JG and Matsuno, S and Takemori, D and Hayato, Y and Ishii, T and Kobayashi, T and Maruyama, T and Nakamura, K and Obayashi, Y and Oyama, Y and Sakuda, M and Yoshida, M and Kohama, M and Iwashita, T and Suzuki, AT and Ichikawa, A and Inagaki, T and Kato, I and Nakaya, T and Nishikawa, K and Haines, TJ and Dazeley, S and Hatakeyama, S and Svoboda, R and Blaufuss, E and Goodman,
JA and Guillian, G and Sullivan, GW and Turcan, D and Scholberg, K and Habig, A and Ackermann, M and Hill, J and Jung, CK and Martens, K and Mauger, C and McGrew, C and Sharkey, E and Viren, B and Yanagisawa, C and Toshito, T and Mitsuda, C and Miyano, K and Shibata, T and Kajiyama, Y and Nagashima, Y and Nitta, K and Takita, M and Kim, HI and Kim, SB and Yoo, J and Okazawa, H and Ishizuka, T and Etoh, M and Gando, Y and Hasegawa, T and Inoue, K and Ishihara, K and Shirai, J and Suzuki, A and Koshiba, M and Hatakeyama, Y and Ichikawa, Y and Koike, M and Nishijima, K and Ishino,
H and Nishimura, R and Watanabe, Y and Kielczewska, D and Berns, HG and Boyd, SC and Stachyra, AL and Wilkes, RJ and Super-Kamiokande
Collaboration},
Title = {Search for supernova relic neutrinos at Super-Kamiokande.},
Journal = {Physical review letters},
Volume = {90},
Number = {6},
Pages = {061101},
Year = {2003},
Month = {February},
ISSN = {0031-9007},
url = {http://www.ncbi.nlm.nih.gov/pubmed/12633283},
Abstract = {A search for the relic neutrinos from all past core-collapse
supernovae was conducted using 1496 days of data from the
Super-Kamiokande detector. This analysis looked for
electron-type antineutrinos that had produced a positron
with an energy greater than 18 MeV. In the absence of a
signal, 90% C.L. upper limits on the total flux were set for
several theoretical models; these limits ranged from 20 to
130 macro nu(e) cm(-2) s(-1). Additionally, an upper bound
of 1.2 macro nu(e) cm(-2) s(-1) was set for the supernova
relic neutrino flux in the energy region E(nu)>19.3
MeV.},
Doi = {10.1103/physrevlett.90.061101},
Key = {Malek:2002ns}
}
@article{Walter:2002wh,
Author = {WALTER, CW},
Title = {RECENT RESULTS FROM THE K2K EXPERIMENT},
Journal = {Fundamental Interactions},
Volume = {C0209101},
Pages = {TH03},
Publisher = {WORLD SCIENTIFIC},
Year = {2003},
Month = {February},
ISBN = {9789812382931},
url = {http://arxiv.org/pdf/hep-ex/0211059},
Abstract = {http://arxiv.org/abs/hep-ex/0211059},
Doi = {10.1142/9789812705136_0044},
Key = {Walter:2002wh}
}
@article{Fukuda:2002uc,
Author = {Fukuda, S and Fukuda, Y and Hayakawa, T and Ichihara, E and Ishitsuka,
M and Itow, Y and Kajita, T and Kameda, J and Kaneyuki, K and Kasuga, S and Kobayashi, K and Kobayashi, Y and Koshio, Y and Miura, M and Moriyama,
S and Nakahata, M and Nakayama, S and Namba, T and Obayashi, Y and Okada,
A and Oketa, M and Okumura, K and Oyabu, T and Sakurai, N and Shiozawa, M and Suzuki, Y and Takeuchi, Y and Toshito, T and Totsuka, Y and Yamada, S and Desai, S and Earl, M and Hong, JT and Kearns, E and Masuzawa, M and Messier, MD and Stone, JL and Sulak, LR and Walter, CW and Wang, W and Scholberg, K and Barszczak, T and Casper, D and Liu, DW and Gajewski, W and Halverson, PG and Hsu, J and Kropp, WR and Mine, S and Price, LR and Reines, F and Smy, M and Sobel, HW and Vagins, MR and Ganezer, KS and Keig,
WE and Ellsworth, RW and Tasaka, S and Flanagan, JW and Kibayashi, A and Learned, JG and Matsuno, S and Stenger, VJ and Hayato, Y and Ishii, T and Ichikawa, A and Kanzaki, J and Kobayashi, T and Maruyama, T and Nakamura, K and Oyama, Y and Sakai, A and Sakuda, M and Sasaki, O and Echigo, S and Iwashita, T and Kohama, M and Suzuki, AT and Hasegawa, M and Inagaki, T and Kato, I and Maesaka, H and Nakaya, T and Nishikawa, K and Yamamoto, S and Haines, TJ and Kim, BK and Sanford, R and Svoboda, R and Blaufuss, E and Chen, ML and Conner, Z and Goodman, JA and Guillian, E and Sullivan, GW and Turcan, D and Habig, A and Ackerman, M and Goebel, F and Hill, J},
Title = {The Super-Kamiokande detector},
Journal = {Nuclear Instruments and Methods in Physics Research, Section
A: Accelerators, Spectrometers, Detectors and Associated
Equipment},
Volume = {501},
Number = {2-3},
Pages = {418-462},
Publisher = {Elsevier BV},
Year = {2003},
Month = {April},
ISSN = {0168-9002},
url = {http://dx.doi.org/10.1016/S0168-9002(03)00425-X},
Abstract = {Super-Kamiokande is the world's largest water Cherenkov
detector, with net mass 50,000 tons. During the period
April, 1996 to July, 2001, Super-Kamiokande I collected 1678
live-days of data, observing neutrinos from the Sun, Earth's
atmosphere, and the K2K long-baseline neutrino beam with
high efficiency. These data provided crucial information for
our current understanding of neutrino oscillations, as well
as setting stringent limits on nucleon decay. In this paper,
we describe the detector in detail, including its site,
configuration, data acquisition equipment, online and
offline software, and calibration systems which were used
during Super-Kamiokande I. © 2003 Elsevier Science B.V. All
rights reserved.},
Doi = {10.1016/S0168-9002(03)00425-X},
Key = {Fukuda:2002uc}
}
@article{Walter:2003zj,
Author = {Walter, CW},
Title = {Distinguishing νμ→ντ
oscillations and exotic oscillation/decay hypotheses using
Super-K atmospheric neutrino data},
Journal = {Nuclear Instruments and Methods in Physics Research, Section
A: Accelerators, Spectrometers, Detectors and Associated
Equipment},
Volume = {503},
Number = {1-2},
Pages = {110-113},
Publisher = {Elsevier BV},
Year = {2003},
Month = {May},
ISSN = {0168-9002},
url = {http://dx.doi.org/10.1016/S0168-9002(03)00649-1},
Abstract = {In this talk, I will review the Super-K analysis to
distinguish between the νμ→ντ oscillation hypothesis
and other exotic oscillation/decay scenarios. All of the
tested exotic hypotheses are excluded by the Super-K
atmospheric neutrino data at the greater than 4σ level. A
limit is placed on the admixture of νsterile states in a
ντ, νsterile mixture to be less than 25% at 90% CL. In
addition, a 2.2σ tau lepton appearance signal is reported
which is consistent with our expectation of νμ→ντ
oscillations. © 2003 Elsevier Science B.V. All rights
reserved.},
Doi = {10.1016/S0168-9002(03)00649-1},
Key = {Walter:2003zj}
}
@article{Gando:2002ub,
Author = {Gando, Y and Fukuda, S and Fukuda, Y and Ishitsuka, M and Itow, Y and Kajita, T and Kameda, J and Kaneyuki, K and Kobayashi, K and Koshio, Y and Miura, M and Moriyama, S and Nakahata, M and Nakayama, S and Namba, T and Obayashi, Y and Okada, A and Ooyabu, T and Saji, C and Sakurai, N and Shiozawa, M and Suzuki, Y and Takeuchi, H and Takeuchi, Y and Totsuka,
Y and Yamada, S and Desai, S and Earl, M and Kearns, E and Messier, MD and Stone, JL and Sulak, LR and Walter, CW and Goldhaber, M and Barszczak,
T and Casper, D and Gajewski, W and Kropp, WR and Mine, S and Liu, DW and Smy,
MB and Sobel, HW and Vagins, MR and Gago, A and Ganezer, KS and Hill, J and Keig, WE and Ellsworth, RW and Tasaka, S and Kibayashi, A and Learned,
JG and Matsuno, S and Takemori, D and Hayato, Y and Ichikawa, AK and Ishii,
T and Kobayashi, T and Maruyama, T and Nakamura, K and Oyama, Y and Sakuda,
M and Yoshida, M and Kohama, M and Iwashita, T and Suzuki, AT and Inagaki,
T and Kato, I and Nakaya, T and Nishikawa, K and Haines, TJ and Dazeley, S and Hatakeyama, S and Svoboda, R and Blaufuss, E and Chen, ML and Goodman,
JA and Guillian, G and Sullivan, GW and Turcan, D and Scholberg, K and Habig, A and Ackermann, M and Jung, CK and Martens, K and Malek, M and Mauger, C and McGrew, C and Sharkey, E and Viren, B and Yanagisawa, C and Toshito, T and Mitsuda, C and Miyano, K and Shibata, T and Kajiyama, Y and Nagashima, Y and Nitta, K and Takita, M and Kim, HI and Kim, SB and Yoo, J and Okazawa, H and Ishizuka, T and Etoh, M and Hasegawa, T and Inoue, K and Ishihara, K and Shirai, J and Suzuki, A and Koshiba, M and Hatakeyama,
Y and Ichikawa, Y and Koike, M and Nishijima, K and Ishino, H and Morii, M and Nishimura, R and Watanabe, Y and Kielczewska, D and Berns, HG and Boyd,
SC and Stachyra, AL and Wilkes, RJ and Super-Kamiokande
Collaboration},
Title = {Search for nu(e) from the sun at Super-Kamiokande-I.},
Journal = {Physical review letters},
Volume = {90},
Number = {17},
Pages = {171302},
Year = {2003},
Month = {May},
ISSN = {0031-9007},
url = {http://www.ncbi.nlm.nih.gov/pubmed/12786067},
Abstract = {We present the results of a search for low energy nu(e) from
the Sun using 1496 days of data from Super-Kamiokande-I. We
observe no significant excess of events and set an upper
limit for the conversion probability to nu(e) of the 8B
solar neutrino. This conversion limit is 0.8% (90% C.L.) of
the standard solar model's neutrino flux for total
energy=8-20 MeV. We also set a flux limit for monochromatic
nu(e) for E(nu(e))=10-17 MeV.},
Doi = {10.1103/physrevlett.90.171302},
Key = {Gando:2002ub}
}
@article{Ambrosio:2002id,
Author = {Ambrosio, M and Antolini, R and Baldini, A and Barbarino, GC and Barish,
BC and Battistoni, G and Becherini, Y and Bellotti, R and Bemporad, C and Bernardini, P and Bilokon, H and Bower, C and Brigida, M and Bussino, S and Cafagna, F and Calicchio, M and Campana, D and Carboni, M and Caruso, R and Cecchini, S and Cei, F and Chiarella, V and Choudhary, BC and Coutu, S and Cozzi, M and de Cataldo, G and Dekhissi, H and de Marzo, C and de Mitri,
I and Derkaoui, J and de Vincenzi, M and di Credico, A and Erriquez, O and Favuzzi, C and Forti, C and Fusco, P and Giacomelli, G and Giannini, G and Giglietto, N and Giorgini, M and Grassi, M and Grillo, A and Guarino, F and Gustavino, C and Habig, A and Hanson, K and Heinz, R and Iarocci, E and Katsavounidis, E and Katsavounidis, I and Kearns, E and Kim, H and Kyriazopoulou, S and Lamanna, E and Lane, C and Levin, DS and Lipari, P and Longley, NP and Longo, MJ and Loparco, F and Mancarella, G and Mandrioli, G and Margiotta, A and Marini, A and Martello, D and Marzari-Chiesa, A and Mazziotta, MN and Michael, DG and Monacelli, P and Montaruli, T and Monteno, M and Mufson, S and Musser, J and Nicolò, D and Nolty, R and Orth, C and Osteria, G and Palamara, O and Patera, V and Patrizii, L and Pazzi, R and Peck, CW and Perrone, L and Petrera, S and Pistilli, P and Popa, V and Rainò, A and Reynoldson, J and Ronga, F and Satriano, C and Scapparone, E and Scholberg, K and Sciubba, A and Serra,
P and Sioli, M and Sirri, G and Sitta, M and Spinelli, P and Spinetti, M and Spurio, M},
Title = {Measurement of the residual energy of muons in the Gran
Sasso underground laboratories},
Journal = {Astroparticle Physics},
Volume = {19},
Number = {3},
Pages = {313-328},
Publisher = {Elsevier BV},
Year = {2003},
Month = {June},
ISSN = {0927-6505},
url = {http://arxiv.org/pdf/hep-ex/0207043},
Abstract = {The MACRO detector was located in the Hall B of the Gran
Sasso underground laboratories under an average rock
overburden of 3700 hg/cm2. A transition radiation detector
composed of three identical modules, covering a total
horizontal area of 36 m2, was installed inside the empty
upper part of the detector in order to measure the residual
energy of muons. This paper presents the measurement of the
residual energy of single and double muons crossing the
apparatus. Our data show that double muons are more
energetic than single ones. This measurement is performed
over a standard rock depth range from 3000 to 6500 hg/cm2.
© 2002 Elsevier Science B.V. All rights
reserved.},
Doi = {10.1016/S0927-6505(02)00217-7},
Key = {Ambrosio:2002id}
}
@article{Ambrosio:2003yz,
Author = {Ambrosio, M and Antolini, R and Bakari, D and Baldini, A and Barbarino,
GC and Barish, BC and Battistoni, G and Becherini, Y and Bellotti, R and Bemporad, C and Bernardini, P and Bilokon, H and Bloise, C and Bower, C and Brigida, M and Bussino, S and Cafagna, F and Calicchio, M and Campana,
D and Carboni, M and Caruso, R and Cecchini, S and Cei, F and Chiarella, V and Chiarusi, T and Choudhary, BC and Coutu, S and Cozzi, M and de Cataldo,
G and Dekhissi, H and de Marzo, C and de Mitri, I and Derkaoui, J and de
Vincenzi, M and di Credico, A and Favuzzi, C and Forti, C and Fusco, P and Giacomelli, G and Giannini, G and Giglietto, N and Giorgini, M and Grassi, M and Grillo, A and Gustavino, C and Habig, A and Hanson, K and Heinz, R and Iarocci, E and Katsavounidis, E and Katsavounidis, I and Kearns, E and Kim, H and Kumar, A and Kyriazopoulou, S and Lamanna, E and Lane, C and Levin, DS and Lipari, P and Longo, MJ and Loparco, F and Maaroufi, F and Mancarella, G and Mandrioli, G and Manzoor, S and Margiotta, A and Marini, A and Martello, D and Marzari-Chiesa, A and Mazziotta, MN and Michael, DG and Mikheyev, S and Monacelli, P and Montaruli, T and Monteno, M and Mufson, S and Musser, J and Nicolò, D and Nolty, R and Orth, C and Osteria, G and Palamara, O and Patera, V and Patrizii, L and Pazzi, R and Peck, CW and Perrone, L and Petrera, S and Popa, V and Rainò, A and Reynoldson, J and Ronga, F and Rrhioua, A and Satriano, C and Scapparone, E and Scholberg, K and Sciubba, A and Serra,
P and Sioli, M and Sirri, G},
Title = {Atmospheric neutrino oscillations from upward throughgoing
muon multiple scattering in MACRO},
Journal = {Physics Letters, Section B: Nuclear, Elementary Particle and
High-Energy Physics},
Volume = {566},
Number = {1-2},
Pages = {35-44},
Publisher = {Elsevier BV},
Year = {2003},
Month = {July},
ISSN = {0370-2693},
url = {http://arxiv.org/pdf/hep-ex/0304037},
Abstract = {The energy of atmospheric neutrinos detected by MACRO was
estimated using multiple Coulomb scattering of upward
throughgoing muons. This analysis allows a test of
atmospheric neutrino oscillations, relying on the distortion
of the muon energy distribution. These results have been
combined with those coming from the upward throughgoing muon
angular distribution only. Both analyses are independent of
the neutrino flux normalization and provide strong evidence,
above the 4σ level, in favour of neutrino oscillations. ©
2003 Published by Elsevier B.V.},
Doi = {10.1016/S0370-2693(03)00806-2},
Key = {Ambrosio:2003yz}
}
@article{Ambrosio:2003mz,
Author = {Ambrosio, M and Antolini, R and Baldini, A and Barbarino, GC and Barish,
BC and Battistoni, G and Becherini, Y and Bellotti, R and Bemporad, C and Bernardini, P and Bilokon, H and Bower, C and Brigida, M and Bussino, S and Cafagna, F and Calicchio, M and Campana, D and Carboni, M and Caruso, R and Cecchini, S and Cei, F and Chiarella, V and Chiarusi, T and Choudhary,
BC and Coutu, S and Cozzi, M and de Cataldo, G and Dekhissi, H and de
Marzo, C and de Mitri, I and Derkaoui, J and de Vincenzi, M and di
Credico, A and Erriquez, O and Favuzzi, C and Forti, C and Fusco, P and Giacomelli, G and Giannini, G and Giglietto, N and Giorgini, M and Grassi, M and Grillo, A and Gustavino, C and Habig, A and Hanson, K and Heinz, R and Katsavounidis, E and Katsavounidis, I and Kearns, E and Kim, H and Kumar, A and Kyriazopoulou, S and Lamanna, E and Lane, C and Levin, DS and Lipari, P and Longley, NP and Longo, MJ and Loparco, F and Maaroufi, F and Mancarella, G and Mandrioli, G and Manzoor, S and Margiotta, A and Marini, A and Martello, D and Marzari-Chiesa, A and Mazziotta, MN and Michael, DG and Monacelli, P and Montaruli, T and Monteno, M and Mufson, S and Musser, J and Nicolò, D and Nolty, R and Orth, C and Osteria, G and Palamara, O and Patrizii, L and Pazzi, R and Peck, CW and Perrone, L and Petrera, S and Popa, V and Rainò, A and Reynoldson, J and Ronga, F and Satriano, C and Scapparone, E and Scholberg, K and Sioli, M and Sirri, G and Sitta, M and Spinelli, P and Spinetti, M and Spurio, M and Steinberg, R and Stone,
JL},
Title = {Moon and Sun shadowing effect in the MACRO
detector},
Journal = {Astroparticle Physics},
Volume = {20},
Number = {2},
Pages = {145-156},
Publisher = {Elsevier BV},
Year = {2003},
Month = {November},
ISSN = {0927-6505},
url = {http://arxiv.org/pdf/astro-ph/0302586},
Abstract = {Using data collected by the MACRO experiment from 1989 to
the end of its operations in 2000, we have studied in the
underground muon flux the shadowing effects due to both the
Moon and the Sun. We have observed the shadow cast by the
Moon at its apparent position with a significance of 6.5σ.
The Moon shadowing effect has been used to verify the
pointing capability of the detector and to determine the
instrument resolution for the search of muon excesses from
any direction of the celestial sphere. The dependence of the
effect on the geomagnetic field is clearly shown by
splitting the data sample in day and night observations. The
Sun shadow, observed with a significance of 4.6σ is
displaced by about 0.6° from its apparent position. In this
case however the explanation resides in the configuration of
the Solar and Interplanetary Magnetic Fields, which affect
the propagation of cosmic ray particles between the Sun, and
the Earth. The displacement of the Sun shadow with respect
to the real Sun position has been used to establish an upper
limit on the antimatter flux in cosmic rays of about 48% at
68% c.l. and primary energies of about 20 TeV. © 2003
Elsevier B.V. All rights reserved.},
Doi = {10.1016/S0927-6505(03)00169-5},
Key = {Ambrosio:2003mz}
}
@article{Walter:2004de,
Author = {Walter, CW},
Title = {Low Energy Neutrino-Nucleus Interactions},
Journal = {AIP Conference Proceedings},
Volume = {721},
Pages = {247-251},
Publisher = {AIP},
Editor = {Para, A},
Year = {2004},
ISBN = {0-7354-0201-9},
url = {http://dx.doi.org/10.1063/1.1818408},
Doi = {10.1063/1.1818408},
Key = {Walter:2004de}
}
@article{Smy:2003jf,
Author = {Smy, MB and Ashie, Y and Fukuda, S and Fukuda, Y and Ishihara, K and Itow,
Y and Koshio, Y and Minamino, A and Miura, M and Moriyama, S and Nakahata,
M and Namba, T and Nambu, R and Obayashi, Y and Sakurai, N and Shiozawa, M and Suzuki, Y and Takeuchi, H and Takeuchi, Y and Yamada, S and Ishitsuka,
M and Kajita, T and Kaneyuki, K and Nakayama, S and Okada, A and Ooyabu, T and Saji, C and Desai, S and Earl, M and Kearns, E and Messier, MD and Stone,
JL and Sulak, LR and Walter, CW and Wang, W and Goldhaber, M and Barszczak,
T and Casper, D and Gajewski, W and Kropp, WR and Mine, S and Liu, DW and Sobel, HW and Vagins, MR and Gago, A and Ganezer, KS and Hill, J and Keig,
WE and Kim, JY and Lim, IT and Ellsworth, RW and Tasaka, S and Kibayashi,
A and Learned, JG and Matsuno, S and Takemori, D and Hayato, Y and Ichikawa, AK and Ishii, T and Kameda, J and Kobayashi, T and Maruyama,
T and Nakamura, K and Nitta, K and Oyama, Y and Sakuda, M and Totsuka, Y and Yoshida, M and Iwashita, T and Suzuki, AT and Inagaki, T and Kato, I and Nakaya, T and Nishikawa, K and Haines, TJ and Dazeley, S and Hatakeyama,
S and Svoboda, R and Blaufuss, E and Goodman, JA and Guillian, G and Sullivan, GW and Turcan, D and Scholberg, K and Habig, A and Ackermann,
M and Jung, CK and Kato, T and Kobayashi, K and Martens, K and Malek, M and Mauger, C and McGrew, C and Sharkey, E and Viren, B and Yanagisawa, C and Toshito, T and Mitsuda, C and Miyano, K and Shibata,
T},
Title = {Precise measurement of the solar neutrino day-night and
seasonal variation in Super-Kamiokande-I},
Journal = {Physical Review D - Particles, Fields, Gravitation and
Cosmology},
Volume = {69},
Number = {1},
Pages = {011104},
Publisher = {American Physical Society (APS)},
Year = {2004},
Month = {January},
ISSN = {0556-2821},
url = {http://arxiv.org/pdf/hep-ex/0309011},
Abstract = {The time variation of the elastic scattering rate of solar
neutrinos with electrons in Super-Kamiokande-I was fit to
the variations expected from active two-neutrino
oscillations. The best fit in the large mixing angle
solution has a mixing angle of [Formula Presented] and a
mass squared difference of [Formula Presented] between the
two neutrino mass eigenstates. The fitted day-night
asymmetry of [Formula Presented] has improved statistical
precision over previous measurements and agrees well with
the expected asymmetry of [Formula Presented] © 2004 The
American Physical Society.},
Doi = {10.1103/PhysRevD.69.011104},
Key = {Smy:2003jf}
}
@article{Desai:2004pq,
Author = {Desai, S and Ashie, Y and Fukuda, S and Fukuda, Y and Ishihara, K and Itow,
Y and Koshio, Y and Minamino, A and Miura, M and Moriyama, S and Nakahata,
M and Namba, T and Nambu, R and Obayashi, Y and Sakurai, N and Shiozawa, M and Suzuki, Y and Takeuchi, H and Takeuchi, Y and Yamada, S and Ishitsuka,
M and Kajita, T and Kaneyuki, K and Nakayama, S and Okada, A and Ooyabu, T and Saji, C and Earl, M and Kearns, E and Stone, JL and Sulak, LR and Walter,
CW and Wang, W and Goldhaber, M and Barszczak, T and Casper, D and Cravens,
JP and Gajewski, W and Kropp, WR and Mine, S and Liu, DW and Smy, MB and Sobel, HW and Sterner, CW and Vagins, MR and Ganezer, KS and Hill, J and Keig, WE and Kim, JY and Lim, IT and Ellsworth, RW and Tasaka, S and Guillian, G and Kibayashi, A and Learned, JG and Matsuno, S and Takemori, D and Messier, MD and Hayato, Y and Ichikawa, AK and Ishida,
T and Ishii, T and Iwashita, T and Kameda, J and Kobayashi, T and Maruyama,
T and Nakamura, K and Nitta, K and Oyama, Y and Sakuda, M and Totsuka, Y and Suzuki, AT and Hasegawa, M and Hayashi, K and Inagaki, T and Kato, I and Maesaka, H and Morita, T and Nakaya, T and Nishikawa, K and Sasaki, T and Ueda, S and Yamamoto, S and Haines, TJ and Dazeley, S and Hatakeyama, S and Svoboda, R and Blaufuss, E and Goodman, JA and Sullivan, GW and Turcan,
D and Scholberg, K and Habig, A and Jung, CK and Kato, T and Kobayashi, K and Malek, M and Mauger, C and McGrew, C and Sarrat, A},
Title = {Search for dark matter WIMPs using upward through-going
muons in Super-Kamiokande},
Journal = {Physical Review D - Particles, Fields, Gravitation and
Cosmology},
Volume = {70},
Number = {8},
Pages = {083523-1-083523-11},
Publisher = {American Physical Society (APS)},
Year = {2004},
Month = {January},
ISSN = {0556-2821},
url = {http://arxiv.org/pdf/hep-ex/0404025},
Abstract = {We present the results of indirect searches for Weakly
Interacting Massive Particles (WIMPs), with 1679.6 live days
of data from the Super-Kamiokande detector using
neutrino-induced upward through-going muons. The search is
performed by looking for an excess of high energy muon
neutrinos from WIMP annihilations in the Sun, the core of
the Earth, and the Galactic Center, as compared to the
number expected from the atmospheric neutrino background. No
statistically significant excess was seen. We calculate the
flux limits in various angular cones around each of the
above celestial objects. We obtain conservative
model-independent upper limits on the WIMP-nucleon cross
section as a function of WIMP mass, and compare these
results with the corresponding results from direct dark
matter detection experiments. © 2004 The American Physical
Society.},
Doi = {10.1103/PhysRevD.70.083523},
Key = {Desai:2004pq}
}
@article{Ambrosio:2004ub,
Author = {Collaboration, TMACRO},
Title = {Final Search for Lightly Ionizing Particles with the MACRO
detector},
Year = {2004},
Month = {February},
url = {http://arxiv.org/pdf/hep-ex/0402006},
Abstract = {We present the final results of a search for lightly
ionizing particles using the entire cosmic ray data set the
MACRO detector collected during its 1995-2000 run. Like the
original search performed with the data of 1995-96, this
search was sensitive to fractionally charged particles with
an electric charge q as low as e/5 and with velocities
between approximately 0.25c and c. The efficiency of this
search was approx 70% for q = e/5 and increased rapidly to
100% for higher charges. No candidate events were observed.
This corresponds to a 90% C. L. upper limit on their
isotropic flux of 6.1x10^-16 cm^-2 sec^-1 sr^-1 which
represents the most stringent experimental limit ever
obtained.},
Key = {Ambrosio:2004ub}
}
@article{fds304629,
Author = {Aglietta, M and Alessandro, B and Antonioli, P and Arneodo, F and Bergamasco, L and Bertaina, M and Castagnoli, C and Castellina, A and Chiavassa, A and Cini, G and D'Ettorre Piazzoli and B and di Sciascio,
G and Fulgione, W and Galeotti, P and Ghia, PL and Iacovacci, M and Mannocchi, G and Morello, C and Navarra, G and Saavedra, O and Stamerra,
A and Trinchero, GC and Valchierotti, S and Vallania, P and Vernetto, S and Vigorito, C and Ambrosio, M and Antolini, R and Baldini, A and Barbarino, GC and Barish, BC and Battistoni, G and Becherini, Y and Bellotti, R and Bemporad, C and Bernardini, P and Bilokon, H and Bower,
C and Brigida, M and Bussino, S and Cafagna, F and Calicchio, M and Campana, D and Carboni, M and Caruso, R and Cecchini, S and Cei, F and Chiarella, V and Choudhary, BC and Coutu, S and Cozzi, M and de Cataldo,
G and Dekhissi, H and de Marzo, C and de Mitri, I and Derkaoui, J and de
Vincenzi, M and di Credico, A and Erriquez, O and Favuzzi, C and Forti,
C and Fusco, P and Giacomelli, G and Giannini, G and Giglietto, N and Giorgini, M and Grassi, M and Grillo, A and Guarino, F and Gustavino, C and Habig, A and Hanson, K and Heinz, R and Iarocci, E and Katsavounidis, E and Katsavounidis, I and Kearns, E and Kim, H and Kyriazopoulou, S and Lamanna, E and Lane, C and Levin, DS and Lipari, P and Longley, NP and Longo, MJ and Loparco, F and Maaroufi, F and Mancarella, G and Mandrioli, G and Margiotta, A and Marini, A and Martello, D and Marzari-Chiesa, A and Mazziotta, MN and Michael, DG and Monacelli, P and Montaruli, T and Monteno, M and Mufson, S and Musser,
J},
Title = {The cosmic ray primary composition between 1015
and 1016 eV from Extensive Air Showers
electromagnetic and TeV muon data},
Journal = {Astroparticle Physics},
Volume = {20},
Number = {6},
Pages = {641-652},
Publisher = {Elsevier BV},
Year = {2004},
Month = {March},
ISSN = {0927-6505},
url = {http://dx.doi.org/10.1016/j.astropartphys.2003.10.004},
Abstract = {The cosmic ray primary composition in the energy range
between 1015 and 1016 eV, i.e., around the "knee" of the
primary spectrum, has been studied through the combined
measurements of the EAS-TOP air shower array (2005 m a.s.l.,
105 m2 collecting area) and the MACRO underground detector
(963 m a.s.l., 3100 m w.e. of minimum rock overburden, 920
m2 effective area) at the National Gran Sasso Laboratories.
The used observables are the air shower size (Ne) measured
by EAS-TOP and the muon number (Nμ) recorded by MACRO. The
two detectors are separated on average by 1200 m of rock,
and located at a respective zenith angle of about 30°. The
energy threshold at the surface for muons reaching the MACRO
depth is approximately 1.3 TeV. Such muons are produced in
the early stages of the shower development and in a
kinematic region quite different from the one relevant for
the usual Nμ-Ne studies. The measurement leads to a primary
composition becoming heavier at the knee of the primary
spectrum, the knee itself resulting from the steepening of
the spectrum of a primary light component (p, He) of Δγ=
0.7±0.4 at E0∼4×1015 eV. The result confirms the ones
reported from the observation of the low energy muons at the
surface (typically in the GeV energy range), showing that
the conclusions do not depend on the production region
kinematics. Thus, the hadronic interaction model used
(CORSIKA/QGSJET) provides consistent composition results
from data related to secondaries produced in a rapidity
region exceeding the central one. Such an evolution of the
composition in the knee region supports the "standard"
galactic acceleration/propagation models that imply rigidity
dependent breaks of the different components, and therefore
breaks occurring at lower energies in the spectra of the
light nuclei. © 2003 Elsevier B.V. All rights
reserved.},
Doi = {10.1016/j.astropartphys.2003.10.004},
Key = {fds304629}
}
@article{Aglietta:2004ws,
Author = {Aglietta, M and Alessandro, B and Antonioli, P and Arneodo, F and Bergamasco, L and Bertaina, M and Castagnoli, C and Castellina, A and Chiavassa, A and Cini, G and D'Ettorre Piazzoli and B and di Sciascio,
G and Fulgione, W and Galeotti, P and Ghia, PL and Iacovacci, M and Mannocchi, G and Morello, C and Navarra, G and Saavedra, O and Stamerra,
A and Trinchero, GC and Valchierotti, S and Vallania, P and Vernetto, S and Vigorito, C and Ambrosio, M and Antolini, R and Baldini, A and Barbarino, GC and Barish, BC and Battistoni, G and Becherini, Y and Bellotti, R and Bemporad, C and Bernardini, P and Bilokon, H and Bower,
C and Brigida, M and Bussino, S and Cafagna, F and Calicchio, M and Campana, D and Carboni, M and Caruso, R and Cecchini, S and Cei, F and Chiarella, V and Chiarusi, T and Choudhary, BC and Coutu, S and Cozzi,
M and de Cataldo, G and Dekhissi, H and de Marzo, C and de Mitri, I and Derkaoui, J and de Vincenzi, M and di Credico, A and Erriquez, O and Favuzzi, C and Forti, C and Fusco, P and Giacomelli, G and Giannini, G and Giglietto, N and Giorgini, M and Grassi, M and Grillo, A and Guarino, F and Gustavino, C and Habig, A and Hanson, K and Heinz, R and Iarocci, E and Katsavounidis, E and Katsavounidis, I and Kearns, E and Kim, H and Kyriazopoulou, S and Lamanna, E and Lane, C and Levin, DS and Lipari, P and Longley, NP and Longo, MJ and Loparco, F and Maaroufi, F and Mancarella,
G and Mandrioli, G and Margiotta, A and Marini, A and Martello, D and Marzari-Chiesa, A and Mazziotta, MN and Michael, DG and Monacelli, P and Montaruli, T and Monteno, M and Mufson, S},
Title = {The cosmic ray proton, helium and CNO fluxes in the 100 TeV
energy region from TeV muons and EAS atmospheric Cherenkov
light observations of MACRO and EAS-TOP},
Journal = {Astroparticle Physics},
Volume = {21},
Number = {3},
Pages = {223-240},
Publisher = {Elsevier BV},
Year = {2004},
Month = {June},
ISSN = {0927-6505},
url = {http://dx.doi.org/10.1016/j.astropartphys.2004.01.005},
Abstract = {The primary cosmic ray (CR) proton, helium and CNO fluxes in
the energy range 80-300 TeV are studied at the National Gran
Sasso Laboratories by means of EAS-TOP (Campo Imperatore,
2005 m a.s.l.) and MACRO (deep underground, 3100 m w.e., the
surface energy threshold for a muon reaching the detector
being Eμth≈1.3 TeV). The measurement is based on: (a) the
selection of primaries based on their energy/nucleon (i.e.,
with energy/nucleon sufficient to produce a muon with energy
larger than 1.3 TeV) and the reconstruction of the shower
geometry by means of the muons recorded by MACRO in the deep
underground laboratories; (b) the detection of the
associated atmospheric Cherenkov light (C.l.) signals by
means of the C.l. detector of EAS-TOP. The C.l. density at
core distance r>100 m is directly related to the total
primary energy E0. Proton and helium ("p + He") and proton,
helium and CNO ("p + He + CNO") primaries are thus selected
at E0≃80 TeV, and at E0≃250 TeV, respectively. Their
flux is measured: Jp+He(80 Tev= (1.8±0.4)×10-6 m-2 s-1
sr-1 TeV-1, and Jp+He+CNO(250 TeV)=(1.1±0.3)×10-7 m-2 s-1
sr-1 TeV-1, their relative weights being: Jp+He/Jp+He+CNO
(250 TeV)=0.78±0.17. By using the measurements of the
proton spectrum obtained from the direct experiments and
hadron flux data in the atmosphere, we obtain for the
relative weights of the three components at 250 TeV:
Jp:JHe:JCNO =(0.20±0.08): (0.58±0.19):(0.22±0.17). This
corresponds to the dominance of helium over proton primaries
at 100-1000 TeV, and a possible non-negligible contribution
from CNO.The lateral distribution of Cherenkov light in
Extensive Air Showers (EASs), which is related to the rate
of energy deposit of the primary in the atmosphere, is
measured for a selected proton and helium primary beam, and
good agreement is found when compared with the one
calculated with the CORSIKA/QGSJET simulation model. © 2004
Elsevier B.V. All rights reserved.},
Doi = {10.1016/j.astropartphys.2004.01.005},
Key = {Aglietta:2004ws}
}
@article{Ahn:2004te,
Author = {Ahn, MH and Aoki, S and Ashie, Y and Bhang, H and Boyd, S and Casper, D and Choi, JH and Fukuda, S and Fukuda, Y and Gran, R and Hara, T and Hasegawa,
M and Hasegawa, T and Hayashi, K and Hayato, Y and Hill, J and Ichikawa,
AK and Ikeda, A and Inagaki, T and Ishida, T and Ishii, T and Ishitsuka, M and Itow, Y and Iwashita, T and Jang, HI and Jang, JS and Jeon, EJ and Joo, KK and Jung, CK and Kajita, T and Kameda, J and Kaneyuki, K and Kato, I and Kearns, E and Kibayashi, A and Kielczewska, D and Kim, BJ and Kim, CO and Kim, JY and Kim, SB and Kobayashi, K and Kobayashi, T and Koshio, Y and Kropp, WR and Learned, JG and Lim, SH and Lim, IT and Maesaka, H and Maruyama, T and Matsuno, S and Mauger, C and Mcgrew, C and Minamino, A and Mine, S and Miura, M and Miyano, K and Morita, T and Moriyama, S and Nakahata, M and Nakamura, K and Nakano, I and Nakata, F and Nakaya, T and Nakayama, S and Namba, T and Nambu, R and Nishikawa, K and Nishiyama, S and Noda, S and Obayashi, Y and Okada, A and Oyama, Y and Pac, MY and Park, H and Saji, C and Sakuda, M and Sarrat, A and Sasaki, T and Sasao, N and Scholberg, K and Sekiguchi, M and Sharkey, E and Shiozawa, M and Shiraishi, KK and Smy, M and Sobel, HW and Stone, JL and Suga, Y and Sulak,
LR and Suzuki, A and Suzuki, Y and Takeuchi, Y and Tamura, N and Tanaka, M and Totsuka, Y and Ueda, S and Vagins, MR and Walter, CW and Wang, W and Wilkes, RJ and Yamada, S and Yamamoto, S and Yanagisawa, C and Yokoyama,
H and Yoo, J and Yoshida, M and Zalipska, J and K2K Collaboration},
Title = {Search for electron neutrino appearance in a 250 km
long-baseline experiment.},
Journal = {Physical review letters},
Volume = {93},
Number = {5},
Pages = {051801},
Year = {2004},
Month = {July},
ISSN = {0031-9007},
url = {http://www.ncbi.nlm.nih.gov/pubmed/15323684},
Abstract = {We present a search for electron neutrino appearance from
accelerator-produced muon neutrinos in the K2K long-baseline
neutrino experiment. One candidate event is found in the
data corresponding to an exposure of 4.8 x 10(19) protons on
target. The expected background in the absence of neutrino
oscillations is estimated to be 2.4+/-0.6 events and is
dominated by misidentification of events from neutral
current pi(0) production. We exclude the nu(micro) to nu(e)
oscillations at 90% C.L. for the effective mixing angle in
the 2-flavor approximation of sin((2)2theta(microe)(
approximately 1/2sin((2)2theta(13))>0.15 at
Deltam(2)(microe)=2.8 x 10(-3) eV(2), the best-fit value of
the nu(micro) disappearance analysis in K2K. The most
stringent limit of sin((2)2theta(microe)<0.09 is obtained at
Deltam(2)(microe)=6 x 10(-3) eV(2).},
Doi = {10.1103/physrevlett.93.051801},
Key = {Ahn:2004te}
}
@article{Liu:2004ny,
Author = {Liu, DW and Ashie, Y and Fukuda, S and Fukuda, Y and Ishihara, K and Itow,
Y and Koshio, Y and Minamino, A and Miura, M and Moriyama, S and Nakahata,
M and Namba, T and Nambu, R and Obayashi, Y and Sakurai, N and Shiozawa, M and Suzuki, Y and Takeuchi, H and Takeuchi, Y and Yamada, S and Ishitsuka,
M and Kajita, T and Kaneyuki, K and Nakayama, S and Okada, A and Ooyabu, T and Saji, C and Desai, S and Earl, M and Kearns, E and Messier, MD and Stone,
JL and Sulak, LR and Walter, CW and Wang, W and Barszczak, T and Casper, D and Cravens, JP and Gajewski, W and Kropp, WR and Mine, S and Smy, MB and Sobel, HW and Sterner, CW and Vagins, MR and Ganezer, KS and Hill, J and Keig, WE and Kim, JY and Lim, IT and Ellsworth, RW and Tasaka, S and Kibayashi, A and Learned, JG and Matsuno, S and Takemori, D and Hayato,
Y and Ichikawa, AK and Ishida, T and Ishii, T and Iwashita, T and Kameda,
J and Kobayashi, T and Maruyama, T and Nakamura, K and Nitta, K and Oyama,
Y and Sakuda, M and Totsuka, Y and Suzuki, AT and Hasegawa, M and Hayashi,
K and Inagaki, T and Kato, I and Maesaka, H and Morita, T and Nakaya, T and Nishikawa, K and Sasaki, T and Ueda, S and Yamamoto, S and Haines, TJ and Dazeley, S and Hatakeyama, S and Svoboda, R and Blaufuss, E and Goodman,
JA and Guillian, G and Sullivan, GW and Turcan, D and Scholberg, K and Habig, A and Ackermann, M and Jung, CK and Kato, T and Kobayashi, K and Martens, K and Malek, M and Mauger, C and McGrew, C and Sharkey, E and Viren, B and Yanagisawa, C and Toshito, T and Mitsuda, C and Miyano, K and Shibata, T and Ishii, J and Kajiyama, Y and Kuno, Y and Nagashima, Y and Takita, M and Yoshida, M and Kim, HI and Kim, SB and Yoo, J and Okazawa, H and Ishizuka, T and Choi, Y and Seo, HK and Gando, Y and Hasegawa, T and Inoue,
K and Shirai, J and Suzuki, A and Koshiba, M and Hashimoto, T and Nakajima,
Y and Nishijima, K and Ishino, H and Morii, M and Nishimura, R and Watanabe, Y and Kielczewska, D and Zalipska, J and Gran, R and Shiraishi, KK and Washburn, K and Wilkes, RJ},
Title = {Limits on the neutrino magnetic moment using 1496 days of
Super-Kamiokande-I solar neutrino data.},
Journal = {Physical review letters},
Volume = {93},
Number = {2},
Pages = {021802},
Year = {2004},
Month = {July},
ISSN = {0031-9007},
url = {http://www.ncbi.nlm.nih.gov/pubmed/15323899},
Abstract = {A search for a nonzero neutrino magnetic moment has been
conducted using 1496 live days of solar neutrino data from
Super-Kamiokande-I. Specifically, we searched for
distortions to the energy spectrum of recoil electrons
arising from magnetic scattering due to a nonzero neutrino
magnetic moment. In the absence of a clear signal, we found
micro(nu)</=(3.6x10(-10))micro(B) at 90% C.L. by fitting to
the Super-Kamiokande day-night spectra. The fitting took
into account the effect of neutrino oscillation on the
shapes of energy spectra. With additional information from
other solar neutrino and KamLAND experiments constraining
the oscillation region, a limit of micro(nu)</=(1.1x10(-10))micro(B)
at 90% C.L. was obtained.},
Doi = {10.1103/physrevlett.93.021802},
Key = {Liu:2004ny}
}
@article{Ashie:2004mr,
Author = {Ashie, Y and Hosaka, J and Ishihara, K and Itow, Y and Kameda, J and Koshio, Y and Minamino, A and Mitsuda, C and Miura, M and Moriyama, S and Nakahata, M and Namba, T and Nambu, R and Obayashi, Y and Shiozawa, M and Suzuki, Y and Takeuchi, Y and Taki, K and Yamada, S and Ishitsuka, M and Kajita, T and Kaneyuki, K and Nakayama, S and Okada, A and Okumura, K and Ooyabu, T and Saji, C and Takenaga, Y and Desai, S and Kearns, E and Likhoded, S and Stone, JL and Sulak, LR and Walter, CW and Wang, W and Goldhaber, M and Casper, D and Cravens, JP and Gajewski, W and Kropp,
WR and Liu, DW and Mine, S and Smy, MB and Sobel, HW and Sterner, CW and Vagins, MR and Ganezer, KS and Hill, J and Keig, WE and Jang, JS and Kim,
JY and Lim, IT and Ellsworth, RW and Tasaka, S and Guillian, G and Kibayashi, A and Learned, JG and Matsuno, S and Takemori, D and Messier,
MD and Hayato, Y and Ichikawa, AK and Ishida, T and Ishii, T and Iwashita,
T and Kobayashi, T and Maruyama, T and Nakamura, K and Nitta, K and Oyama,
Y and Sakuda, M and Totsuka, Y and Suzuki, AT and Hasegawa, M and Hayashi,
K and Inagaki, T and Kato, I and Maesaka, H and Morita, T and Nakaya, T and Nishikawa, K and Sasaki, T and Ueda, S and Yamamoto, S and Haines, TJ and Dazeley, S and Hatakeyama, S and Svoboda, R and Blaufuss, E and Goodman,
JA and Sullivan, GW and Turcan, D and Scholberg, K and Habig, A and Fukuda,
Y and Jung, CK and Kato, T and Kobayashi, K and Malek, M and Mauger, C and McGrew, C and Sarrat, A and Sharkey, E and Yanagisawa, C and Toshito, T and Miyano, K and Tamura, N and Ishii, J and Kuno, Y and Nagashima, Y and Takita, M and Yoshida, M and Kim, SB and Yoo, J and Okazawa, H and Ishizuka, T and Choi, Y and Seo, HK and Gando, Y and Hasegawa, T and Inoue,
K and Shirai, J and Suzuki, A and Koshiba, M and Nakajima, Y and Nishijima,
K and Harada, T and Ishino, H and Nishimura, R and Watanabe, Y and Kielczewska, D and Zalipska, J and Berns, HG and Gran, R and Shiraishi,
KK and Stachyra, A and Washburn, K and Wilkes, RJ and Super-Kamiokande
Collaboration},
Title = {Evidence for an oscillatory signature in atmospheric
neutrino oscillations.},
Journal = {Physical review letters},
Volume = {93},
Number = {10},
Pages = {101801},
Year = {2004},
Month = {September},
ISSN = {0031-9007},
url = {http://www.ncbi.nlm.nih.gov/pubmed/15447395},
Abstract = {Muon neutrino disappearance probability as a function of
neutrino flight length L over neutrino energy E was studied.
A dip in the L/E distribution was observed in the data, as
predicted from the sinusoidal flavor transition probability
of neutrino oscillation. The observed L/E distribution
constrained nu(micro)<-->nu(tau) neutrino oscillation
parameters; 1.9x10(-3)<Deltam(2)<3.0x10(-3) eV(2) and
sin((2)2theta>0.90 at 90% confidence level.},
Doi = {10.1103/physrevlett.93.101801},
Key = {Ashie:2004mr}
}
@article{Ambrosio:2004fq,
Author = {Ambrosio, M and Antolini, R and Baldini, A and Barbarino, GC and Barish,
BC and Battistoni, G and Bellotti, R and Bemporad, C and Bernardini, P and Bilokon, H and Bloise, C and Bower, C and Brigida, M and Bussino, S and Cafagna, F and Campana, D and Carboni, M and Cecchini, S and Cei, F and Chiarella, V and Choudhary, BC and Coutu, S and Cozzi, M and de Cataldo,
G and Dekhissi, H and de Marzo, C and de Mitri, I and Derkaoui, J and de
Vincenzi, M and di Credico, A and Favuzzi, C and Forti, C and Fusco, P and Giacomelli, G and Giannini, G and Giglietto, N and Giorgini, M and Grassi, M and Grillo, A and Gustavino, C and Habig, A and Hanson, K and Heinz, R and Iarocci, E and Katsavounidis, E and Katsavounidis, I and Kearns, E and Kim, H and Kyriazopoulou, S and Lamanna, E and Lane, C and Levin, DS and Lipari, P and Longley, NP and Longo, MJ and Loparco, F and Maaroufi, F and Mancarella, G and Mandrioli, G and Margiotta, A and Marini, A and Martello, D and Marzari-Chiesa, A and Mazziotta, MN and Michael, DG and Monacelli, P and Montaruli, T and Monteno, M and Mufson,
S and Musser, J and Nicolò, D and Nolty, R and Orth, C and Osteria, G and Palamara, O and Patera, V and Patrizii, L and Pazzi, R and Peck, CW and Perrone, L and Petrera, S and Popa, V and Rainò, A and Reynoldson, J and Ronga, F and Satriano, C and Scapparone, E and Scholberg, K and Sciubba,
A and Sioli, M and Sirri, G and Sitta, M and Spinelli, P and Spinetti, M and Spurio, M and Steinberg, R and Stone, JL and Sulak, LR and Surdo, A and Tarlè, G},
Title = {Search for stellar gravitational collapses with the MACRO
detector},
Journal = {European Physical Journal C},
Volume = {37},
Number = {3},
Pages = {265-272},
Publisher = {Springer Nature America, Inc},
Year = {2004},
Month = {October},
ISSN = {1434-6044},
url = {http://dx.doi.org/10.1140/epjc/s2004-01981-3},
Abstract = {We present the final results of the search for stellar
gravitational collapses obtained by the MACRO experiment.
The detector was active for a stellar collapse search for
more than 11 years and it was sensitive to collapses
occurring all over in our galaxy for 8.6 years. A real time
system for a prompt recognition of neutrino bursts was
developed and was operating on-line for almost the whole
life of the experiment. No signal compatible with a neutrino
burst from a galactic supernova was observed. ©
Springer-Verlag / Società Italiana di Fisica
2004.},
Doi = {10.1140/epjc/s2004-01981-3},
Key = {Ambrosio:2004fq}
}
@article{fds326728,
Author = {Desai, S and Ashie, Y and Fukuda, S and Fukuda, Y and Ishihara, K and Itow,
Y and Koshio, Y and Minamino, A and Miura, M and Moriyama, S and Nakahata,
M and Namba, T and Nambu, R and Obayashi, Y and Sakurai, N and Shiozawa, M and Suzuki, Y and Takeuchi, H and Takeuchi, Y and Yamada, S and Ishitsuka,
M and Kajita, T and Kaneyuki, K and Nakayama, S and Okada, A and Ooyabu, T and Saji, C and Earl, M and Kearns, E and Stone, JL and Sulak, LR and Walter,
CW and Wang, W and Goldhaber, M and Barszczak, T and Casper, D and Cravens,
JP and Gajewski, W and Kropp, WR and Mine, S and Liu, DW and Smy, MB and Sobel, HW and Sterner, CW and Vagins, MR and Ganezer, KS and Hill, J and Keig, WE and Kim, JY and Lim, IT and Ellsworth, RW and Tasaka, S and Guillian, G and Kibayashi, A and Learned, JG and Matsuno, S and Takemori, D and Messier, MD and Hayato, Y and Ichikawa, AK and Ishida,
T and Ishii, T and Iwashita, T and Kameda, J and Kobayashi, T and Maruyama,
T and Nakamura, K and Nitta, K and Oyama, Y and Sakuda, M and Totsuka, Y and Suzuki, AT and Hasegawa, M and Hayashi, K and Inagaki, T and Kato, I and Maesaka, H and Morita, T and Nakaya, T and Nishikawa, K and Sasaki, T and Ueda, S and Yamamoto, S and Haines, TJ and Dazeley, S and Hatakeyama, S and Svoboda, R and Blaufuss, E and Goodman, JA and Sullivan, GW and Turcan,
D and Scholberg, K and Habig, A and Jung, CK and Kato, T and Kobayashi, K and Malek, M and Mauger, C and McGrew, C and Sarrat, A and Sharkey, E and Yanagisawa, C and Toshito, T and Mitsuda, C and Miyano, K and Shibata,
T and Kajiyama, Y and Nagashima, Y and Takita, M and Yoshida, M and Kim,
HI and Kim, SB and Yoo, J and Okazawa, H and Ishizuka, T and Choi, Y and Seo,
HK and Gando, Y and Hasegawa, T and Inoue, K and Shirai, J and Suzuki, A and Koshiba, M and Hashimoto, T and Nakajima, Y and Nishijima, K and Harada,
T and Ishino, H and Morii, M and Nishimura, R and Watanabe, Y and Kielczewska, D and Zalipska, J and Gran, R and Shiraishi, KK and Washburn, K and Wilkes, RJ},
Title = {Publisher's Note: Search for dark matter WIMPs using upward
through-going muons in Super-Kamiokande [Phys. Rev.
D70, 083523 (2004)]},
Journal = {Physical Review D},
Volume = {70},
Number = {10},
Publisher = {American Physical Society (APS)},
Year = {2004},
Month = {November},
url = {http://dx.doi.org/10.1103/physrevd.70.109901},
Doi = {10.1103/physrevd.70.109901},
Key = {fds326728}
}
@article{Ambrosio:2004ig,
Author = {Ambrosio, M and Antolini, R and Bakari, D and Baldini, A and Barbarino,
GC and Barish, BC and Battistoni, G and Becherini, Y and Bellotti, R and Bemporad, C and Bernardini, P and Bilokon, H and Bloise, C and Bower, C and Brigida, M and Cafagna, F and Campana, D and Carboni, M and Cecchini, S and Cei, F and Chiarella, V and Choudhary, BC and Cosson, D and Coutu, S and de
Cataldo, G and Dekhissi, H and de Marzo, C and de Mitri, I and Denni, U and Derkauoi, J and de Vincenzi, M and di Credico, A and Favuzzi, C and Forti, C and Frani, A and Fusco, P and Giacomelli, G and Giannini, G and Giglietto, N and Giorgini, M and Grassi, M and Grillo, A and Guarino, F and Gustavino, C and Habig, A and Hanson, K and Heinz, R and Iarocci, E and Katsavounidis, E and Katsavounidis, I and Kearns, E and Kim, H and Kyriazopoulou, S and Lamanna, E and Lane, C and Levin, DS and Lipari, P and Longo, MJ and Loparco, F and Maaroufi, F and Mancarella, G and Mandrioli, G and Manzoor, S and Margiotta, A and Marini, A and Martello,
D and Marzari-Chiesa, A and Mazziotta, MN and Mengucci, A and Michael,
DG and Mikheyev, S and Monacelli, P and Montaruli, T and Monteno, M and Mufson, S and Musser, J and Nicolò, D and Nolty, R and Orth, C and Osteria, G and Palamara, O and Patera, V and Patrizii, L and Pazzi, R and Peck, CW and Perrone, L and Petrera, S and Popa, V and Rainò, A and Reynoldson, J and Ronga, F and Satriano, C and Scholberg, K and Sciubba,
A and Sioli, M and Sitta, M and Spinelli, P and Spinetti, M and Spurio, M and Steinberg, R},
Title = {Measurements of atmospheric muon neutrino oscillations,
global analysis of the data collected with MACRO
detector},
Journal = {European Physical Journal C},
Volume = {36},
Number = {3},
Pages = {323-339},
Publisher = {Springer Nature},
Year = {2004},
Month = {December},
ISSN = {1434-6044},
url = {http://dx.doi.org/10.1140/epjc/s2004-01951-9},
Abstract = {The final analysis of atmospheric neutrino events collected
with the MACRO detector is presented. Three different
classes of events, generated by neutrinos in different
energy ranges, are studied looking at rates, angular
distributions and estimated energies. The results are
consistent for all the subsamples and indicate a flux
deficit that depends on energy and path-length of neutrinos.
The no-oscillation hypothesis is excluded at ∼ 5σ, while
the hypothesis of vμ → vτ oscillation gives a
satisfactory description of all data. The parameters with
highest probability in a two flavor scenario are sin2 2θm =
1 and Δm2 = 0.0023 eV2. This result is independent of the
absolute normalization of the atmospheric neutrino fluxes.
The data can also be used to put experimental constrain on
this normalization. © Springer-Verlag / Società Italiana
di Fisica 2004.},
Doi = {10.1140/epjc/s2004-01951-9},
Key = {Ambrosio:2004ig}
}
@article{fds248786,
Author = {Ashie, and Y, and others},
Title = {A measurement of atmospheric neutrino oscillation parameters
by Super-Kamiokande I},
Journal = {Phys. Rev.},
Volume = {D71},
Number = {11},
Pages = {112005},
Publisher = {American Physical Society (APS)},
Year = {2005},
url = {http://dx.doi.org/10.1103/PhysRevD.71.112005},
Abstract = {We present a combined analysis of fully-contained,
partially-contained and upward-going muon atmospheric
neutrino data from a 1489d exposure of the Super-Kamiokande
detector. The data samples span roughly five decades in
neutrino energy, from 100MeV to 10eV. A detailed Monte Carlo
comparison is described and presented. The data is fit to
the Monte Carlo expectation, and is found to be consistent
with neutrino oscillations of νμντ with sin22θ>0.92 and
1.5×10-3<Δm2<3.4×10-3eV2 at 90% confidence level. © 2005
The American Physical Society.},
Doi = {10.1103/PhysRevD.71.112005},
Key = {fds248786}
}
@article{Kobayashi:2005pe,
Author = {Kobayashi, and K, and others},
Title = {Search for nucleon decay via modes favored by supersymmetric
grand unification models in Super-Kamiokande-I},
Journal = {Phys.Rev.},
Volume = {D72},
Number = {5},
Pages = {052007},
Publisher = {American Physical Society (APS)},
Year = {2005},
ISSN = {1550-7998},
url = {http://arxiv.org/pdf/hep-ex/0502026},
Abstract = {We report the results for nucleon decay searches via modes
favored by supersymmetric grand unified models in
Super-Kamiokande. Using 1489 days of full Super-Kamiokande-I
data, we searched for p→ν̄K+, n→ν̄K0, p→μ+K0, and
p→e+K0 modes. We found no evidence for nucleon decay in
any of these modes. We set lower limits of partial nucleon
lifetime 2.3×1033, 1.3×1032, 1.3×1033, and 1.0×1033years
at 90% confidence level for p→ν̄K+, n→ν̄K0,
p→μ+K0, and p→e+K0 modes, respectively. These results
give a strong constraint on supersymmetric grand unification
models. © 2005 The American Physical Society.},
Doi = {10.1103/PhysRevD.72.052007},
Key = {Kobayashi:2005pe}
}
@article{Aliu:2004sq,
Author = {Aliu, and E, and others},
Title = {Evidence for muon neutrino oscillation in an
accelerator-based experiment},
Journal = {Phys. Rev. Lett.},
Volume = {94},
Number = {8},
Pages = {081802},
Year = {2005},
ISSN = {0031-9007},
url = {http://www.ncbi.nlm.nih.gov/pubmed/15783876},
Abstract = {We present results for nu(mu) oscillation in the KEK to
Kamioka (K2K) long-baseline neutrino oscillation experiment.
K2K uses an accelerator-produced nu(mu) beam with a mean
energy of 1.3 GeV directed at the Super-Kamiokande detector.
We observed the energy-dependent disappearance of nu(mu),
which we presume have oscillated to nu(tau). The probability
that we would observe these results if there is no neutrino
oscillation is 0.0050% (4.0 sigma).},
Doi = {10.1103/physrevlett.94.081802},
Key = {Aliu:2004sq}
}
@article{Nakayama:2004dp,
Author = {Nakayama, and S, and others},
Title = {Measurement of single pi0 production in neutral current
neutrino interactions with water by a 1.3-GeV wide band muon
neutrino beam},
Journal = {Phys. Lettl},
Volume = {B619},
Number = {3-4},
Pages = {255-262},
Publisher = {Elsevier BV},
Year = {2005},
url = {http://arxiv.org/pdf/hep-ex/0408134},
Abstract = {http://arxiv.org/abs/hep-ex/0408134},
Doi = {10.1016/j.physletb.2005.05.044},
Key = {Nakayama:2004dp}
}
@article{fds318498,
Author = {Yoshizawa, T and Sakuda, M and Nakano, I and Iwashita, H and Keppel, C and Walter, C and Gran, R and JLAB, E-C},
Title = {26pZB-2 Measurement of electron-nucleous quasi-elastic cross
section and N^*(1232) production cross section using 1GeV
electron beam.},
Journal = {Meeting abstracts of the Physical Society of
Japan},
Volume = {60},
Number = {1},
Pages = {30 pages},
Publisher = {The Physical Society of Japan (JPS)},
Year = {2005},
Month = {March},
Key = {fds318498}
}
@article{fds248703,
Author = {Cravens, P and Hosaka, J and Ishihara, K and Kameda, J and Koshio, Y and Minamino, A and Mitsuda, G and Miura, M and Moriyama, S and Nakahata, M and Namba, T and Obayashi, Y and Shiozawa, M and Suzuki, Y and Takeda, A and Takeuchi, Y and Yamada, S and Higuchi, I and Ishitsuka, M and Kajita, T and Kaneyuki, K and Mitsuka, G and Nakayama, S and Nishino, H and Okada, A and Okumura, K and Saji, C and Takenaga, Y and Clark, S and Desai, S and Kearns, E and Likhoded, S and Stone, JL and Sulak, LR and Wang, W and Goldhaber, M and Casper, D and Cravens, JP and Kropp, WR and Liu, DW and Mine, S and Regis, C and Smy, MB and Sobel, HW and Sterner, CW and Vagins,
MR and Ganezer, KS and Hill, JE and Keig, WE and Jang, JS and Kim, JY and Lim,
IT and Scholberg, K and Walter, CW and Wendell, R and Ellsworth, RW and Tasaka, S and Guillian, E and Kibayashi, A and Learned, JG and Matsuno,
S and Messier, MD and Hayato, Y and Ichikawa, AK and Ishida, T and Ishii,
T and Iwashita, T and Kobayasln, T and Nakadaira, T and Nakamura, K and Nitta, K and Oyama, Y and Totsuka, Y and Suzuki, AT and Hasegawa, M and Kato, I and Maesaka, H and Nakaya, T and Nishikawa, K and Sasaki, T and Sato, H and Yamamoto, S and Yokoyama, M and Haines, TJ and Dazeley, S and Hatakeyama, S and Svoboda, R and Blaufuss, E and Goodman, JA and Sullivan, GW and Turcan, D and Cooley, J and Habig, A and Fukuda, Y and Sato, T and Itow, Y and Jung, CK and Kato, T and Kobayashi, K and Malek, M and Mauger, C and McGrew, C and Sarrat, A and Yanagisawa, C and Tamura, N and Sakuda, M and Kuno, Y and Yoshida, M and Kim, SB and Yoo, J and Ishizuka,
T and Okazawa, H and Choi, Y and Seo, HK and Gando, Y and Hasegawa, T and Inoue, K and Shirai, J and Suzuki, A and Nishijima, K and Ishino, H and Watanabe, Y and Koshiba, M and Kielezewska, D and Zalipska, J and Berns,
HG and Gran, R and Shiraishi, KK and Stachyra, A and Washburn, K and Wilkes, RJ},
Title = {Current status of solar neutrinos at super-kamiokande},
Journal = {Annual Meeting of the Division of Particles and Fields of
the American Physical Society, DPF 2006, and the Annual Fall
Meeting of the Japan Particle Physics Community},
Publisher = {American Physical Society},
Year = {2006},
Abstract = {• SK-III has been started and is taking data • SK-II
data has been updated to its final 791d • Oscillation
analysis with SK-I, SK-II data has been performed and shows
consistency with final SK-I data set • SK-II shows
consistency within the global analysis • Hope to see
energy spectrum distortion in SK-III.},
Key = {fds248703}
}
@article{Swanson:2006gm,
Author = {Swanson, and C, ME and others},
Title = {Search for diffuse astrophysical neutrino flux using
ultra-high energy upward-going muons in Super-Kamiokande
I},
Journal = {Astrophys. J.},
Volume = {652},
Number = {1 I},
Pages = {206},
Publisher = {IOP Publishing},
Year = {2006},
ISSN = {0004-637X},
url = {http://arxiv.org/pdf/astro-ph/0606126},
Abstract = {http://arxiv.org/abs/astro-ph/0606126},
Doi = {10.1086/507983},
Key = {Swanson:2006gm}
}
@article{Hosaka:2006zd,
Author = {Hosaka, and J, and others},
Title = {Three flavor neutrino oscillation analysis of atmospheric
neutrinos in Super-Kamiokande},
Journal = {Phys. Rev.},
Volume = {D74},
Number = {3},
Pages = {032002},
Publisher = {American Physical Society (APS)},
Year = {2006},
ISSN = {1550-7998},
url = {http://arxiv.org/pdf/hep-ex/0604011},
Abstract = {http://arxiv.org/abs/hep-ex/0604011},
Doi = {10.1103/PhysRevD.74.032002},
Key = {Hosaka:2006zd}
}
@article{Abe:2006at,
Author = {Abe, and K, and others},
Title = {High energy neutrino astronomy using upward-going muons in
Super-Kamiokande-I},
Journal = {Astrophys. J.},
Volume = {652},
Number = {1 I},
Pages = {198},
Publisher = {IOP Publishing},
Year = {2006},
ISSN = {0004-637X},
url = {http://arxiv.org/pdf/astro-ph/0606413},
Abstract = {http://arxiv.org/abs/astro-ph/0606413},
Doi = {10.1086/508016},
Key = {Abe:2006at}
}
@article{Abe:2006fu,
Author = {Abe, and K, and others},
Title = {A measurement of atmospheric neutrino flux consistent with
tau neutrino appearance},
Journal = {Phys. Rev. Lett.},
Volume = {97},
Number = {17},
Pages = {171801},
Year = {2006},
ISSN = {0031-9007},
url = {http://www.ncbi.nlm.nih.gov/pubmed/17155460},
Abstract = {http://arxiv.org/abs/hep-ex/0607059},
Doi = {10.1103/physrevlett.97.171801},
Key = {Abe:2006fu}
}
@article{Hasegawa:2005td,
Author = {Hasegawa, and M, and others},
Title = {Search for coherent charged pion production in neutrino
carbon interactions},
Journal = {Phys. Rev. Lett.},
Volume = {95},
Number = {25},
Pages = {252301},
Year = {2006},
ISSN = {0031-9007},
url = {http://www.ncbi.nlm.nih.gov/pubmed/16384451},
Abstract = {http://arxiv.org/pdf/hep-ex/0506008},
Doi = {10.1103/physrevlett.95.252301},
Key = {Hasegawa:2005td}
}
@article{:2008zn,
Author = {Hosaka, and J, and others},
Title = {Solar neutrino measurements in Super-Kamiokande-I},
Journal = {Phys. Rev.},
Volume = {D83},
Number = {3},
Pages = {112001},
Publisher = {American Physical Society (APS)},
Year = {2006},
ISSN = {1550-7998},
url = {http://arxiv.org/pdf/0803.4312},
Abstract = {The results of the second phase of the Super-Kamiokande
solar neutrino measurement are presented and compared to the
first phase. The solar neutrino flux spectrum and time
variation as well as oscillation results are statistically
consistent with the first phase and do not show spectral
distortion. The time-dependent flux measurement of the
combined first and second phases coincides with the full
period of solar cycle 23 and shows no correlation with solar
activity. The measured B8 total flux is (2.38±0.05(stat.)-0.15+0.16(sys.))×106cm-2s-1
and the day-night difference is found to be
(-6.3±4.2(stat.)±3.7(sys.))%. There is no evidence of
systematic tendencies between the first and second phases.
© 2008 The American Physical Society.},
Doi = {10.1103/PhysRevD.78.032002},
Key = {:2008zn}
}
@article{fds376418,
Author = {Cravens, P and Hosaka, J and Ishihara, K and Kameda, J and Koshio, Y and Minamino, A and Mitsuda, G and Miura, M and Moriyama, S and Nakahata, M and Namba, T and Obayashi, Y and Shiozawa, M and Suzuki, Y and Takeda, A and Takeuchi, Y and Yamada, S and Higuchi, I and Ishitsuka, M and Kajita, T and Kaneyuki, K and Mitsuka, G and Nakayama, S and Nishino, H and Okada, A and Okumura, K and Saji, C and Takenaga, Y and Clark, S and Desai, S and Kearns, E and Likhoded, S and Stone, JL and Sulak, LR and Wang, W and Goldhaber, M and Casper, D and Cravens, JP and Kropp, WR and Liu, DW and Mine, S and Regis, C and Smy, MB and Sobel, HW and Sterner, CW and Vagins,
MR and Ganezer, KS and Hill, JE and Keig, WE and Jang, JS and Kim, JY and Lim,
IT and Scholberg, K and Walter, CW and Wendell, R and Ellsworth, RW and Tasaka, S and Guillian, E and Kibayashi, A and Learned, JG and Matsuno,
S and Messier, MD and Hayato, Y and Ichikawa, AK and Ishida, T and Ishii,
T and Iwashita, T and Kobayasln, T and Nakadaira, T and Nakamura, K and Nitta, K and Oyama, Y and Totsuka, Y and Suzuki, AT and Hasegawa, M and Kato, I and Maesaka, H and Nakaya, T and Nishikawa, K and Sasaki, T and Sato, H and Yamamoto, S and Yokoyama, M and Haines, TJ and Dazeley, S and Hatakeyama, S and Svoboda, R and Blaufuss, E and Goodman, JA and Sullivan, GW and Turcan, D and Cooley, J and Habig, A and Fukuda, Y and Sato, T and Itow, Y and Jung, CK and Kato, T and Kobayashi, K and Malek,
M},
Title = {Current status of solar neutrinos at super-kamiokande},
Journal = {Annual Meeting of the Division of Particles and Fields of
the American Physical Society, DPF 2006, and the Annual Fall
Meeting of the Japan Particle Physics Community},
Year = {2006},
Month = {January},
Abstract = {• SK-III has been started and is taking data • SK-II
data has been updated to its final 791d • Oscillation
analysis with SK-I, SK-II data has been performed and shows
consistency with final SK-I data set • SK-II shows
consistency within the global analysis • Hope to see
energy spectrum distortion in SK-III.},
Key = {fds376418}
}
@article{fds304630,
Author = {Yamamoto, S and Zalipska, J and Aliu, E and Andringa, S and Aoki, S and Argyriades, J and Asakura, K and Ashie, R and Berghaus, F and Berns, H and Bhang, H and Blondel, A and Borghi, S and Bouchez, J and Burguet-Castell, J and Casper, D and Catala, J and Cavata, C and Cervera, A and Chen, SM and Cho, KO and Choi, JH and Dore, U and Espinal,
X and Fechner, M and Fernandez, E and Fukuda, Y and Gomez-Cadenas, J and Gran, R and Hara, T and Hasegawa, M and Hasegawa, T and Hayashi, K and Hayato, Y and Helmer, RL and Hiraide, K and Hosaka, J and Ichikawa, AK and Iinuma, M and Ikeda, A and Inagaki, T and Ishida, T and Ishihara, K and Ishii, T and Ishitsuka, M and Itow, Y and Iwashita, T and Jang, HI and Jeon, EJ and Jeong, IS and Joo, KK and Jover, G and Jung, CK and Kajita, T and Kameda, J and Kaneyuki, K and Kato, I and Kearns, E and Kerr, D and Kim,
CO and Khabibullin, M and Khotjantsev, A and Kielczewska, D and Kim, JY and Kim, SB and Kitching, P and Kobayashi, K and Kobayashi, T and Konaka, A and Koshio, Y and Kropp, W and Kubota, J and Kudenko, Y and Kuno, Y and Kurimoto, Y and Kutter, T and Learned, J and Likhoded, S and Lim, IT and Loverre, PF and Ludovici, L and Maesaka, H and Mallet, J and Mariani, C and Matsuno, S and Matveev, V and McConnel, K and McGrew, C and Mikheyev, S and Minamino, A and Mine, S and Mineev, O and Mitsuda, C and Miura, M and Moriguchi, Y and Morita, T and Moriyama, S and Nakadaira, T and Nakahata, M and Nakamura, K and Nakano, I and Nakaya, T and Nakayama, S and Namba, T and Nambu, R and Nawang, S and Nishikawa, K and Nitta, K and Nova,
F and Novella, P and Obayashi, Y and Okada, A and Okumura, K and Oser, SM and Oyama, Y and Pac, MY and Pierre, F and Rodriguez, A and Saji, C and Sakuda,
M and Sanchez, F and Sarrat, A and Sasaki, T and Sato, H and Scholberg, K and Schroeter, R and Sekiguchi, M and Shiozawa, M and Shiraishi, K and Sitjes, G and Smy, M and Sobel, H and Sorel, M and Stone, J and Sulak, L and Suzuki, A and Suzuki, Y and Takahashi, T and Takenaga, Y and Takeuchi,
Y and Taki, K and Takubo, Y and Tamura, N and Tanaka, M and Terri, R and T'jampens, S and Tornero-Lopez, A and Totsuka, Y and Ueda, S and Vagins,
M and Whitehead, L and Walter, CW and Wang, W and Wilkes, RJ and Yamada, S and Yanagisawa, C and Yershov, N and Yokoyama, H and Yokoyama, M and Yoo, J and Yoshida, M and K2K Collaboration},
Title = {Improved search for nu(mu) --> nu(e) oscillation in a
long-baseline accelerator experiment.},
Journal = {Physical review letters},
Volume = {96},
Number = {18},
Pages = {181801},
Year = {2006},
Month = {May},
ISSN = {0031-9007},
url = {http://www.ncbi.nlm.nih.gov/pubmed/16712358},
Abstract = {We performed an improved search for nu(mu) --> nu(e)
oscillation with the KEK to Kamioka (K2K) long-baseline
neutrino oscillation experiment, using the full data sample
of 9.2 x 10(19) protons on target. No evidence for a nu(e)
appearance signal was found, and we set bounds on the nu(mu)
--> nu(e) oscillation parameters. At Deltam(2)=2.8 x 10(-3)
eV(2), the best-fit value of the K2Knu(mu) disappearance
analysis, we set an upper limit of sin(2)2theta(mue) < 0.13
at a 90% confidence level.},
Doi = {10.1103/physrevlett.96.181801},
Key = {fds304630}
}
@article{fds287698,
Author = {Gran, R and Jeon, EJ and Aliu, E and Andringa, S and Aoki, S and Argyriades, J and Asakura, K and Ashie, R and Berghaus, F and Berns, H and Bhang, H and Blondel, A and Borghi, S and Bouchez, J and Burguet-Castell, J and Casper, D and Catala, J and Cavata, C and Cervera, A and Chen, SM and Cho, KO and Choi, JH and Dore, U and Espinal,
X and Fechner, M and Fernandez, E and Fukuda, Y and Gomez-Cadenas, J and Hara, T and Hasegawa, M and Hasegawa, T and Hayashi, K and Hayato, Y and Helmer, RL and Hiraide, K and Hosaka, J and Ichikawa, AK and Iinuma, M and Ikeda, A and Inagaki, T and Ishida, T and Ishihara, K and Ishii, T and Ishitsuka, M and Itow, Y and Iwashita, T and Jang, HI and Jeong, IS and Joo, KK and Jover, G and Jung, CK and Kajita, T and Kameda, J and Kaneyuki,
K and Kato, I and Kearns, E and Kerr, D and Kim, CO and Khabibullin, M and Khotjantsev, A and Kielczewska, D and Kim, JY and Kim, SB and Kitching,
P and Kobayashi, K and Kobayashi, T and Konaka, A and Koshio, Y and Kropp,
W and Kubota, J and Kudenko, Y and Kuno, Y and Kurimoto, Y and Kutter, T and Learned, J and Likhoded, S and Lim, IT and Loverre, PF and Ludovici, L and Maesaka, H and Mallet, J and Mariani, C and Matsuno, S and Matveev, V and McConnel Mahn and KB and McGrew, C and Mikheyev, S and Minamino, A and Mine, S and Mineev, O and Mitsuda, C and Miura, M and Moriguchi, Y and Morita, T and Moriyama, S and Nakadaira, T and Nakahata, M and Nakamura,
K and Nakano, I and Nakaya, T},
Title = {Measurement of the quasielastic axial vector mass in
neutrino interactions on oxygen},
Journal = {Physical Review D - Particles, Fields, Gravitation and
Cosmology},
Volume = {74},
Number = {5},
Publisher = {American Physical Society (APS)},
Year = {2006},
Month = {September},
ISSN = {1550-7998},
url = {http://dx.doi.org/10.1103/PhysRevD.74.052002},
Abstract = {The weak nucleon axial-vector form factor for quasielastic
interactions is determined using neutrino interaction data
from the K2K Scintillating Fiber detector in the neutrino
beam at KEK. More than 12000 events are analyzed, of which
half are charged-current quasielastic interactions
νμn→μ-p occurring primarily in oxygen nuclei. We use a
relativistic Fermi gas model for oxygen and assume the form
factor is approximately a dipole with one parameter, the
axial-vector mass MA, and fit to the shape of the
distribution of the square of the momentum transfer from the
nucleon to the nucleus. Our best fit result for
MA=1.20±0.12GeV. Furthermore, this analysis includes
updated vector form factors from recent electron scattering
experiments and a discussion of the effects of the nucleon
momentum on the shape of the fitted distributions. © 2006
The American Physical Society.},
Doi = {10.1103/PhysRevD.74.052002},
Key = {fds287698}
}
@article{Ahn:2006zz,
Author = {Ahn, MH and Aliu, E and Andringa, S and Aoki, S and Aoyama, Y and Argyriades, J and Asakura, K and Ashie, R and Berghaus, F and Berns, HG and Bhang, H and Blondel, A and Borghi, S and Bouchez, J and Boyd, SC and Burguet-Castell, J and Casper, D and Catala, J and Cavata, C and Cervera, A and Chen, SM and Cho, KO and Choi, JH and Dore, U and Echigo, S and Espinal, X and Fechner, M and Fernandez, E and Fujii, K and Fujii, Y and Fukuda, S and Fukuda, Y and Gomez-Cadenas, J and Gran, R and Hara, T and Hasegawa, M and Hasegawa, T and Hayashi, K and Hayato, Y and Helmer, RL and Higuchi, I and Hill, J and Hiraide, K and Hirose, E and Hosaka, J and Ichikawa, AK and Ieiri, M and Iinuma, M and Ikeda, A and Inagaki, T and Ishida, T and Ishihara, K and Ishii, H and Ishii, T and Ishino, H and Ishitsuka, M and Itow, Y and Iwashita, T and Jang, HI and Jang, JS and Jeon, EJ and Jeong, IS and Joo, KK and Jover, G and Jung, CK and Kajita, T and Kameda, J and Kaneyuki, K and Kang, BH and Kato, I and Kato, Y and Kearns,
E and Kerr, D and Kim, CO and Khabibullin, M and Khotjantsev, A and Kielczewska, D and Kim, BJ and Kim, HI and Kim, JH and Kim, JY and Kim, SB and Kitamura, M and Kitching, P and Kobayashi, K and Kobayashi, T and Kohama, M and Konaka, A and Koshio, Y and Kropp, W and Kubota, J and Kudenko, Y and Kume, G and Kuno, Y and Kurimoto, Y and Kutter, T and Learned, J and Likhoded, S and Lim, IT and Lim, SH},
Title = {Measurement of neutrino oscillation by the K2K
experiment},
Journal = {Physical Review D - Particles, Fields, Gravitation and
Cosmology},
Volume = {74},
Number = {7},
Pages = {072003},
Publisher = {American Physical Society (APS)},
Year = {2006},
Month = {October},
ISSN = {1550-7998},
url = {http://arxiv.org/pdf/hep-ex/0606032},
Abstract = {We present measurements of νμ disappearance in K2K, the
KEK to Kamioka long-baseline neutrino oscillation
experiment. One-hundred and twelve beam-originated neutrino
events are observed in the fiducial volume of
Super-Kamiokande with an expectation of 158.1-8.6+9.2 events
without oscillation. A distortion of the energy spectrum is
also seen in 58 single-ring muonlike events with
reconstructed energies. The probability that the
observations are explained by the expectation for no
neutrino oscillation is 0.0015% (4.3σ). In a two-flavor
oscillation scenario, the allowed Δm2 region at sin 22θ=1
is between 1.9 and 3.5×10-3eV2 at the 90% C.L. with a
best-fit value of 2.8×10-3eV2. © 2006 The American
Physical Society.},
Doi = {10.1103/PhysRevD.74.072003},
Key = {Ahn:2006zz}
}
@article{Takenaga:2006nr,
Author = {Takenaga, and Y, and others},
Title = {Search for neutral Q-balls in Super-Kamiokande
II},
Journal = {Phys. Lett. B},
Volume = {647},
Number = {1},
Pages = {18-22},
Publisher = {Elsevier BV},
Year = {2007},
ISSN = {0370-2693},
url = {http://arxiv.org/pdf/hep-ex/0608057},
Abstract = {http://arxiv.org/abs/hep-ex/0608057},
Doi = {10.1016/j.physletb.2007.01.047},
Key = {Takenaga:2006nr}
}
@article{Ikeda:2007sa,
Author = {Ikeda, M and others},
Title = {Search for Supernova Neutrino Bursts at Super-Kamiokande},
Journal = {Astrophys. J.},
Volume = {669},
Number = {1},
Pages = {519},
Publisher = {IOP Publishing},
Year = {2007},
ISSN = {0004-637X},
url = {http://arxiv.org/pdf/arXiv:0706.2283 [astro-ph]},
Abstract = {We report the results of a search for neutrino bursts from
supernova explosions using the Super-Kamiokande detector.
Super-Kamiokande is sensitive to core-collapse supernova
explosions via observation of their neutrino emissions. The
expected number of events comprising such a burst is ∼104,
and the average energy of the neutrinos is in the range of a
few tens of MeV for a core-collapse supernova explosion at a
typical distance in our galaxy (10 kpc); this strong signal
means that the detection efficiency anywhere within our
galaxy and well past the Magellanic Clouds should be 100%.
We examined a data set taken from 1996 May to 2001 July, and
from 2002 December to 2005 October, corresponding to 2589.2
live days. However, there is no evidence of such a supernova
explosion during the data-taking period. The 90% CL. upper
limit on the rate of core-collapse supernova explosions out
to distances of 100 kpc is found to be 0.32 SN yr-1. ©
2007. The American Astronomical Society. All rights
reserved.},
Doi = {10.1086/521547},
Key = {Ikeda:2007sa}
}
@article{fds248743,
Author = {Guillian, G and Hosaka, J and Ishihara, K and Kameda, J and Koshio, Y and Minamino, A and Mitsuda, C and Miura, M and Moriyama, S and Nakahata, M and Namba, T and Obayashi, Y and Ogawa, H and Shiozawa, M and Suzuki, Y and Takeda, A and Takeuchi, Y and Yamada, S and Higuchi, I and Ishitsuka, M and Kajita, T and Kaneyuki, K and Mitsuka, G and Nakayama, S and Nishino, H and Okada, A and Okumura, K and Saji, C and Takenaga, Y and Desai, S and Kearns, E and Stone, JL and Sulak, LR and Wang, W and Goldhaber, M and Casper, D and Gajewski, W and Griskevich, J and Kropp, WR and Liu, DW and Mine, S and Smy, MB and Sobel, HW and Vagins, MR and Ganezer, KS and Hill,
J and Keig, WE and Scholberg, K and Walter, CW and Ellsworth, RW and Tasaka, S and Kibayashi, A and Learned, JG and Matsuno, S and Messier,
MD and Hayato, Y and Ichikawa, AK and Ishida, T and Ishii, T and Iwashita,
T and Kobayashi, T and Nakadaira, T and Nakamura, K and Nitta, K and Oyama,
Y and Totsuka, Y and Suzuki, AT and Hasegawa, M and Kato, I and Maesaka, H and Nakaya, T and Nishikawa, K and Sato, H and Yamamoto, S and Yokoyama, M and Haines, TJ and Dazeley, S and Hatakeyama, S and Svoboda, R and Blaufuss,
E and Goodman, JA and Sullivan, GW and Turcan, D and Habig, A and Fukuda,
Y and Itow, Y and Sakuda, M and Yoshida, M and Kim, SB and Yoo, J and Okazawa,
H and Ishizuka, T and Jung, CK and Kato, T and Kobayashi, K and Malek, M and Mauger, C and McGrew, C and Sharkey, E and Yanagisawa,
C},
Title = {Observation of the anisotropy of 10 TeV primary cosmic ray
nuclei flux with the Super-Kamiokande-I detector},
Journal = {Physical Review D - Particles, Fields, Gravitation and
Cosmology},
Volume = {75},
Number = {6},
Pages = {17 pages},
Publisher = {AMERICAN PHYSICAL SOC},
Year = {2007},
Month = {March},
ISSN = {1550-7998},
url = {http://dx.doi.org/10.1103/PhysRevD.75.062003},
Abstract = {The relative sidereal variation in the arrival direction of
primary cosmic ray nuclei of median energy 10 TeV was
measured using downward, through-going muons detected with
the Super-Kamiokande-I detector. The projection of the
anisotropy map onto the right ascension axis has a first
harmonic amplitude of (6.64±0.98stat±0.55syst)×10-4 and a
phase at maximum at (33.2°±8.2°stat±5.1°syst) right
ascension. A sky map in equatorial coordinates indicates an
excess region in the constellation of Taurus and a deficit
region toward Virgo. The excess region is centered at
(αT,δT)=(75°±7°,-5°±9°) with a half-opening angle
χT=(39±7)°; the excess flux is (0.104±0.020)% above the
isotropic expectation. The corresponding parameters for the
deficit region are (αV,δV)= (205°±7°,5°±10°),
χV=(54±7)°, and (-0.094±0.014)%. The data do not allow
us to rule out a pure dipole form for the anisotropy
(allowed at 13% confidence level); they are better described
by the excess and deficit cones described above. We explored
the implications under the assumption that the true
anisotropy is not distorted too much by the analysis filter
so that it is well-described by the observed excess and
deficit cones. © 2007 The American Physical
Society.},
Doi = {10.1103/PhysRevD.75.062003},
Key = {fds248743}
}
@article{fds330715,
Author = {Durand, G and Cadelis, L and Minier, V and Veyssière, C and Walter, C and Pierre, A and Agabi, A and Fossat, E and Jeanneaux,
F},
Title = {GIVRE: A protection againt frost deposit on polar
instruments},
Journal = {EAS Publications Series},
Volume = {25},
Pages = {77-80},
Publisher = {E D P SCIENCES},
Year = {2007},
Month = {August},
url = {http://dx.doi.org/10.1051/eas:2007076},
Abstract = {The CEA, in coordination with IPEV and LUAN, will prepare an
experiment to study frost formation on surfaces in radiative
cooling in the winter. This experiment has been shipped to
be installed at Concordia before the 2007 winter period. It
will be controlled from Concordia winterover personal,
through PC server that will locally archive data from
WEBcams and several local heat regulators. This experiment
will be used to give recipes on the way to compensate with
heaters the radiative cooling from the sky and maintain
instrument surfaces at temperature just above icing
conditions. The individual regulators proposed in this
experiment will be usable as standalone ice protection
systems for existing and future telescopes. © EAS, EDP
Sciences 2007.},
Doi = {10.1051/eas:2007076},
Key = {fds330715}
}
@inproceedings{Walter:2007wf,
Author = {Walter, CW},
Title = {Why understanding neutrino interactions is important for
oscillation physics},
Journal = {AIP Conference Proceedings},
Volume = {967},
Pages = {3-8},
Booktitle = {Proceedings of 5th International Workshop on
Neutrino-Nucleus Interactions in the Few-GeV Region
(NuInt07)},
Publisher = {AIP},
Year = {2007},
Month = {December},
ISSN = {0094-243X},
url = {http://arxiv.org/pdf/arXiv:0709.3616 [hep-ex]},
Abstract = {Uncertainties in knowledge of neutrino interactions directly
impact the ability measure the parameters of neutrino
oscillation. Experiments which make use of differing
technologies and neutrino beams are sensitive to different
uncertainties. © 2007 American Institute of
Physics.},
Doi = {10.1063/1.2834507},
Key = {Walter:2007wf}
}
@article{Watanabe:2008ru,
Author = {Watanabe, and H, and others},
Title = {{First Study of Neutron Tagging with a Water Cherenkov
Detector}},
Journal = {Astroparticle Physics},
Volume = {31},
Number = {4},
Pages = {320-328},
Publisher = {Elsevier BV},
Year = {2008},
ISSN = {0927-6505},
url = {http://arxiv.org/pdf/0811.0735},
Abstract = {http://arxiv.org/abs/0811.0735},
Doi = {10.1016/j.astropartphys.2009.03.002},
Key = {Watanabe:2008ru}
}
@article{Abe:2008zza,
Author = {Abe, and K, and others},
Title = {Search for matter-dependent atmospheric neutrino
oscillations in Super-Kamiokande},
Journal = {Phys. Rev.},
Volume = {D77},
Number = {5},
Pages = {052001},
Publisher = {American Physical Society (APS)},
Year = {2008},
ISSN = {1550-7998},
url = {http://arxiv.org/pdf/0801.0776},
Abstract = {We consider νμ→ντ oscillations in the context of the
mass varying neutrino (MaVaN) model, where the neutrino mass
can vary depending on the electron density along the flight
path of the neutrino. Our analysis assumes a mechanism with
dependence only upon the electron density, hence ordinary
matter density, of the medium through which the neutrino
travels. Fully-contained, partially-contained and
upward-going muon atmospheric neutrino data from the
Super-Kamiokande detector, taken from the entire SK-I period
of 1489 live days, are compared to MaVaN model predictions.
We find that, for the case of 2-flavor oscillations, and for
the specific models tested, oscillation independent of
electron density is favored over density dependence.
Assuming maximal mixing, the best-fit case and the
density-independent case do not differ significantly. ©
2008 The American Physical Society.},
Doi = {10.1103/PhysRevD.77.052001},
Key = {Abe:2008zza}
}
@article{Abe:2010hy,
Author = {Cravens, and P, J and others},
Title = {Solar neutrino measurements in Super-Kamiokande-II},
Journal = {Phys. Rev.},
Volume = {D78},
Number = {11},
Pages = {032002},
Year = {2008},
ISSN = {1550-7998},
url = {http://gateway.webofknowledge.com/gateway/Gateway.cgi?GWVersion=2&SrcApp=PARTNER_APP&SrcAuth=LinksAMR&KeyUT=WOS:000288787100001&DestLinkType=FullRecord&DestApp=ALL_WOS&UsrCustomerID=47d3190e77e5a3a53558812f597b0b92},
Abstract = {http://arxiv.org/abs/0803.4312},
Doi = {10.1103/PhysRevD.73.112001},
Key = {Abe:2010hy}
}
@article{Desai:2007ra,
Author = {Desai, and S, and others},
Title = {Study of TeV Neutrinos with Upward Showering Muons in
Super-Kamiokande},
Journal = {Astropart. Phys.},
Volume = {29},
Number = {1},
Pages = {42-54},
Publisher = {Elsevier BV},
Year = {2008},
ISSN = {0927-6505},
url = {http://arxiv.org/pdf/0711.0053},
Abstract = {http://arxiv.org/abs/0711.0053},
Doi = {10.1016/j.astropartphys.2007.11.005},
Key = {Desai:2007ra}
}
@article{fds318497,
Author = {Danzer, SC and Kotloski, RJ and Walter, C and Hughes, M and McNamara,
JO},
Title = {Altered morphology of hippocampal dentate granule cell
presynaptic and postsynaptic terminals following conditional
deletion of TrkB.},
Journal = {Hippocampus},
Volume = {18},
Number = {7},
Pages = {668-678},
Year = {2008},
url = {http://dx.doi.org/10.1002/hipo.20426},
Abstract = {Dentate granule cells play a critical role in the function
of the entorhinal-hippocampal circuitry in health and
disease. Dentate granule cells are situated to regulate the
flow of information into the hippocampus, a structure
required for normal learning and memory. Correspondingly,
impaired granule cell function leads to memory deficits,
and, interestingly, altered granule cell connectivity may
contribute to the hyperexcitability of limbic epilepsy. It
is important, therefore, to understand the molecular
determinants of synaptic connectivity of these neurons.
Brain-derived neurotrophic factor and its receptor TrkB are
expressed at high levels in the dentate gyrus (DG) of the
hippocampus, and are implicated in regulating neuronal
development, neuronal plasticity, learning, and the
development of epilepsy. Whether and how TrkB regulates
granule cell structure, however, is incompletely understood.
To begin to elucidate the role of TrkB in regulating granule
cell morphology, here we examine conditional TrkB knockout
mice crossed to mice expressing green fluorescent protein in
subsets of dentate granule cells. In stratum lucidum, where
granule cell mossy fiber axons project, the density of giant
mossy fiber boutons was unchanged, suggesting similar output
to CA3 pyramidal cell targets. However, filopodial
extensions of giant boutons, which contact inhibitory
interneurons, were increased in number in TrkB knockout mice
relative to wildtype controls, predicting enhanced
feedforward inhibition of CA3 pyramidal cells. In knockout
animals, dentate granule cells possessed fewer primary
dendrites and enlarged dendritic spines, indicative of
disrupted excitatory synaptic input to the granule cells.
Together, these findings demonstrate that TrkB is required
for development and/or maintenance of normal synaptic
connectivity of the granule cells, thereby implying an
important role for TrkB in the function of the granule cells
and hippocampal circuitry.},
Doi = {10.1002/hipo.20426},
Key = {fds318497}
}
@article{fds304631,
Author = {Mine, S and Alcaraz, JL and Andringa, S and Aoki, S and Argyriades, J and Asakura, K and Ashie, R and Berghaus, F and Berns, H and Bhang, H and Blondel, A and Borghi, S and Bouchez, J and Burguet-Castell, J and Casper, D and Catala, J and Cavata, C and Cervera, A and Chen, SM and Cho,
KO and Choi, JH and Dore, U and Espinal, X and Fechner, M and Fernandez, E and Fujii, Y and Fukuda, Y and Gomez-Cadenas, J and Gran, R and Hara, T and Hasegawa, M and Hasegawa, T and Hayato, Y and Helmer, RL and Hiraide, K and Hosaka, J and Ichikawa, AK and Iinuma, M and Ikeda, A and Ishida, T and Ishihara, K and Ishii, T and Ishitsuka, M and Itow, Y and Iwashita, T and Jang, HI and Jeon, EJ and Jeong, IS and Joo, KK and Jover, G and Jung, CK and Kajita, T and Kameda, J and Kaneyuki, K and Kato, I and Kearns, E and Kim,
CO and Khabibullin, M and Khotjantsev, A and Kielczewska, D and Kim, JY and Kim, SB and Kitching, P and Kobayashi, K and Kobayashi, T and Konaka, A and Koshio, Y and Kropp, W and Kudenko, Y and Kuno, Y and Kurimoto, Y and Kutter, T and Learned, J and Likhoded, S and Lim, IT and Loverre, PF and Ludovici, L and Maesaka, H and Mallet, J and Mariani, C and Matsuno, S and Matveev, V and McConnel, K and McGrew, C and Mikheyev, S and Minamino,
A and Mineev, O and Mitsuda, C and Miura, M and Moriguchi, Y and Moriyama,
S and Nakadaira, T and Nakahata, M and Nakamura, K and Nakano, I and Nakaya, T and Nakayama, S and Namba, T and Nambu, R and Nawang,
S},
Title = {Experimental study of the atmospheric neutrino backgrounds
for p→e+π0 searches in water Cherenkov
detectors},
Journal = {Physical Review D - Particles, Fields, Gravitation and
Cosmology},
Volume = {77},
Number = {3},
Publisher = {American Physical Society (APS)},
Year = {2008},
Month = {February},
ISSN = {1550-7998},
url = {http://dx.doi.org/10.1103/PhysRevD.77.032003},
Abstract = {The atmospheric neutrino background for proton decay via
p→e+π0 in ring imaging water Cherenkov detectors is
studied with an artificial accelerator neutrino beam for the
first time. In total, 3.14×105 neutrino events
corresponding to about 10 megaton-years of atmospheric
neutrino interactions were collected by a 1000 ton water
Cherenkov detector (KT). The KT charged-current single π0
production data are well reproduced by simulation programs
of neutrino and secondary hadronic interactions used in the
Super-Kamiokande (SK) proton decay search. The obtained
p→e+π0 background rate by the KT data for SK from the
atmospheric neutrinos whose energies are below 3 GeV is
1.63-0.33+0.42(stat)-0.51+0.45(syst)(megaton-year)- 1. This
result is also relevant to possible future, megaton-scale
water Cherenkov detectors. © 2008 The American Physical
Society.},
Doi = {10.1103/PhysRevD.77.032003},
Key = {fds304631}
}
@article{Hernandez:2008zza,
Author = {Hernández, P and Walter, CW and Yasuda, O},
Title = {Summary of working group one},
Journal = {AIP Conference Proceedings},
Volume = {981},
Pages = {135-138},
Publisher = {AIP},
Year = {2008},
Month = {March},
ISSN = {0094-243X},
url = {http://dx.doi.org/10.1063/1.2898909},
Abstract = {The theoretical and experimental issues discussed in working
group one at Nufact07 are summarized. © 2008 American
Institute of Physics.},
Doi = {10.1063/1.2898909},
Key = {Hernandez:2008zza}
}
@article{Mariani:2010ez,
Author = {Rodriguez, A and Whitehead, L and Alcaraz, JL and Andringa, S and Aoki,
S and Argyriades, J and Asakura, K and Ashie, R and Berghaus, F and Berns,
H and Bhang, H and Blondel, A and Borghi, S and Bouchez, J and Burguet-Castell, J and Casper, D and Catala, J and Cavata, C and Cervera, A and Chen, SM and Cho, KO and Choi, JH and Dore, U and Espinal,
X and Fechner, M and Fernandez, E and Fujii, Y and Fukuda, Y and Gomez-Cadenas, J and Gran, R and Hara, T and Hasegawa, M and Hasegawa,
T and Hayato, Y and Helmer, RL and Hiraide, K and Hosaka, J and Ichikawa,
AK and Iinuma, M and Ikeda, A and Ishida, T and Ishihara, K and Ishii, T and Ishitsuka, M and Itow, Y and Iwashita, T and Jang, HI and Jeon, EJ and Jeong, IS and Joo, KK and Jover, G and Jung, CK and Kajita, T and Kameda,
J and Kaneyuki, K and Kato, I and Kearns, E and Kim, CO and Khabibullin, M and Khotjantsev, A and Kielczewska, D and Kim, JY and Kim, SB and Kitching,
P and Kobayashi, K and Kobayashi, T and Konaka, A and Koshio, Y and Kropp,
W and Kudenko, Y and Kuno, Y and Kurimoto, Y and Kutter, T and Learned, J and Likhoded, S and Lim, IT and Loverre, PF and Ludovici, L and Maesaka, H and Mallet, J and Mariani, C and Matsuno, S and Matveev, V and McConnel, K and McGrew, C and Mikheyev, S and Minamino, A and Mine, S and Mineev, O and Mitsuda, C and Miura, M and Moriguchi, Y and Moriyama, S and Nakadaira,
T and Nakahata, M and Nakamura, K and Nakano, I and Nakaya, T and Nakayama,
S and Namba, T},
Title = {Measurement of single charged pion production in the
charged-current interactions of neutrinos in a 1.3GeV wide
band beam},
Journal = {Physical Review D - Particles, Fields, Gravitation and
Cosmology},
Volume = {78},
Number = {3},
Pages = {054023},
Publisher = {American Physical Society (APS)},
Year = {2008},
Month = {August},
ISSN = {1550-7998},
url = {http://gateway.webofknowledge.com/gateway/Gateway.cgi?GWVersion=2&SrcApp=PARTNER_APP&SrcAuth=LinksAMR&KeyUT=WOS:000288448700003&DestLinkType=FullRecord&DestApp=ALL_WOS&UsrCustomerID=47d3190e77e5a3a53558812f597b0b92},
Abstract = {Single charged pion production in charged-current muon
neutrino interactions with carbon is studied using data
collected in the K2K long-baseline neutrino experiment. The
mean energy of the incident muon neutrinos is 1.3 GeV. The
data used in this analysis are mainly from a fully active
scintillator detector, SciBar. The cross section for single
π+ production in the resonance region (W<2GeV/c2) relative
to the charged-current quasielastic cross section is found
to be 0.734-0.153+0.140. The energy-dependent cross section
ratio is also measured. The results are consistent with a
previous experiment and the prediction of our model. © 2008
The American Physical Society.},
Doi = {10.1103/PhysRevD.78.032003},
Key = {Mariani:2010ez}
}
@article{fds248719,
Author = {Choubey, S and Hernández, P and Walter, CW},
Title = {Summary of working group I: Theory},
Journal = {10th International Workshop on Neutrino Factories, Super
Beams and Beta Beams, NUFACT08},
Year = {2008},
Month = {December},
Abstract = {We present the highlights of the parallel sessions of
Working Group I at Nufact08. © owned by the
author.},
Key = {fds248719}
}
@article{Bernstein:2009ms,
Author = {Kadel, RW and Bernstein, A and Blucher, E and Cline, DB and Diwan, MV and Fleming, B and Kearns, E and Klein, J and Lande, K and Lanni, F and Lissauer, D and McKeown, R and Morse, W and Rameika, R and Scholberg, K and Smy, M and Sobel, H and Sullivan, G and Svoboda, R and Vagins, M and Walter, C and Zwaska, R},
Title = {Report on the Depth Requirements for a Massive Detector at
Homestake},
Publisher = {Office of Scientific and Technical Information
(OSTI)},
Year = {2008},
Month = {December},
url = {http://arxiv.org/pdf/0907.4183},
Abstract = {http://arxiv.org/abs/0907.4183},
Doi = {10.2172/946806},
Key = {Bernstein:2009ms}
}
@article{Thrane:2009tw,
Author = {Thrane, E and Abe, K and Hayato, Y and Iida, T and Ikeda, M and Kameda, J and Kobayashi, K and Koshio, Y and Miura, M and Moriyama, S and Nakahata, M and Nakayama, S and Obayashi, Y and Ogawa, H and Sekiya, H and Shiozawa, M and Suzuki, Y and Takeda, A and Takenaga, Y and Takeuchi, Y and Ueno, K and Ueshima, K and Watanabe, H and Yamada, S and Vagins, MR and Hazama, S and Higuchi, I and Ishihara, C and Kajita, T and Kaneyuki, K and Mitsuka, G and Nishino, H and Okumura, K and Tanimoto, N and Dufour, F and Kearns, E and Litos, M and Raaf, JL and Stone, JL and Sulak, LR and Goldhaber, M and Bays, K and Casper, D and Cravens, JP and Kropp, WR and Mine, S and Regis,
C and Smy, MB and Sobel, HW and Ganezer, KS and Hill, J and Keig, WE and Jang,
JS and Jeong, IS and Kim, JY and Lim, IT and Fechner, M and Scholberg, K and Walter, CW and Wendell, R and Tasaka, S and Learned, JG and Matsuno, S and Watanabe, Y and Hasegawa, T and Ishida, T and Ishii, T and Kobayashi, T and Nakadaira, T and Nakamura, K and Nishikawa, K and Oyama, Y and Sakashita, K and Sekiguchi, T and Tsukamoto, T and Suzuki, AT and Ichikawa, AK and Minamino, A and Nakaya, T and Yokoyama, M and Dazeley,
S and Svoboda, R and Habig, A and Fukuda, Y and Itow, Y and Tanaka, T and Jung, CK and Lopez, G and McGrew, C and Yanagisawa, C and Tamura, N and Idehara, Y and Ishino, H and Kibayashi, A and Sakuda, M and Kuno, Y and Yoshida, M and Kim, SB and Yang, BS and Ishizuka,
T},
Title = {Search for astrophysical neutrino point sources at
super-kamiokande},
Journal = {Astrophysical Journal},
Volume = {704},
Number = {1},
Pages = {503-512},
Publisher = {IOP Publishing},
Year = {2009},
Month = {January},
ISSN = {0004-637X},
url = {http://arxiv.org/pdf/0907.1594},
Abstract = {It has been hypothesized that large fluxes of neutrinos may
be created in astrophysical "cosmic accelerators." The
primary background for a search for astrophysical neutrinos
comes from atmospheric neutrinos, which do not exhibit the
pointlike directional clustering that characterizes a
distant astrophysical signal. We perform a search for
neutrino point sources using the upward-going muon data from
three phases of operation (SK-I, SK-II, and SK-III) spanning
2623 days of live time taken from 1996 April 1 to 2007
August 11. The search looks for signals from suspected
galactic and extragalactic sources, transient sources, and
uncataloged sources. While we find interesting signatures
from two objects - RX J1713.7-3946 (97.5% CL) and GRB
991004D (95.3% CL) - these signatures lack compelling
statistical significance given trial factors. We set limits
on the flux and fluence of neutrino point sources above
energies of 1.6 GeV. © 2009 The American Astronomical
Society. All rights reserved.},
Doi = {10.1088/0004-637X/704/1/503},
Key = {Thrane:2009tw}
}
@article{Thrane:2009fj,
Author = {Thrane, E and Abe, K and Hayato, Y and Iida, T and Ikeda, M and Kameda, J and Kobayashi, K and Koshio, Y and Miura, M and Moriyama, S and Nakahata, M and Nakayama, S and Obayashi, Y and Ogawa, H and Sekiya, H and Shiozawa, M and Suzuki, Y and Takeda, A and Takenaga, Y and Takeuchi, Y and Ueno, K and Ueshima, K and Watanabe, H and Yamada, S and Vagins, MR and Hazama, S and Higuchi, I and Ishihara, C and Kajita, T and Kaneyuki, K and Mitsuka, G and Nishino, H and Okumura, K and Tanimoto, N and Dufour, F and Kearns, E and Litos, M and Raaf, JL and Stone, JL and Sulak, LR and Goldhaber, M and Bays, K and Casper, D and Cravens, JP and Kropp, WR and Mine, S and Regis,
C and Smy, MB and Sobel, HW and Ganezer, KS and Hill, J and Keig, WE and Jang,
JS and Jeong, IS and Kim, JY and Lim, IT and Fechner, M and Scholberg, K and Walter, CW and Wendell, R and Tasaka, S and Learned, JG and Matsuno, S and Watanabe, Y and Hasegawa, T and Ishida, T and Ishii, T and Kobayashi, T and Nakadaira, T and Nakamura, K and Nishikawa, K and Oyama, Y and Sakashita, K and Sekiguchi, T and Tsukamoto, T and Suzuki, AT and Ichikawa, AK and Minamino, A and Nakaya, T and Yokoyama, M and Dazeley,
S and Svoboda, R and Habig, A and Fukuda, Y and Itow, Y and Tanaka, T and Jung, CK and Lopez, G and McGrew, C and Yanagisawa, C and Tamura, N and Idehara, Y and Ishino, H and Kibayashi, A and Sakuda, M and Kuno, Y and Yoshida, M and Kim, SB and Yang, BS and Ishizuka,
T},
Title = {Search for neutrinos from GRB 080319B at
super-kamiokande},
Journal = {Astrophysical Journal},
Volume = {697},
Number = {1},
Pages = {730-734},
Publisher = {IOP Publishing},
Year = {2009},
Month = {January},
ISSN = {0004-637X},
url = {http://arxiv.org/pdf/0903.0624},
Abstract = {We perform a search for neutrinos coincident with GRB
080319B - the brightest GRB observed to date - in a 1000 s
window. No statistically significant coincidences were
observed and we thereby obtain an upper limit on the fluence
of neutrino-induced muons from this source. From this we
apply reasonable assumptions to derive a limit on neutrino
fluence from the GRB. © 2009. The American Astronomical
Society. All rights reserved.},
Doi = {10.1088/0004-637X/697/1/730},
Key = {Thrane:2009fj}
}
@article{:2009gd,
Author = {Nishino, H and Clark, S and Abe, K and Hayato, Y and Iida, T and Ikeda, M and Kameda, J and Kobayashi, K and Koshio, Y and Miura, M and Moriyama, S and Nakahata, M and Nakayama, S and Obayashi, Y and Ogawa, H and Sekiya, H and Shiozawa, M and Suzuki, Y and Takeda, A and Takenaga, Y and Takeuchi, Y and Ueno, K and Ueshima, K and Watanabe, H and Yamada, S and Hazama, S and Higuchi, I and Ishihara, C and Kajita, T and Kaneyuki, K and Mitsuka, G and Okumura, K and Tanimoto, N and Vagins, MR and Dufour, F and Kearns, E and Litos, M and Raaf, JL and Stone, JL and Sulak, LR and Wang, W and Goldhaber, M and Dazeley, S and Svoboda, R and Bays, K and Casper, D and Cravens, JP and Kropp, WR and Mine, S and Regis, C and Smy, MB and Sobel,
HW and Ganezer, KS and Hill, J and Keig, WE and Jang, JS and Kim, JY and Lim,
IT and Fechner, M and Scholberg, K and Walter, CW and Wendell, R and Tasaka, S and Learned, JG and Matsuno, S and Watanabe, Y and Hasegawa,
T and Ishida, T and Ishii, T and Kobayashi, T and Nakadaira, T and Nakamura, K and Nishikawa, K and Oyama, Y and Sakashita, K and Sekiguchi, T and Tsukamoto, T and Suzuki, AT and Minamino, A and Nakaya,
T and Yokoyama, M and Fukuda, Y and Itow, Y and Tanaka, T and Jung, CK and Lopez, G and McGrew, C and Terri, R and Yanagisawa, C and Tamura, N and Idehara, Y and Sakuda, M and Kuno, Y and Yoshida, M and Kim, SB and Yang,
BS and Ishizuka, T and Okazawa, H and Choi, Y and Seo, HK and Furuse, Y and Nishijima, K and Yokosawa, Y and Koshiba, M and Totsuka, Y and Chen, S and Heng, Y and Yang, Z and Zhang, H and Kielczewska, D and Thrane, E and Wilkes, RJ and Super-Kamiokande Collaboration},
Title = {Search for proton decay via p-->e+pi0 and p-->micro+pi0 in a
large water Cherenkov detector.},
Journal = {Physical review letters},
Volume = {102},
Number = {14},
Pages = {141801},
Year = {2009},
Month = {April},
ISSN = {0031-9007},
url = {http://www.ncbi.nlm.nih.gov/pubmed/19392425},
Abstract = {We have searched for proton decays via p-->e;{+}pi;{0} and
p-->micro;{+}pi;{0} using data from a 91.7 kt.yr exposure of
Super-Kamiokande-I and a 49.2 kt.yr exposure of
Super-Kamiokande-II. No candidate events were observed with
expected backgrounds induced by atmospheric neutrinos of 0.3
events for each decay mode. From these results, we set lower
limits on the partial lifetime of 8.2 x 10;{33} and 6.6 x
10;{33} years at 90% confidence level for p-->e;{+}pi;{0}
and p-->micro;{+}pi;{0} modes, respectively.},
Doi = {10.1103/physrevlett.102.141801},
Key = {:2009gd}
}
@article{:2009dpa,
Author = {Fechner, M and Abe, K and Hayato, Y and Iida, T and Ikeda, M and Kameda, J and Kobayashi, K and Koshio, Y and Miura, M and Moriyama, S and Nakahata, M and Nakayama, S and Obayashi, Y and Ogawa, H and Sekiya, H and Shiozawa, M and Suzuki, Y and Takeda, A and Takenaga, Y and Takeuchi, Y and Ueno, K and Ueshima, K and Watanabe, H and Yamada, S and Hazama, S and Higuchi, I and Ishihara, C and Kajita, T and Kaneyuki, K and Mitsuka, G and Nishino, H and Okumura, K and Tanimoto, N and Vagins, MR and Dufour, F and Kearns, E and Litos, M and Raaf, JL and Stone, JL and Sulak, LR and Wang, W and Goldhaber, M and Dazeley, S and Svoboda, R and Bayes, K and Casper, D and Cravens, JP and Kropp, WR and Mine, S and Regis, C and Smy, MB and Sobel,
HW and Ganezer, KS and Hill, J and Keig, WE and Jang, JS and Kim, JY and Lim,
IT and Scholberg, K and Walter, CW and Wendell, R and Tasaka, S and Learned, JG and Matsuno, S and Watanabe, Y and Hasegawa, T and Ishida,
T and Ishii, T and Kobayashi, T and Nakadaira, T and Nakamura, K and Nishikawa, K and Oyama, Y and Sakashita, K and Sekiguchi, T and Tsukamoto, T and Suzuki, AT and Minamino, A and Nakaya, T and Yokoyama,
M and Fukuda, Y and Itow, Y and Tanaka, T and Jung, CK and Lopez, G and McGrew, C and Terri, R and Yanagisawa, C and Tamura, N and Idehara, Y and Sakuda, M and Kuno, Y and Yoshida, M and Kim, SB and Yang, BS and Ishizuka,
T and Okazawa, H and Choi, Y and Seo, HK and Furuse,
Y},
Title = {Kinematic reconstruction of atmospheric neutrino events in a
large water Cherenkov detector with proton
identification},
Journal = {Physical Review D - Particles, Fields, Gravitation and
Cosmology},
Volume = {79},
Number = {11},
Pages = {112010},
Publisher = {American Physical Society (APS)},
Year = {2009},
Month = {June},
ISSN = {1550-7998},
url = {http://arxiv.org/pdf/0901.1645},
Abstract = {We report the development of a proton identification method
for the Super-Kamiokande (SK) detector. This new tool is
applied to the search for events with a single proton track,
a high purity neutral current sample of interest for sterile
neutrino searches. After selection using a neural network,
we observe 38 events in the combined SK-I and SK-II data
corresponding to 2285.1 days of exposure, with an estimated
signal-to-background ratio of 1.6 to 1. Proton
identification was also applied to a direct search for
charged-current quasielastic (CCQE) events, obtaining a high
precision sample of fully kinematically reconstructed
atmospheric neutrinos, which has not been previously
reported in water Cherenkov detectors. The CCQE fraction of
this sample is 55%, and its neutrino (as opposed to
antineutrino) fraction is 91.7±3%. We selected 78μ-like
and 47 e-like events in the SK-I and SK-II data set. With
this data, a clear zenith angle distortion of the neutrino
direction itself is reported in a sub-GeV sample of μ
neutrinos where the lepton angular correlation to the
incoming neutrino is weak. Our fit to νμ→ντ
oscillations using the neutrino LE distribution of the CCQE
sample alone yields a wide acceptance region compatible with
our previous results and excludes the no-oscillation
hypothesis at 3-sigma. © 2009 The American Physical
Society.},
Doi = {10.1103/PhysRevD.79.112010},
Key = {:2009dpa}
}
@article{fds369856,
Author = {Hernandez, P},
Title = {WG1 summary},
Journal = {Proceedings of 10th International Workshop on Neutrino
Factories, Super beams and Beta beams —
PoS(Nufact08)},
Publisher = {Sissa Medialab},
Year = {2009},
Month = {July},
url = {http://dx.doi.org/10.22323/1.074.0026},
Doi = {10.22323/1.074.0026},
Key = {fds369856}
}
@article{Andreopoulos:2009zza,
Author = {Andreopoulos, C and Gallagher, H and Hayato, Y and Sobczyk, JT and Walter, C and Zeller, S},
Title = {The path forward: Monte Carlo convergence
discussion},
Journal = {AIP Conference Proceedings},
Volume = {1189},
Pages = {312-319},
Publisher = {AIP},
Year = {2009},
Month = {December},
ISSN = {0094-243X},
url = {http://dx.doi.org/10.1063/1.3274175},
Abstract = {This is a summary of "the path forward" discussion session
of the NuInt09 workshop which focused on Monte Carlo event
generators. The main questions raised as part of this
discussion are: how to make Monte Carlo generators more
reliable and how important it is to work on a universal
Monte Carlo generator of events? In this contribution,
several experts in the field summarize their views, as
presented at the workshop. © 2009 American Institute of
Physics.},
Doi = {10.1063/1.3274175},
Key = {Andreopoulos:2009zza}
}
@article{Fechner:2009mq,
Author = {Fechner, M and Walter, CW},
Title = {The physics impact of proton track identification in future
megaton-scale water Cherenkov detectors},
Journal = {Journal of High Energy Physics},
Volume = {2009},
Number = {11},
Pages = {040-040},
Publisher = {Springer Nature},
Year = {2009},
Month = {December},
ISSN = {1126-6708},
url = {http://arxiv.org/pdf/0901.1950},
Abstract = {In this paper, we investigate the impact in future
megaton-scale water Cherenkov detectors of identifying
proton Cherenkov rings. We estimate the expected event rates
for detected neutral current and charged current
quasi-elastic neutrino interactions from atmospheric
neutrinos in a megaton-scale Super-Kamiokande-like detector
with both 40% and 20% photo-cathode coverage. With this
sample we examine the prospects for measuring the neutrino
oscillation pattern, and searching for sterile neutrinos. We
also determine the size of selected charged current
quasi-elastic samples in a 300-kton fiducial volume
Super-Kamiokande-like detector from examples of both
conventional super-beams and beta-beams proposed in the
literature. With these samples, it is shown that full
kinematic neutrino reconstruction using the outgoing proton
can improve the reconstructed energy resolution, and give
good neutrino versus anti-neutrino tagging capabilities,
adding important capabilities to water Cherenkov detectors
in future projects. We determine the beam parameters
necessary to make use of this technique and present
distributions of neutrino and anti-neutrino selection
efficiencies. © 2009 SISSA.},
Doi = {10.1088/1126-6708/2009/11/040},
Key = {Fechner:2009mq}
}
@article{fds248721,
Author = {Iida, T and Bays, K},
Title = {A Search for supernova relic neutrinos at
Super-Kamiokande},
Journal = {Journal of Physics: Conference Series},
Volume = {203},
Year = {2010},
ISSN = {1742-6588},
url = {http://dx.doi.org/10.1088/1742-6596/203/1/012088},
Abstract = {Supernova relic neutrinos (SRN) are the diffuse supernova
neutrino background from all past supernovae. No experiment
has succeeded in detecting SRN yet. Currently, the
Super-Kamiokande experiment has the world's best flux upper
limit of 1.2 e/cm2/sec for Ev < 19.3MeV. We have worked
to improve this value by improving the data analysis. We
have achieved better reduction efficiency and lowered the
analysis energy threshold by developing a new spallation cut
as well as optimizing other cuts. © 2010 IOP Publishing
Ltd.},
Doi = {10.1088/1742-6596/203/1/012088},
Key = {fds248721}
}
@article{Nakamura:2010zzi,
Author = {Nakamura, and K, and others},
Title = {Review of particle physics},
Journal = {J. Phys.},
Volume = {G37},
Number = {7 A},
Pages = {075021},
Publisher = {IOP Publishing},
Year = {2010},
ISSN = {0954-3899},
url = {http://gateway.webofknowledge.com/gateway/Gateway.cgi?GWVersion=2&SrcApp=PARTNER_APP&SrcAuth=LinksAMR&KeyUT=WOS:000282072100001&DestLinkType=FullRecord&DestApp=ALL_WOS&UsrCustomerID=47d3190e77e5a3a53558812f597b0b92},
Abstract = {This biennial Review summarizes much of particle physics.
Using data from previous editions, plus 2158 new
measurements from 551 papers, we list, evaluate, and average
measured properties of gauge bosons, leptons, quarks,
mesons, and baryons. We also summarize searches for
hypothetical particles such as Higgs bosons, heavy
neutrinos, and supersymmetric particles. All the particle
properties and search limits are listed in Summary Tables.
We also give numerous tables, figures, formulae, and reviews
of topics such as the Standard Model, particle detectors,
probability, and statistics. Among the 108 reviews are many
that are new or heavily revised including those on neutrino
mass, mixing, and oscillations, QCD, top quark, CKM
quark-mixing matrix, Vud& Vus, Vcb& Vub, fragmentation
functions, particle detectors for accelerator and
non-accelerator physics, magnetic monopoles, cosmological
parameters, and big bang cosmology. © 2010 Regents of the
University of California.},
Doi = {10.1088/0954-3899/37/7A/075021},
Key = {Nakamura:2010zzi}
}
@article{Choubey:2009zz,
Author = {Choubey, S and Schwetz, T and Walter, C},
Title = {Working group I report (theory)},
Journal = {AIP Conference Proceedings},
Volume = {1222},
Pages = {65-74},
Publisher = {AIP},
Year = {2010},
Month = {January},
ISSN = {0094-243X},
url = {http://dx.doi.org/10.1063/1.3399397},
Abstract = {The summary of the talks and discussions in Working Group I
(Neutrino Oscillation Physics) at the NuFact08 workshop is
presented here. © 2010 American Institute of
Physics.},
Doi = {10.1063/1.3399397},
Key = {Choubey:2009zz}
}
@article{fds327690,
Author = {Scholberg, K},
Title = {Experimentation of neutrino physics},
Journal = {TASI 2008 - Proceedings of the 2008 Theoretical Advanced
Study Institute in Elementary Particle Physics: The Dawn of
the LHC Era},
Pages = {565-622},
Publisher = {World Scientific},
Year = {2010},
Month = {January},
url = {http://dx.doi.org/10.1142/9789812838360_0012},
Abstract = {These lectures broadly describe experimental progress in
neutrino physics over the past few decades. I will describe
the basic picture, how we know what we now know, and the
next steps for the future. Copyright © 2010 by World
Scientific Publishing Co. Pte. Ltd.},
Doi = {10.1142/9789812838360_0012},
Key = {fds327690}
}
@article{Wendell:2010md,
Author = {Wendell, R and Ishihara, C and Abe, K and Hayato, Y and Iida, T and Ikeda,
M and Iyogi, K and Kameda, J and Kobayashi, K and Koshio, Y and Kozuma, Y and Miura, M and Moriyama, S and Nakahata, M and Nakayama, S and Obayashi,
Y and Ogawa, H and Sekiya, H and Shiozawa, M and Suzuki, Y and Takeda, A and Takenaga, Y and Takeuchi, Y and Ueno, K and Ueshima, K and Watanabe, H and Yamada, S and Yokozawa, T and Hazama, S and Kaji, H and Kajita, T and Kaneyuki, K and McLachlan, T and Okumura, K and Shimizu, Y and Tanimoto,
N and Vagins, MR and Dufour, F and Kearns, E and Litos, M and Raaf, JL and Stone, JL and Sulak, LR and Wang, W and Goldhaber, M and Bays, K and Casper, D and Cravens, JP and Kropp, WR and Mine, S and Regis, C and Smy,
MB and Sobel, HW and Ganezer, KS and Hill, J and Keig, WE and Jang, JS and Kim, JY and Lim, IT and Albert, J and Fechner, M and Scholberg, K and Walter, CW and Tasaka, S and Learned, JG and Matsuno, S and Watanabe, Y and Hasegawa, T and Ishida, T and Ishii, T and Kobayashi, T and Nakadaira,
T and Nakamura, K and Nishikawa, K and Nishino, H and Oyama, Y and Sakashita, K and Sekiguchi, T and Tsukamoto, T and Suzuki, AT and Minamino, A and Nakaya, T and Fukuda, Y and Itow, Y and Mitsuka, G and Tanaka, T and Jung, CK and Lopez, G and McGrew, C and Yanagisawa, C and Tamura, N and Ishino, H and Kibayashi, A and Mino, S and Mori, T and Sakuda, M and Toyota, H and Kuno, Y and Yoshida, M and Kim,
SB},
Title = {Atmospheric neutrino oscillation analysis with subleading
effects in Super-Kamiokande I, II, and III},
Journal = {Physical Review D - Particles, Fields, Gravitation and
Cosmology},
Volume = {81},
Number = {9},
Pages = {092004},
Publisher = {American Physical Society (APS)},
Year = {2010},
Month = {May},
ISSN = {1550-7998},
url = {http://hdl.handle.net/10161/4274 Duke open
access},
Abstract = {We present a search for nonzero θ13 and deviations of
sin2θ23 from 0.5 in the oscillations of atmospheric
neutrino data from Super-Kamiokande I, II, and III. No
distortions of the neutrino flux consistent with nonzero
θ13 are found and both neutrino mass hierarchy hypotheses
are in agreement with the data. The data are best fit at
Δm2=2.1×10-3eV2, sin2θ13=0.0, and sin2θ23=0.5. In the
normal (inverted) hierarchy θ13 and Δm2 are constrained at
the one-dimensional 90% C.L. to sin2θ13<0.04(0.09) and
1.9(1.7)×10 -3<Δm2<2.6(2.7)×10-3eV2. The atmospheric
mixing angle is within 0.407≤sin2θ23≤0.583 at 90% C.L.
© 2010 The American Physical Society.},
Doi = {10.1103/PhysRevD.81.092004},
Key = {Wendell:2010md}
}
@article{Abe:2011ks,
Author = {Abe, and K, and others},
Title = {The T2K Experiment},
Journal = {Nucl.Instrum.Meth.},
Volume = {A659},
Number = {1},
Pages = {106-135},
Publisher = {Elsevier BV},
Year = {2011},
ISSN = {0168-9002},
url = {http://arxiv.org/pdf/1106.1238},
Abstract = {http://arxiv.org/abs/1106.1238},
Doi = {10.1016/j.nima.2011.06.067},
Key = {Abe:2011ks}
}
@article{Abe:2011sj,
Author = {Abe, and K, and others},
Title = {Indication of Electron Neutrino Appearance from an
Accelerator-produced Off-axis Muon Neutrino
Beam},
Journal = {Phys. Rev. Lett.},
Volume = {107},
Number = {4},
Pages = {041801},
Year = {2011},
url = {http://www.ncbi.nlm.nih.gov/pubmed/21866992},
Abstract = {http://arxiv.org/abs/1106.2822},
Doi = {10.1103/PhysRevLett.107.041801},
Key = {Abe:2011sj}
}
@article{:2008ea,
Author = {Mariani, C and Tornero-Lopez, A and Alcaraz, JL and Andringa, S and Aoki, S and Aoyama, Y and Argyriades, J and Asakura, K and Ashie, R and Berghaus, F and Berns, H and Bhang, H and Blondel, A and Borghi, S and Bouchez, J and Burguet-Castell, J and Casper, D and Catala, J and Cavata, C and Cervera, A and Chen, SM and Cho, KO and Choi, JH and Dore, U and Espinal, X and Fechner, M and Fernandez, E and Fujii, Y and Fukuda, Y and Gomez-Cadenas, J and Gran, R and Hara, T and Hasegawa, M and Hasegawa,
T and Hayato, Y and Helmer, RL and Hiraide, K and Hosaka, J and Ichikawa,
AK and Iinuma, M and Ikeda, A and Ishida, T and Ishihara, K and Ishii, T and Ishitsuka, M and Itow, Y and Iwashita, T and Jang, HI and Jeon, EJ and Jeong, IS and Joo, KK and Jover Manas and G and Jung, CK and Kajita, T and Kameda, J and Kaneyuki, K and Kato, I and Kearns, E and Kim, CO and Khabibullin, M and Khotjantsev, A and Kielczewska, D and Kim, JY and Kim, SB and Kitching, P and Kobayashi, K and Kobayashi, T and Konaka, A and Koshio, Y and Kropp, W and Kudenko, Y and Kuno, Y and Kurimoto, Y and Kutter, T and Learned, J and Likhoded, S and Lim, IT and Loverre, PF and Ludovici, L and Maesaka, H and Mallet, J and Matsuno, S and Matveev, V and McConnel Mahn and K and McGrew, C and Mikheyev, S and Minamino, A and Mine,
S and Mineev, O and Mitsuda, C and Miura, M and Moriguchi, Y and Moriyama,
S and Nakadaira, T and Nakahata, M and Nakamura, K and Nakano, I and Nakaya, T and Nakayama, S and Namba, T},
Title = {Measurement of inclusive π0 production in the
charged-current interactions of neutrinos in a 1.3-GeV wide
band beam},
Journal = {Physical Review D - Particles, Fields, Gravitation and
Cosmology},
Volume = {83},
Number = {5},
Pages = {032003},
Year = {2011},
Month = {March},
ISSN = {1550-7998},
url = {http://arxiv.org/pdf/0805.0186},
Abstract = {In this paper, we report on the measurement of the rate of
inclusive π0 production induced by charged-current neutrino
interactions in a C 8H8 target at a mean energy of 1.3 GeV
in the K2K near detector. Out of a sample of 11606
charged-current neutrino interactions, we select 479 π0
events with two reconstructed photons. We find that the
cross section for the inclusive π0 production relative to
the charged-current quasielastic cross section is
σCCπ0σCCQE=0. 426±0.032(stat)±0.035(syst). The
energy-dependent cross section ratio is also measured. The
results are consistent with previous experiments for
exclusive channels on different targets. © 2011 American
Physical Society.},
Doi = {10.1103/PhysRevD.83.054023},
Key = {:2008ea}
}
@article{fds337273,
Author = {Abe, K and Hayato, Y and Iida, T and Ikeda, M and Ishihara, C and Iyogi, K and Kameda, J and Kobayashi, K and Koshio, Y and Kozuma, Y and Miura, M and Moriyama, S and Nakahata, M and Nakayama, S and Obayashi, Y and Ogawa,
H and Sekiya, H and Shiozawa, M and Suzuki, Y and Takeda, A and Takenaga,
Y and Ueno, K and Ueshima, K and Watanabe, H and Yamada, S and Yokozawa, T and Hazama, S and Kaji, H and Kajita, T and Kaneyuki, K and McLachlan, T and Okumura, K and Shimizu, Y and Tanimoto, N and Vagins, MR and Labarga, L and Magro, LM and Dufour, F and Kearns, E and Litos, M and Raaf, JL and Stone,
JL and Sulak, LR and Wang, W and Goldhaber, M and Bays, K and Casper, D and Cravens, JP and Kropp, WR and Mine, S and Regis, C and Renshaw, A and Smy,
MB and Sobel, HW and Ganezer, KS and Hill, J and Keig, WE and Jang, JS and Kim, JY and Lim, IT and Albert, J and Wendell, R and Wongjirad, T and Scholberg, K and Walter, CW and Ishizuka, T and Tasaka, S and Learned,
JG and Matsuno, S and Watanabe, Y and Hasegawa, T and Ishida, T and Ishii,
T and Kobayashi, T and Nakadaira, T and Nakamura, K and Nishikawa, K and Nishino, H and Oyama, Y and Sakashita, K and Sekiguchi, T and Tsukamoto,
T and Suzuki, AT and Takeuchi, Y and Minamino, A and Nakaya, T and Fukuda,
Y and Itow, Y and Mitsuka, G and Tanaka, T and Jung, CK and Lopez, G and McGrew, C and Terri, R and Yanagisawa, C and Tamura, N and Ishino, H and Kibayashi, A and Mino, S and Mori, T},
Title = {Solar neutrino results in Super-Kamiokande-III},
Journal = {Physical Review D - Particles, Fields, Gravitation and
Cosmology},
Volume = {83},
Number = {5},
Publisher = {American Physical Society (APS)},
Year = {2011},
Month = {March},
url = {http://dx.doi.org/10.1103/PhysRevD.83.052010},
Abstract = {The results of the third phase of the Super-Kamiokande solar
neutrino measurement are presented and compared to the first
and second phase results. With improved detector
calibrations, a full detector simulation, and improved
analysis methods, the systematic uncertainty on the total
neutrino flux is estimated to be ±2.1%, which is about two
thirds of the systematic uncertainty for the first phase of
Super-Kamiokande. The observed B8 solar flux in the 5.0 to
20 MeV total electron energy region is 2.32±0.04(stat)
±0.05(sys)×106cm-2sec-1 under the assumption of pure
electron-flavor content, in agreement with previous
measurements. A combined oscillation analysis is carried out
using SK-I, II, and III data, and the results are also
combined with the results of other solar neutrino
experiments. The best-fit oscillation parameters are
obtained to be sin2θ12=0.30-0.01+0.02(tan2θ
12=0.42-0.02+0.04) and Δm212=6.2-1.9+1.1×10 -5eV2.
Combined with KamLAND results, the best-fit oscillation
parameters are found to be sin2θ12=0.31±0.
01(tan2θ12=0.44±0.03) and Δm212=7.6±0.2×10-5eV2. The B8
neutrino flux obtained from global solar neutrino
experiments is 5.3±0.2(stat+sys) ×106cm-2s-1, while the B8
flux becomes 5.1±0.1(stat+sys)×106cm-2s-1 by adding
KamLAND results. In a three-flavor analysis combining all
solar neutrino experiments, the upper limit of sin2θ13 is
0.060 at 95% C.L.. After combination with KamLAND results,
the upper limit of sin2θ13 is found to be 0.059 at 95% C.L.
© 2011 American Physical Society.},
Doi = {10.1103/PhysRevD.83.052010},
Key = {fds337273}
}
@article{fds330713,
Author = {Renard, B and Dispau, G and Donati, A and Genini, L and Gournay, JF and Kuster, O and Molinié, F and Schild, T and Touzery, R and Vieillard, L and Walter, C},
Title = {Ten years of cryomagnetic W7-X test facility construction
and operation},
Journal = {Cryogenics},
Volume = {51},
Number = {7},
Pages = {384-388},
Publisher = {Elsevier BV},
Year = {2011},
Month = {July},
url = {http://dx.doi.org/10.1016/j.cryogenics.2011.03.005},
Abstract = {The construction, commissioning, and operation phases of the
W7-X cryomagnetic test facility in CEA Saclay lasted ten
years. The large diversity of equipments called, specialties
involved and problems solved attest the expertise that was
required to operate the test facility and test the coils.
Nearly one hundred cryogenic tests were performed on the
seventy W7-X coils, at a rate always increasing, using two
cryostats each holding two coils. This paper presents the
test facility and its operation first, the cryogenic
difficulties that were confronted with their solutions, the
electro-magnetic difficulties encountered along with
corrective actions, and finally the instrumentation and data
acquisition aspects. © 2011 Elsevier Ltd. All rights
reserved.},
Doi = {10.1016/j.cryogenics.2011.03.005},
Key = {fds330713}
}
@article{fds362614,
Author = {Collaboration, TLBNE and Akiri, T and Allspach, D and Andrews, M and Arisaka, K and Arrieta-Diaz, E and Artuso, M and Bai, X and Balantekin,
B and Baller, B and Barletta, W and Barr, G and Bass, M and Beck, A and Becker, B and Bellini, V and Benhar, O and Berger, B and Bergevin, M and Berman, E and Berns, H and Bernstein, A and Beroz, F and Bhatnagar, V and Bhuyan, B and Bionta, R and Bishai, M and Blake, A and Blaufuss, E and Bleakley, B and Blucher, E and Blusk, S and Boehnlein, D and Bolton, T and Brack, J and Bradford, R and Breedon, R and Bromberg, C and Brown, R and Buchanan, N and Camilleri, L and Campbell, M and Carr, R and Carminati,
G and Chen, A and Chen, H and Cherdack, D and Chi, C and Childress, S and Choudhary, B and Church, E and Cline, D and Coleman, S and Corey, R and D'Agostino, M and Davies, G and Dazeley, S and Jong, JD and DeMaat, B and Demuth, D and Dighe, A and Djurcic, Z and Dolph, J and Drake, G and Drozhdin, A and Duan, H and Duyang, H and Dye, S and Dykhuis, T and Edmunds, D and Elliott, S and Enomoto, S and Escobar, C and Felde, J and Feyzi, F and Fleming, B and Fowler, J and Fox, W and Friedland, A and Fujikawa, B and Gallagher, H and Garilli, G and Garvey, G and Gehman, V and Geronimo, G and Gill, R and Goodman, M and Goon, J and Gorbunov, D and Gran, R and Guarino, V and Guarnaccia, E and Guenette, R and Gupta, P and Habig, A and Hackenberg, R and Hahn, A and Hahn, R and Haines, T and Hans,
S and Harton, J and Hays, S and Hazen, E and He, Q and Heavey, A and Heeger,
K and Hellauer, R and Himmel, A and Horton-Smith, G and Howell, J and Huber, P and Hurh, P and Huston, J and Hylen, J and Insler, J and Jaffe, D and James, C and Johnson, C and Johnson, M and Johnson, R and Johnson, W and Johnston, W and Johnstone, J and Jones, B and Jostlein, H and Junk, T and Junnarkar, S and Kadel, R and Kafka, T and Kaminski, D and Karagiorgi,
G and Karle, A and Kaspar, J and Katori, T and Kayser, B and Kearns, E and Kettell, S and Khanam, F and Klein, J and Kneller, J and Koizumi, G and Kopp, J and Kopp, S and Kropp, W and Kudryavtsev, V and Kumar, A and Kumar,
J and Kutter, T and Lackowski, T and Lande, K and Lane, C and Lang, K and Lanni, F and Lanza, R and Latorre, T and Learned, J and Lee, D and Lee, K and Li, Y and Linden, S and Ling, J and Link, J and Littenberg, L and Loiacono,
L and Liu, T and Losecco, J and Louis, W and Lucas, P and Lunardini, C and Lundberg, B and Lundin, T and Makowiecki, D and Malys, S and Mandal, S and Mann, A and Mantsch, P and Marciano, W and Mariani, C and Maricic, J and Marino, A and Marshak, M and Maruyama, R and Mathews, J and Matsuno, S and Mauger, C and McCluskey, E and McDonald, K and McFarland, K and McKeown,
R and McTaggart, R and Mehdiyev, R and Melnitchouk, W and Meng, Y and Mercurio, B and Messier, M and Metcalf, W and Milincic, R and Miller, W and Mills, G and Mishra, S and MoedSher, S and Mohapatra, D and Mokhov, N and Moore, C and Morfin, J and Morse, W and Moss, A and Mufson, S and Musser,
J and Naples, D and Napolitano, J and Newcomer, M and Norris, B and Ouedraogo, S and Page, B and Pakvasa, S and Paley, J and Paolone, V and Papadimitriou, V and Parsa, Z and Partyka, K and Pavlovic, Z and Pearson, C and Perasso, S and Petti, R and Plunkett, R and Polly, C and Pordes, S and Potenza, R and Prakash, A and Prokofiev, O and Qian, X and Raaf, J and Radeka, V and Raghavan, R and Rameika, R and Rebel, B and Rescia, S and Reitzner, D and Richardson, M and Riesselman, K and Robinson, M and Rosen, M and Rosenfeld, C and Rucinski, R and Russo, T and Sahijpal, S and Salon, S and Samios, N and Sanchez, M and Schmitt, R and Schmitz, D and Schneps, J and Scholberg, K and Seibert, S and Sergiampietri, F and Shaevitz, M and Shanahan, P and Shaposhnikov, M and Sharma, R and Simos, N and Singh, V and Sinnis, G and Sippach, W and Skwarnicki, T and Smy, M and Sobel, H and Soderberg, M and Sondericker,
J and Sondheim, W and Spitz, J and Spooner, N and Stancari, M and Stancu,
I and Stewart, J and Stoler, P and Stone, J and Stone, S and Strait, J and Straszheim, T and Striganov, S and Sullivan, G and Svoboda, R and Szczerbinska, B and Szelc, A and Talaga, R and Tanaka, H and Tayloe, R and Taylor, D and Thomas, J and Thompson, L and Thomson, M and Thorn, C and Tian, X and Toki, W and Tolich, N and Tripathi, M and Trovato, M and Tseung, H and Tzanov, M and Urheim, J and Usman, S and Vagins, M and Berg,
RV and Water, RVD and Varner, G and Vaziri, K and Velev, G and Viren, B and Wachala, T and Walter, C and Wang, H and Wang, Z and Warner, D and Webber,
D and Weber, A and Wendell, R and Wendt, C and Wetstein, M and White, H and White, S and Whitehead, L and Willis, W and Wilson, RJ and Winslow, L and Ye, J and Yeh, M and Yu, B and Zeller, G and Zhang, C and Zimmerman, E and Zwaska, R},
Title = {The 2010 Interim Report of the Long-Baseline Neutrino
Experiment Collaboration Physics Working
Groups},
Year = {2011},
Month = {October},
Abstract = {In early 2010, the Long-Baseline Neutrino Experiment (LBNE)
science collaboration initiated a study to investigate the
physics potential of the experiment with a broad set of
different beam, near- and far-detector configurations. Nine
initial topics were identified as scientific areas that
motivate construction of a long-baseline neutrino experiment
with a very large far detector. We summarize the scientific
justification for each topic and the estimated performance
for a set of far detector reference configurations. We
report also on a study of optimized beam parameters and the
physics capability of proposed Near Detector configurations.
This document was presented to the collaboration in fall
2010 and updated with minor modifications in early
2011.},
Key = {fds362614}
}
@article{fds326727,
Author = {Tremblin, P and Minier, V and Schneider, N and Durand, GA and Ashley,
MCB and Lawrence, JS and Luong-Van, DM and Storey, JWV and Reinert, Y and Veyssiere, C and Walter, C and Ade, P and Calisse, PG and Challita, Z and Fossat, E and Sabbatini, L and Pellegrini, A and Ricaud, P and Urban,
J},
Title = {Site testing for submillimetre astronomy at Dome C,
Antarctica},
Journal = {Astronomy and Astrophysics},
Volume = {535},
Pages = {A112-A112},
Publisher = {E D P SCIENCES},
Year = {2011},
Month = {November},
url = {http://dx.doi.org/10.1051/0004-6361/201117345},
Abstract = {Aims. Over the past few years a major effort has been put
into the exploration of potential sites for the deployment
of submillimetre astronomical facilities. Amongst the most
important sites are Dome C and Dome A on the Antarctic
Plateau, and the Chajnantor area in Chile. In this context,
we report on measurements of the sky opacity at 200 μm over
a period of three years at the French-Italian station,
Concordia, at Dome C, Antarctica. We also present some
solutions to the challenges of operating in the harsh polar
environment. Methods. The 200-μm atmospheric opacity was
measured with a tipper. The forward atmospheric model
MOLIERE (Microwave Observation LIne Estimation and
REtrieval) was used to calculate the atmospheric
transmission and to evaluate the precipitable water vapour
content (PWV) from the observed sky opacity. These results
have been compared with satellite measurements from the
Infrared Atmospheric Sounding Interferometer (IASI) on
Metop-A, with balloon humidity sondes and with results
obtained by a ground-based microwave radiometer (HAMSTRAD).
In addition, a series of experiments has been designed to
study frost formation on surfaces, and the temporal and
spatial evolution of thermal gradients in the low
atmosphere. Results. Dome C offers exceptional conditions in
terms of absolute atmospheric transmission and stability for
submillimetre astronomy. Over the austral winter the PWV
exhibits long periods during which it is stable and at a
very low level (0.1 to 0.3 mm). Higher values (0.2 to 0.8
mm) of PWV are observed during the short summer period.
Based on observations over three years, a transmission of
around 50% at 350 μm is achieved for 75% of the time. The
200-μm window opens with a typical transmission of 10% to
15% for 25% of the time. Conclusions. Dome C is one of the
best accessible sites on Earth for submillimetre astronomy.
Observations at 350 or 450 μm are possible all year round,
and the 200-μm window opens long enough and with a
sufficient transparency to be useful. Although the polar
environment severely constrains hardware design, a permanent
observatory with appropriate technical capabilities is
feasible. Because of the very good astronomical conditions,
high angular resolution and time series (multi-year)
observations at Dome C with a medium size single dish
telescope would enable unique studies to be conducted, some
of which are not otherwise feasible even from space. © 2011
ESO.},
Doi = {10.1051/0004-6361/201117345},
Key = {fds326727}
}
@article{fds248723,
Author = {Walter, C},
Title = {Cross-section effects in the super-kamiokande tau appearance
analysis},
Journal = {AIP Conference Proceedings},
Volume = {1405},
Pages = {186-191},
Publisher = {AIP},
Year = {2011},
Month = {December},
ISSN = {0094-243X},
url = {http://dx.doi.org/10.1063/1.3661583},
Abstract = {In this talk, I explain the search for tau neutrino
appearance in the atmospheric neutrino flux at
Super-Kamiokande with a particular emphasis on the effect
deep inelastic cross section uncertainties have on
interpreting the result. In particular, I explain why the
normalization of the DIS cross-section also needs to be
treated as a parameter in the fit of tau normalization, and
show how a neural net based on event parameters can separate
various cross-section modes in the background sample. ©
2011 American Institute of Physics.},
Doi = {10.1063/1.3661583},
Key = {fds248723}
}
@article{fds248762,
Author = {Tanaka, T and Abe, K and Hayato, Y and Iida, T and Kameda, J and Koshio, Y and Kouzuma, Y and Miura, M and Moriyama, S and Nakahata, M and Nakayama, S and Obayashi, Y and Sekiya, H and Shiozawa, M and Suzuki, Y and Takeda, A and Takenaga, Y and Ueno, K and Ueshima, K and Yamada, S and Yokozawa, T and Ishihara, C and Hazama, S and Kaji, H and Kajita, T and Kaneyuki, K and McLachlan, T and Okumura, K and Shimizu, Y and Tanimoto, N and Dufour,
F and Kearns, E and Litos, M and Raaf, JL and Stone, JL and Sulak, LR and Cravens, JP and Bays, K and Kropp, WR and Mine, S and Regis, C and Smy, MB and Sobel, HW and Ganezer, KS and Hill, J and Keig, WE and Jang, JS and Kim,
JY and Lim, IT and Albert, JB and Scholberg, K and Walter, CW and Wendell,
R and Wongjirad, T and Ishizuka, T and Tasaka, S and Learned, JG and Matsuno, S and Smith, S and Martens, K and Vagins, M and Watanabe, Y and Hasegawa, T and Ishida, T and Ishii, T and Kobayashi, T and Nakadaira,
T and Nakamura, K and Nishikawa, K and Nishino, H and Oyama, Y and Sakashita, K and Sekiguchi, T and Tsukamoto, T and Suzuki, AT and Takeuchi, Y and Ikeda, M and Minamino, A and Nakaya, T and Labarga, L and Fukuda, Y and Itow, Y and Mitsuka, G and Jung, CK and McGrew, C and Lopez,
G and Yanagisawa, C and Tamura, N and Ishino, H and Kibayashi, A and Sakuda, M and Kuno, Y and Yoshida, M and Kim, SB and Yang, BS and Okazawa,
H and Choi, Y and Nishijima, K and Yokosawa, Y and Koshiba,
M},
Title = {An indirect search for weakly interacting massive particles
in the sun using 3109.6days of upward-going muons in
super-kamiokande},
Journal = {Astrophysical Journal},
Volume = {742},
Number = {2},
Pages = {78-78},
Publisher = {IOP Publishing},
Year = {2011},
Month = {December},
ISSN = {0004-637X},
url = {http://dx.doi.org/10.1088/0004-637X/742/2/78},
Abstract = {We present the result of an indirect search for high energy
neutrinos from Weakly Interacting Massive Particle (WIMP)
annihilation in the Sun using upward-going muon (upmu)
events at Super-Kamiokande. Data sets from SKI-SKIII
(3109.6days) were used for the analysis. We looked for an
excess of neutrino signal from the Sun as compared with the
expected atmospheric neutrino background in three upmu
categories: stopping, non-showering, and showering. No
significant excess was observed. The 90% C.L. upper limits
of upmu flux induced by WIMPs of 100GeV c-2 were 6.4 ×
10-15cm -2s-1 and 4.0 × 10-15cm -2s-1 for the soft and hard
annihilation channels, respectively. These limits correspond
to upper limits of 4.5 × 10 -39cm-2 and 2.7 × 10-40cm-2
for spin-dependent WIMP-nucleon scattering cross sections in
the soft and hard annihilation channels, respectively. ©
2011. The American Astronomical Society. All rights
reserved.},
Doi = {10.1088/0004-637X/742/2/78},
Key = {fds248762}
}
@article{Abe:2011ph,
Author = {Abe, K and Hayato, Y and Iida, T and Ikeda, M and Iyogi, K and Kameda, J and Koshio, Y and Kozuma, Y and Miura, M and Moriyama, S and Nakahata, M and Nakayama, S and Obayashi, Y and Sekiya, H and Shiozawa, M and Suzuki, Y and Takeda, A and Takenaga, Y and Takeuchi, Y and Ueno, K and Ueshima, K and Watanabe, H and Yamada, S and Yokozawa, T and Ishihara, C and Kaji, H and Lee, KP and Kajita, T and Kaneyuki, K and McLachlan, T and Okumura, K and Shimizu, Y and Tanimoto, N and Martens, K and Vagins, MR and Labarga, L and Magro, LM and Dufour, F and Kearns, E and Litos, M and Raaf, JL and Stone,
JL and Sulak, LR and Goldhaber, M and Bays, K and Kropp, WR and Mine, S and Regis, C and Smy, MB and Sobel, HW and Ganezer, KS and Hill, J and Keig,
WE and Jang, JS and Kim, JY and Lim, IT and Albert, JB and Scholberg, K and Walter, CW and Wendell, R and Wongjirad, TM and Tasaka, S and Learned,
JG and Matsuno, S and Hasegawa, T and Ishida, T and Ishii, T and Kobayashi,
T and Nakadaira, T and Nakamura, K and Nishikawa, K and Nishino, H and Oyama, Y and Sakashita, K and Sekiguchi, T and Tsukamoto, T and Suzuki,
AT and Minamino, A and Nakaya, T and Fukuda, Y and Itow, Y and Mitsuka, G and Tanaka, T and Jung, CK and Taylor, I and Yanagisawa, C and Ishino, H and Kibayashi, A and Mino, S and Mori, T and Sakuda, M and Toyota, H and Kuno,
Y and Kim, SB and Yang, BS and Ishizuka, T and Okazawa, H and Choi, Y and Nishijima, K and Koshiba, M and Yokoyama, M and Totsuka, Y and Chen, S and Heng, Y and Yang, Z and Zhang, H and Kielczewska, D and Mijakowski, P and Connolly, K and Dziomba, M and Wilkes, RJ and Super-Kamiokande
Collaboration},
Title = {Search for differences in oscillation parameters for
atmospheric neutrinos and antineutrinos at
Super-Kamiokande.},
Journal = {Physical review letters},
Volume = {107},
Number = {24},
Pages = {241801},
Year = {2011},
Month = {December},
url = {http://www.ncbi.nlm.nih.gov/pubmed/22242990},
Abstract = {We present a search for differences in the oscillations of
antineutrinos and neutrinos in the Super-Kamiokande-I, -II,
and -III atmospheric neutrino sample. Under a two-flavor
disappearance model with separate mixing parameters between
neutrinos and antineutrinos, we find no evidence for a
difference in oscillation parameters. Best-fit antineutrino
mixing is found to be at (Δm2,sin2 2θ)=(2.0×10(-3) eV2,
1.0) and is consistent with the overall Super-K
measurement.},
Doi = {10.1103/physrevlett.107.241801},
Key = {Abe:2011ph}
}
@article{Mitsuka:2011ty,
Author = {Mitsuka, G and Abe, K and Hayato, Y and Iida, T and Ikeda, M and Kameda, J and Koshio, Y and Miura, M and Moriyama, S and Nakahata, M and Nakayama, S and Obayashi, Y and Sekiya, H and Shiozawa, M and Suzuki, Y and Takeda, A and Takenaga, Y and Takeuchi, Y and Ueno, K and Ueshima, K and Watanabe, H and Yamada, S and Hazama, S and Higuchi, I and Ishihara, C and Kaji, H and Kajita, T and Kaneyuki, K and Nishino, H and Okumura, K and Tanimoto, N and Dufour, F and Kearns, E and Litos, M and Raaf, JL and Stone, JL and Sulak,
LR and Goldhaber, M and Bays, K and Cravens, JP and Kropp, WR and Mine, S and Regis, C and Smy, MB and Sobel, HW and Vagins, MR and Ganezer, KS and Hill,
J and Keig, WE and Jang, JS and Kim, JY and Lim, IT and Albert, J and Scholberg, K and Walter, CW and Wendell, R and Ishizuka, T and Tasaka,
S and Learned, JG and Matsuno, S and Watanabe, Y and Hasegawa, T and Ishida, T and Ishii, T and Kobayashi, T and Nakadaira, T and Nakamura,
K and Nishikawa, K and Oyama, Y and Sakashita, K and Sekiguchi, T and Tsukamoto, T and Suzuki, AT and Minamino, A and Nakaya, T and Yokoyama,
M and Fukuda, Y and Itow, Y and Tanaka, T and Jung, CK and Lopez, G and McGrew, C and Yanagisawa, C and Tamura, N and Idehara, Y and Sakuda, M and Kuno, Y and Yoshida, M and Kim, SB and Yang, BS and Okazawa, H and Choi, Y and Seo, HK and Furuse, Y and Nishijima, K and Yokosawa, Y and Koshiba, M and Totsuka, Y and Chen, S and Liu, J},
Title = {Study of nonstandard neutrino interactions with atmospheric
neutrino data in Super-Kamiokande i and II},
Journal = {Physical Review D - Particles, Fields, Gravitation and
Cosmology},
Volume = {84},
Number = {11},
Pages = {113008},
Publisher = {American Physical Society (APS)},
Year = {2011},
Month = {December},
ISSN = {1550-7998},
url = {http://arxiv.org/pdf/1109.1889},
Abstract = {In this paper we study nonstandard neutrino interactions as
an example of physics beyond the standard model using
atmospheric neutrino data collected during the
Super-Kamiokande I (1996-2001) and II (2003-2005) periods.
We focus on flavor-changing-neutral-currents (FCNC), which
allow neutrino flavor transitions via neutral current
interactions, and effects which violate lepton
nonuniversality and give rise to different neutral-current
interaction- amplitudes for different neutrino flavors. We
obtain a limit on the FCNC coupling parameter, ε μτ, |ε
μτ|< 1.1×10 -2 at 90% C.L. and various constraints on
other FCNC parameters as a function of the nonuniversality
coupling, ε ee. We find no evidence of nonstandard neutrino
interactions in the Super-Kamiokande atmospheric data. ©
2011 American Physical Society.},
Doi = {10.1103/PhysRevD.84.113008},
Key = {Mitsuka:2011ty}
}
@article{Abe:2011xv,
Author = {Abe, K and Abgrall, N and Ajima, Y and Aihara, H and Albert, JB and others},
Title = {Measurements of the T2K neutrino beam properties using the
INGRID on-axis near detector},
Journal = {Nucl.Instrum.Meth.},
Volume = {A694},
Pages = {211-223},
Publisher = {Elsevier BV},
Year = {2012},
ISSN = {0168-9002},
url = {http://arxiv.org/pdf/1111.3119},
Abstract = {http://arxiv.org/abs/1111.3119},
Doi = {10.1016/j.nima.2012.03.023},
Key = {Abe:2011xv}
}
@article{Beringer:1900zz,
Author = {Beringer, and J, and others},
Title = {Review of Particle Physics (RPP)},
Journal = {Phys.Rev.},
Volume = {D86},
Number = {1},
Pages = {010001},
Publisher = {American Physical Society (APS)},
Year = {2012},
ISSN = {1550-7998},
url = {http://gateway.webofknowledge.com/gateway/Gateway.cgi?GWVersion=2&SrcApp=PARTNER_APP&SrcAuth=LinksAMR&KeyUT=WOS:000306603100001&DestLinkType=FullRecord&DestApp=ALL_WOS&UsrCustomerID=47d3190e77e5a3a53558812f597b0b92},
Abstract = {This biennial Review summarizes much of particle physics.
Using data from previous editions, plus 2658 new
measurements from 644 papers, we list, evaluate, and average
measured properties of gauge bosons, leptons, quarks,
mesons, and baryons. We summarize searches for hypothetical
particles such as Higgs bosons, heavy neutrinos, and
supersymmetric particles. All the particle properties and
search limits are listed in Summary Tables. We also give
numerous tables, figures, formulae, and reviews of topics
such as the Standard Model, particle detectors, probability,
and statistics. Among the 112 reviews are many that are new
or heavily revised including those on Heavy-Quark and
Soft-Collinear Effective Theory, Neutrino Cross Section
Measurements, Monte Carlo Event Generators, Lattice QCD,
Heavy Quarkonium Spectroscopy, Top Quark, Dark Matter, Vcb&
Vub, Quantum Chromodynamics, High-Energy Collider
Parameters, Astrophysical Constants, Cosmological
Parameters, and Dark Matter. A booklet is available
containing the Summary Tables and abbreviated versions of
some of the other sections of this full Review. All tables,
listings, and reviews (and errata) are also available on the
Particle Data Group website: http://pdg.lbl.gov/. The 2012
edition of Review of Particle Physics is published for the
Particle Data Group as article 010001 in volume 86 of
Physical Review D. This edition should be cited as: J.
Beringer et al. (Particle Data Group), Phys. Rev. D 86,
010001 (2012). © 2012 Regents of the University of
California.},
Doi = {10.1103/PhysRevD.86.010001},
Key = {Beringer:1900zz}
}
@article{Abe:2012gx,
Author = {Abe, and K, and others},
Title = {First Muon-Neutrino Disappearance Study with an Off-Axis
Beam},
Journal = {Phys.Rev.},
Volume = {D85},
Number = {3},
Pages = {031103},
Publisher = {American Physical Society (APS)},
Year = {2012},
ISSN = {1550-7998},
url = {http://arxiv.org/pdf/1201.1386},
Abstract = {http://arxiv.org/abs/1201.1386},
Doi = {10.1103/PhysRevD.85.031103},
Key = {Abe:2012gx}
}
@article{fds287700,
Author = {Beringer, J and Arguin, JF and Barnett, RM and Copic, K and Dahl, O and Groom, DE and Lin, CJ and Lys, J and Murayama, H and Wohl, CG and Yao, WM and Zyla, PA and Amsler, C and Antonelli, M and Asner, DM and Baer, H and Band,
HR and Basaglia, T and Bauer, CW and Beatty, JJ and Belousov, VI and Bergren, E and Bernardi, G and Bertl, W and Bethke, S and Bichsel, H and Biebel, O and Blucher, E and Blusk, S and Brooijmans, G and Buchmueller,
O and Cahn, RN and Carena, M and Ceccucci, A and Chakraborty, D and Chen,
MC and Chivukula, RS and Cowan, G and D'ambrosio, G and Damour, T and Florian, DD and Gouvêa, AD and Degrand, T and Jong, PD and Dissertori,
G and Dobrescu, B and Doser, M and Drees, M and Edwards, DA and Eidelman,
S and Erler, J and Ezhela, VV and Fetscher, W and Fields, BD and Foster, B and Gaisser, TK and Garren, L and Gerber, HJ and Gerbier, G and Gherghetta,
T and Golwala, S and Goodman, M and Grab, C and Gritsan, AV and Grivaz, JF and Grünewald, M and Gurtu, A and Gutsche, T and Haber, HE and Hagiwara, K and Hagmann, C and Hanhart, C and Hashimoto, S and Hayes, KG and Heffner, M and Heltsley, B and Hernández-Rey, JJ and Hikasa, K and Höcker, A and Holder, J and Holtkamp, A and Huston, J and Jackson, JD and Johnson, KF and Junk, T and Karlen, D and Kirkby, D and Klein, SR and Klempt, E and Kowalewski, RV and Krauss, F and Kreps, M and Krusche, B and Kuyanov,
YV and Kwon, Y and Lahav, O and Laiho, J and Langacker, P and Liddle, A and Ligeti, Z and Liss, TM and Littenberg, L and Lugovsky, KS and Lugovsky,
SB and Mannel, T and Manohar, AV and Marciano, WJ and Martin, AD and Masoni, A and Matthews, J and Milstead, D and Miquel, R and Mönig, K and Moortgat, F and Nakamura, K and Narain, M and Nason, P and Navas, S and Neubert, M and Nevski, P and Nir, Y and Olive, KA and Pape, L and Parsons,
J and Patrignani, C and Peacock, JA and Petcov, ST and Piepke, A and Pomarol, A and Punzi, G and Quadt, A and Raby, S and Raffelt, G and Ratcliff, BN and Richardson, P and Roesler, S and Rolli, S and Romaniouk, A and Rosenberg, LJ and Rosner, JL and Sachrajda, CT and Sakai, Y and Salam, GP and Sarkar, S and Sauli, F and Schneider, O and Scholberg, K and Scott, D and Seligman, WG and Shaevitz, MH and Sharpe,
SR and Silari, M and Sjöstrand, T and Skands, P and Smith, JG and Smoot,
GF and Spanier, S and Spieler, H and Stahl, A and Stanev, T and Stone, SL and Sumiyoshi, T and Syphers, MJ and Takahashi, F and Tanabashi, M and Terning, J and Titov, M and Tkachenko, NP and Törnqvist, NA and Tovey,
D and Valencia, G and Bibber, KV and Venanzoni, G and Vincter, MG and Vogel, P and Vogt, A and Walkowiak, W and Walter, CW and Ward, DR and Watari, T and Weiglein, G and Weinberg, EJ and Wiencke, LR and Wolfenstein, L and Womersley, J and Woody, CL and Workman, RL and Yamamoto, A and Zeller, GP and Zenin, OV and Zhang, J and Zhu, RY and Harper, G and Lugovsky, VS and Schaffner, P},
Title = {Review of particle physics},
Journal = {Physical Review D - Particles, Fields, Gravitation and
Cosmology},
Volume = {86},
Number = {1},
Year = {2012},
ISSN = {1550-7998},
url = {http://dx.doi.org/10.1103/PhysRevD.70.096011},
Abstract = {This biennial Review summarizes much of particle physics.
Using data from previous editions, plus 2658 new
measurements from 644 papers, we list, evaluate, and average
measured properties of gauge bosons, leptons, quarks,
mesons, and baryons. We summarize searches for hypothetical
particles such as Higgs bosons, heavy neutrinos, and
supersymmetric particles. All the particle properties and
search limits are listed in Summary Tables. We also give
numerous tables, figures, formulae, and reviews of topics
such as the Standard Model, particle detectors, probability,
and statistics. Among the 112 reviews are many that are new
or heavily revised including those on Heavy-Quark and
Soft-Collinear Effective Theory, Neutrino Cross Section
Measurements, Monte Carlo Event Generators, Lattice QCD,
Heavy Quarkonium Spectroscopy, Top Quark, Dark Matter, V cb
& V ub, Quantum Chromodynamics, High-Energy Collider
Parameters, Astrophysical Constants, Cosmological
Parameters, and Dark Matter. A booklet is available
containing the Summary Tables and abbreviated versions of
some of the other sections of this full Review. All tables,
listings, and reviews (and errata) are also available on the
Particle Data Group website: http://pdg.lbl.gov/. The 2012
edition of Review of Particle Physics is published for the
Particle Data Group as article 010001 in volume 86 of
Physical Review D. This edition should be cited as: J.
Beringer et al. (Particle Data Group), Phys. Rev. D 86,
010001 (2012). © 2012 Regents of the University of
California.},
Doi = {10.1103/PhysRevD.70.096011},
Key = {fds287700}
}
@article{Bays:2011si,
Author = {Bays, K and Iida, T and Abe, K and Hayato, Y and Iyogi, K and Kameda, J and Koshio, Y and Marti, L and Miura, M and Moriyama, S and Nakahata, M and Nakayama, S and Obayashi, Y and Sekiya, H and Shiozawa, M and Suzuki, Y and Takeda, A and Takenaga, Y and Ueno, K and Ueshima, K and Yamada, S and Yokozawa, T and Kaji, H and Kajita, T and Kaneyuki, K and McLachlan, T and Okumura, K and Lee, KP and Martens, K and Vagins, M and Labarga, L and Kearns, E and Litos, M and Raaf, JL and Stone, JL and Sulak, LR and Kropp,
WR and Mine, S and Regis, C and Renshaw, A and Smy, MB and Sobel, HW and Ganezer, KS and Hill, J and Keig, WE and Cho, S and Jang, JS and Kim, JY and Lim, IT and Albert, J and Scholberg, K and Walter, CW and Wendell, R and Wongjirad, T and Ishizuka, T and Tasaka, S and Learned, JG and Matsuno,
S and Smith, S and Hasegawa, T and Ishida, T and Ishii, T and Kobayashi, T and Nakadaira, T and Nakamura, K and Nishikawa, K and Oyama, Y and Sakashita, K and Sekiguchi, T and Tsukamoto, T and Suzuki, AT and Takeuchi, Y and Ikeda, M and Matsuoka, K and Minamino, A and Murakami,
A and Nakaya, T and Fukuda, Y and Itow, Y and Mitsuka, G and Miyake, M and Tanaka, T and Hignight, J and Imber, J and Jung, CK and Taylor, I and Yanagisawa, C and Kibayashi, A and Ishino, H and Mino, S and Sakuda, M and Mori, T and Toyota, H and Kuno, Y and Kim, SB and Yang, BS and Okazawa, H and Choi, Y and Nishijima, K and Koshiba, M},
Title = {Supernova relic neutrino search at super-Kamiokande},
Journal = {Physical Review D - Particles, Fields, Gravitation and
Cosmology},
Volume = {85},
Number = {5},
Pages = {052007},
Publisher = {American Physical Society (APS)},
Year = {2012},
Month = {March},
ISSN = {1550-7998},
url = {http://arxiv.org/pdf/1111.5031},
Abstract = {A new Super-Kamiokande search for supernova relic neutrinos
was conducted using 2853 live days of data. Sensitivity is
now greatly improved compared to the 2003 Super-Kamiokande
result, which placed a flux limit near many theoretical
predictions. This more detailed analysis includes a variety
of improvements such as increased efficiency, a lower energy
threshold, and an expanded data set. New combined upper
limits on supernova relic neutrino flux are between 2.8 and
3.1ν ̄ecm -2s -1>16MeV total positron energy (17.3MeV E
ν). © 2012 American Physical Society.},
Doi = {10.1103/PhysRevD.85.052007},
Key = {Bays:2011si}
}
@article{:2012rv,
Author = {Nishino, H and Abe, K and Hayato, Y and Iida, T and Ikeda, M and Kameda, J and Koshio, Y and Miura, M and Moriyama, S and Nakahata, M and Nakayama, S and Obayashi, Y and Sekiya, H and Shiozawa, M and Suzuki, Y and Takeda, A and Takenaga, Y and Takeuchi, Y and Ueno, K and Ueshima, K and Watanabe, H and Yamada, S and Hazama, S and Higuchi, I and Ishihara, C and Kaji, H and Kajita, T and Kaneyuki, K and Mitsuka, G and Okumura, K and Tanimoto, N and Dufour, F and Kearns, E and Litos, M and Raaf, JL and Stone, JL and Sulak,
LR and Goldhaber, M and Bays, K and Cravens, JP and Kropp, WR and Mine, S and Regis, C and Smy, MB and Sobel, HW and Ganezer, KS and Hill, J and Keig,
WE and Jang, JS and Kim, JY and Lim, IT and Albert, JB and Scholberg, K and Walter, CW and Wendell, R and Ishizuka, T and Tasaka, S and Learned, JG and Matsuno, S and Watanabe, Y and Hasegawa, T and Ishida, T and Ishii, T and Kobayashi, T and Nakadaira, T and Nakamura, K and Nishikawa, K and Oyama, Y and Sakashita, K and Sekiguchi, T and Tsukamoto, T and Suzuki,
AT and Minamino, A and Nakaya, T and Yokoyama, M and Fukuda, Y and Itow, Y and Tanaka, T and Jung, CK and Lopez, G and McGrew, C and Yanagisawa, C and Tamura, N and Idehara, Y and Sakuda, M and Kuno, Y and Yoshida, M and Kim,
SB and Yang, BS and Okazawa, H and Choi, Y and Seo, HK and Furuse, Y and Nishijima, K and Yokosawa, Y and Koshiba, M and Totsuka, Y and Vagins,
MR and Chen, S and Heng, Y},
Title = {Search for nucleon decay into charged antilepton plus meson
in Super-Kamiokande i and II},
Journal = {Physical Review D - Particles, Fields, Gravitation and
Cosmology},
Volume = {85},
Number = {11},
Pages = {112001},
Publisher = {American Physical Society (APS)},
Year = {2012},
Month = {June},
ISSN = {1550-7998},
url = {http://arxiv.org/pdf/1203.4030},
Abstract = {Searches for a nucleon decay into a charged antilepton (e +
or μ +) plus a light meson (π0, π -, η, ρ0, ρ -, ω)
were performed using the Super-Kamiokande I and II data.
Twelve nucleon decay modes were searched for. The total
exposure is 140.9kiloton•years, which includes a
91.7kiloton•year exposure (1489.2 live days) of
Super-Kamiokande-I and a 49.2kiloton•year exposure (798.6
live days) of Super-Kamiokande II. The number of candidate
events in the data was consistent with the atmospheric
neutrino background expectation. No significant evidence for
a nucleon decay was observed in the data. Thus, lower limits
on the nucleon partial lifetime at 90% confidence level were
obtained. The limits range from 3.6×1031 to 8.2×1033years,
depending on the decay modes. © 2012 American Physical
Society.},
Doi = {10.1103/PhysRevD.85.112001},
Key = {:2012rv}
}
@article{Regis:2012sn,
Author = {Regis, C and Abe, K and Hayato, Y and Iyogi, K and Kameda, J and Koshio, Y and Marti, L and Miura, M and Moriyama, S and Nakahata, M and Nakayama, S and Obayashi, Y and Sekiya, H and Shiozawa, M and Suzuki, Y and Takeda, A and Takenaga, Y and Ueno, K and Yokozawa, T and Kaji, H and Kajita, T and Kaneyuki, K and Lee, KP and Okumura, K and McLachlan, T and Labarga, L and Kearns, E and Raaf, JL and Stone, JL and Sulak, LR and Goldhaber, M and Bays, K and Carminati, G and Kropp, WR and Mine, S and Renshaw, A and Smy,
MB and Sobel, HW and Ganezer, KS and Hill, J and Keig, WE and Jang, JS and Kim, JY and Lim, IT and Albert, JB and Scholberg, K and Walter, CW and Wendell, RA and Wongjirad, T and Ishizuka, T and Tasaka, S and Learned,
JG and Matsuno, S and Smith, SN and Hasegawa, T and Ishida, T and Ishii, T and Kobayashi, T and Nakadaira, T and Nakamura, K and Nishikawa, K and Oyama, Y and Sakashita, K and Sekiguchi, T and Tsukamoto, T and Suzuki,
AT and Takeuchi, Y and Ieki, K and Ikeda, M and Kubo, H and Minamino, A and Murakami, A and Nakaya, T and Fukuda, Y and Choi, K and Itow, Y and Mitsuka, G and Miyake, M and Mijakowski, P and Hignight, J and Imber, J and Jung, CK and Taylor, I and Yanagisawa, C and Ishino, H and Kibayashi, A and Mori, T and Sakuda, M and Takeuchi, J and Kuno, Y and Kim, SB and Okazawa,
H and Choi, Y and Nishijima, K and Koshiba, M and Totsuka, Y and Yokoyama,
M and Martens, K and Vagins, MR and Chen, S},
Title = {Search for proton decay via p→μ+K0 in Super-Kamiokande I,
II, and III},
Journal = {Physical Review D - Particles, Fields, Gravitation and
Cosmology},
Volume = {86},
Number = {1},
Pages = {012006},
Publisher = {American Physical Society (APS)},
Year = {2012},
Month = {July},
ISSN = {1550-7998},
url = {http://arxiv.org/pdf/1205.6538},
Abstract = {We have searched for proton decay via p→μ +K0 using data
from a 91.7kiloton•year exposure of Super-Kamiokande- I, a
49.2kiloton•year exposure of Super-Kamiokande II, and a
31.9kiloton•year exposure of Super-Kamiokande III. The
number of candidate events in the data was consistent with
the atmospheric neutrino background expectation and no
evidence for proton decay in this mode was found. We set a
partial lifetime lower limit of 1.6×1033years at the 90%
confidence level. © 2012 American Physical
Society.},
Doi = {10.1103/PhysRevD.86.012006},
Key = {Regis:2012sn}
}
@article{Ueno:2012md,
Author = {Ueno, K and Abe, K and Hayato, Y and Iida, T and Iyogi, K and Kameda, J and Koshio, Y and Kozuma, Y and Miura, M and Moriyama, S and Nakahata, M and Nakayama, S and Obayashi, Y and Sekiya, H and Shiozawa, M and Suzuki, Y and Takeda, A and Takenaga, Y and Ueshima, K and Yamada, S and Yokozawa, T and Martens, K and Schuemann, J and Vagins, M and Ishihara, C and Kaji, H and Kajita, T and Kaneyuki, K and McLachlan, T and Okumura, K and Shimizu,
Y and Tanimoto, N and Kearns, E and Litos, M and Raaf, JL and Stone, JL and Sulak, LR and Bays, K and Kropp, WR and Mine, S and Regis, C and Renshaw,
A and Smy, MB and Sobel, HW and Ganezer, KS and Hill, J and Keig, WE and Jang,
JS and Kim, JY and Lim, IT and Albert, JB and Scholberg, K and Walter, CW and Wendell, R and Wongjirad, T and Ishizuka, T and Tasaka, S and Learned,
JG and Matsuno, S and Hasegawa, T and Ishida, T and Ishii, T and Kobayashi,
T and Nakadaira, T and Nakamura, K and Nishikawa, K and Oyama, Y and Sakashita, K and Sekiguchi, T and Tsukamoto, T and Suzuki, AT and Takeuchi, Y and Ikeda, M and Minamino, A and Nakaya, T and Labarga, L and Marti, L and Fukuda, Y and Itow, Y and Mitsuka, G and Tanaka, T and Jung,
CK and Lopez, G and Taylor, I and Yanagisawa, C and Ishino, H and Kibayashi, A and Mino, S and Mori, T and Sakuda, M and Toyota, H and Kuno,
Y and Yoshida, M and Kim, SB and Yang, BS and Okazawa, H and Choi, Y and Nishijima, K and Koshiba, M and Totsuka, Y},
Title = {Search for GUT monopoles at Super-Kamiokande},
Journal = {Astroparticle Physics},
Volume = {36},
Number = {1},
Pages = {131-136},
Publisher = {Elsevier BV},
Year = {2012},
Month = {August},
ISSN = {0927-6505},
url = {http://arxiv.org/pdf/1203.0940},
Abstract = {GUT monopoles captured by the Sun's gravitation are expected
to catalyze proton decays via the Callan-Rubakov process. In
this scenario, protons, which initially decay into pions,
will ultimately produce νe, νμ and ν̄ μ. After
undergoing neutrino oscillation, all neutrino species appear
when they arrive at the Earth, and can be detected by a
50,000 metric ton Water Cherenkov detector, Super-Kamiokande
(SK). A search for low energy neutrinos in the electron
total energy range from 19 to 55 MeV was carried out with SK
and gives a monopole flux limit of F M( σ0/1mb)<6.3×10
-24( βM/10 -3) 2cm- 2s- 1sr- 1 at 90% C.L., where βM is
the monopole velocity in units of the speed of light and σ0
is the catalysis cross section at βM=1. The obtained limit
is several orders of magnitude more stringent than the
current best cosmic-ray supermassive monopole flux limit for
βM<10 -2 and also two orders of magnitude lower than the
result of the Kamiokande experiment, which used a similar
detection method.© 2012 Elsevier B.V. All rights
reserved.},
Doi = {10.1016/j.astropartphys.2012.05.008},
Key = {Ueno:2012md}
}
@article{Abe:2013fuq,
Author = {Abe, K and others},
Title = {Measurement of Neutrino Oscillation Parameters from Muon
Neutrino Disappearance with an Off-axis Beam},
Journal = {Phys. Rev. Lett.},
Volume = {111},
Number = {21},
Pages = {211803-211803},
Year = {2013},
url = {http://arxiv.org/abs/1308.0465v2},
Abstract = {The T2K Collaboration reports a precision measurement of
muon neutrino disappearance with an off-axis neutrino beam
with a peak energy of 0.6 GeV. Near detector measurements
are used to constrain the neutrino flux and cross section
parameters. The Super-Kamiokande far detector, which is 295
km downstream of the neutrino production target, collected
data corresponding to 3.01×10(20) protons on target. In the
absence of neutrino oscillations, 205±17 (syst) events are
expected to be detected while only 58 muon neutrino event
candidates are observed. A fit to the neutrino rate and
energy spectrum, assuming three neutrino flavors and normal
mass hierarchy yields a best-fit mixing angle
sin2(θ23)=0.514±0.082 and mass splitting
|Δm(32)(2)|=2.44(-0.15)(+0.17)×10(-3) eV2/c4. Our result
corresponds to the maximal oscillation disappearance
probability.},
Doi = {10.1103/PhysRevLett.111.211803},
Key = {Abe:2013fuq}
}
@article{Kearns:2013lea,
Author = {Kearns, E and others},
Title = {Hyper-Kamiokande Physics Opportunities},
Journal = {Proceedings, 2013 Community Summer Study on the Future of
U.S. Particle Physics: Snowmass on the Mississippi
(CSS2013): Minneapolis, MN, USA, July 29-August 6,
2013},
Year = {2013},
url = {http://arxiv.org/pdf/1309.0184},
Abstract = {http://arxiv.org/abs/1309.0184},
Key = {Kearns:2013lea}
}
@article{fds347833,
Author = {Adams, C and others},
Title = {The Long-Baseline Neutrino Experiment: Exploring Fundamental
Symmetries of the Universe},
Journal = {Snowmass 2013: Workshop on Energy Frontier Seattle, USA,
June 30-July 3, 2013},
Year = {2013},
Key = {fds347833}
}
@article{fds337613,
Author = {Choi, K and Abe, K and Haga, Y and Hayato, Y and Iyogi, K and Kameda, J and Kishimoto, Y and Miura, M and Moriyama, S and Nakahata, M and Nakano, Y and Nakayama, S and Sekiya, H and Shiozawa, M and Suzuki, Y and Takeda, A and Tomura, T and Wendell, RA and Irvine, T and Kajita, T and Kametani, I and Kaneyuki, K and Lee, KP and Nishimura, Y and Okumura, K and McLachlan,
T and Labarga, L and Kearns, E and Raaf, JL and Stone, JL and Sulak, LR and Berkman, S and Tanaka, HA and Tobayama, S and Goldhaber, M and Carminati, G and Kropp, WR and Mine, S and Renshaw, A and Smy, MB and Sobel, HW and Ganezer, KS and Hill, J and Hong, N and Kim, JY and Lim, IT and Akiri, T and Himmel, A and Scholberg, K and Walter, CW and Wongjirad, T and Ishizuka, T and Tasaka, S and Jang, JS and Learned, JG and Matsuno, S and Smith, SN and Hasegawa, T and Ishida, T and Ishii, T and Kobayashi, T and Nakadaira, T and Nakamura, K and Oyama, Y and Sakashita, K and Sekiguchi, T and Tsukamoto, T and Suzuki, AT and Takeuchi, Y and Bronner, C and Hirota, S and Huang, K and Ieki, K and Ikeda, M and Kikawa,
H and Minamino, A and Nakaya, T and Suzuki, K and Takahashi, S and Fukuda,
Y and Itow, Y and Mitsuka, G and Mijakowski, P and Hignight, J and Imber,
J and Jung, CK and Yanagisawa, C and Ishino, H and Kibayashi, A and Koshio,
Y and Mori, T and Sakuda, M and Yano, T and Kuno, Y and Tacik, R and Kim, SB and Okazawa, H and Choi, Y and Nishijima, K and Koshiba,
M},
Title = {Search for light WIMP captured in the Sun using contained
events in Super-Kamiokande},
Journal = {Proceedings of the 33rd International Cosmic Rays
Conference, ICRC 2013},
Volume = {2013-October},
Year = {2013},
Month = {January},
ISBN = {9788589064293},
Abstract = {Super-Kamiokande can search for dark matter by detecting
neutrinos and muons which are produced by WIMP pair
annihilations occur inside the Sun. The huge gravity and
hydrogen-rich composition of the Sun combined with high
sensitivity of Super-Kamiokande for low energy(few GeV)
neutrinos allow us good sensitivity to light(few GeV to few
10 GeV) WIMP dark matter, especially for spin-dependent
coupling case. In this analysis, we increased signal
acceptance by using fully-contained and partially-contained
neutrino events added to up-going muons in Super-Kamiokande.
We also used minimum χ2 method to use energy, direction and
flavor informations. We fitted Super-Kamiokande I-IV data to
find the allowed contribution of WIMP-induced neutrino
events added to large back-ground of atmospheric neutrino
events. As a result, we found no signal observed and the
null result was interpreted as upper limit on the
spin-dependent (SD) WIMP-proton elastic scattering
cross-section for χχ → bb¯ and χχ → τ+τ− WIMP
annihilation channels. We set current best limit for WIMP
mass below 100 GeV.},
Key = {fds337613}
}
@article{Abe:2012av,
Author = {Abe, K and Abgrall, N and Aihara, H and Akiri, T and Albert, JB and Andreopoulos, C and Aoki, S and Ariga, A and Ariga, T and Assylbekov, S and Autiero, D and Barbi, M and Barker, GJ and Barr, G and Bass, M and Batkiewicz, M and Bay, F and Bentham, SW and Berardi, V and Berger, BE and Berkman, S and Bertram, I and Beznosko, D and Bhadra, S and Blaszczyk,
FDM and Blondel, A and Bojechko, C and Boyd, S and Bravar, A and Bronner,
C and Brook-Roberge, DG and Buchanan, N and Calland, RG and Caravaca
Rodríguez, J and Cartwright, SL and Castillo, R and Catanesi, MG and Cervera, A and Cherdack, D and Christodoulou, G and Clifton, A and Coleman, J and Coleman, SJ and Collazuol, G and Connolly, K and Curioni,
A and Dabrowska, A and Danko, I and Das, R and Davis, S and Day, M and De
André, JPAM and De Perio and P and De Rosa and G and Dealtry, T and Densham,
C and Di Lodovico and F and Di Luise and S and Dobson, J and Duboyski, T and Dufour, F and Dumarchez, J and Dytman, S and Dziewiecki, M and Dziomba,
M and Emery, S and Ereditato, A and Escudero, L and Esposito, LS and Finch,
AJ and Frank, E and Friend, M and Fujii, Y and Fukuda, Y and Galymov, V and Gaudin, A and Giffin, S and Giganti, C and Gilje, K and Golan, T and Gomez-Cadenas, JJ and Gonin, M and Grant, N and Gudin, D and Guzowski,
P and Hadley, DR and Haesler, A and Haigh, MD and Hansen, D and Hara, T and Hartz, M and Hasegawa, T and Hastings, NC and Hayato, Y and Hearty, C and Helmer, RL and Hignight, J and Hillairet, A and Himmel, A and Hiraki,
T},
Title = {T2K neutrino flux prediction},
Journal = {Physical Review D - Particles, Fields, Gravitation and
Cosmology},
Volume = {87},
Number = {1},
Pages = {012001},
Publisher = {American Physical Society (APS)},
Year = {2013},
Month = {January},
url = {http://arxiv.org/abs/1211.0469v3},
Abstract = {The Tokai-to-Kamioka (T2K) experiment studies neutrino
oscillations using an off-axis muon neutrino beam with a
peak energy of about 0.6 GeV that originates at the Japan
Proton Accelerator Research Complex accelerator facility.
Interactions of the neutrinos are observed at near detectors
placed at 280 m from the production target and at the far
detector - Super-Kamiokande - located 295 km away. The flux
prediction is an essential part of the successful prediction
of neutrino interaction rates at the T2K detectors and is an
important input to T2K neutrino oscillation and cross
section measurements. A FLUKA and GEANT3-based simulation
models the physical processes involved in the neutrino
production, from the interaction of primary beam protons in
the T2K target, to the decay of hadrons and muons that
produce neutrinos. The simulation uses proton beam monitor
measurements as inputs. The modeling of hadronic
interactions is reweighted using thin target hadron
production data, including recent charged pion and kaon
measurements from the NA61/SHINE experiment. For the first
T2K analyses the uncertainties on the flux prediction are
evaluated to be below 15% near the flux peak. The
uncertainty on the ratio of the flux predictions at the far
and near detectors is less than 2% near the flux peak. ©
2013 American Physical Society.},
Doi = {10.1103/PhysRevD.87.012001},
Key = {Abe:2012av}
}
@article{fds248715,
Author = {Abe, K and Abgrall, N and Aihara, H and Akiri, T and Albert, JB and Andreopoulos, C and Aoki, S and Ariga, A and Ariga, T and Assylbekov, S and Autiero, D and Barbi, M and Barker, GJ and Barr, G and Bass, M and Batkiewicz, M and Bay, F and Bentham, SW and Berardi, V and Berger, BE and Berkman, S and Bertram, I and Beznosko, D and Bhadra, S and Blaszczyk,
FDM and Blondel, A and Bojechko, C and Boyd, S and Bravar, A and Bronner,
C and Brook-Roberge, DG and Buchanan, N and Calland, RG and Caravaca
Rodriguez, J and Cartwright, SL and Castillo, R and Catanesi, MG and Cervera, A and Cherdack, D and Christodoulou, G and Clifton, A and Coleman, J and Coleman, SJ and Collazuol, G and Connolly, K and Curioni,
A and Dabrowska, A and Danko, I and Das, R and Davis, S and Day, M and De
Andre, JPAM and De Perio and P and De Rosa and G and Dealtry, T and Densham,
C and Di Lodovico and F and Di Luise and S and Dobson, J and Duboyski, T and Dufour, F and Dumarchez, J and Dytman, S and Dziewiecki, M and Dziomba,
M and Emery, S and Ereditato, A and Escudero, L and Esposito, LS and Finch,
AJ and Frank, E and Friend, M and Fujii, Y and Fukuda, Y and Galymov, V and Gaudin, A and Giffin, S and Giganti, C and Gilje, K and Golan, T and Gomez-Cadenas, JJ and Gonin, M and Grant, N and Gudin, D and Guzowski,
P and Hadley, DR and Haesler, A and Haigh, MD and Hansen, D and Hara, T and Hartz, M and Hasegawa, T and Hastings, NC and Hayato, Y and Hearty, C and Helmer, RL and Hignight, J and Hillairet, A and Himmel, A and Hiraki,
T},
Title = {Publisher's Note: T2K neutrino flux prediction},
Journal = {Physical Review D - Particles, Fields, Gravitation and
Cosmology},
Volume = {87},
Number = {1},
Publisher = {American Physical Society (APS)},
Year = {2013},
Month = {January},
ISSN = {1550-7998},
url = {http://gateway.webofknowledge.com/gateway/Gateway.cgi?GWVersion=2&SrcApp=PARTNER_APP&SrcAuth=LinksAMR&KeyUT=WOS:000314229300009&DestLinkType=FullRecord&DestApp=ALL_WOS&UsrCustomerID=47d3190e77e5a3a53558812f597b0b92},
Doi = {10.1103/PhysRevD.87.019902},
Key = {fds248715}
}
@article{Abe:2012jj,
Author = {Abe, K and Hayato, Y and Iida, T and Iyogi, K and Kameda, J and Koshio, Y and Kozuma, Y and Marti, L and Miura, M and Moriyama, S and Nakahata, M and Nakayama, S and Obayashi, Y and Sekiya, H and Shiozawa, M and Suzuki, Y and Takeda, A and Takenaga, Y and Ueno, K and Ueshima, K and Yamada, S and Yokozawa, T and Ishihara, C and Kaji, H and Kajita, T and Kaneyuki, K and Lee, KP and McLachlan, T and Okumura, K and Shimizu, Y and Tanimoto, N and Labarga, L and Kearns, E and Litos, M and Raaf, JL and Stone, JL and Sulak,
LR and Goldhaber, M and Bays, K and Kropp, WR and Mine, S and Regis, C and Renshaw, A and Smy, MB and Sobel, HW and Ganezer, KS and Hill, J and Keig,
WE and Jang, JS and Kim, JY and Lim, IT and Albert, JB and Scholberg, K and Walter, CW and Wendell, R and Wongjirad, TM and Ishizuka, T and Tasaka,
S and Learned, JG and Matsuno, S and Smith, SN and Hasegawa, T and Ishida,
T and Ishii, T and Kobayashi, T and Nakadaira, T and Nakamura, K and Nishikawa, K and Oyama, Y and Sakashita, K and Sekiguchi, T and Tsukamoto, T and Suzuki, AT and Takeuchi, Y and Ikeda, M and Minamino,
A and Nakaya, T and Fukuda, Y and Itow, Y and Mitsuka, G and Tanaka, T and Jung, CK and Lopez, GD and Taylor, I and Yanagisawa, C and Ishino, H and Kibayashi, A and Mino, S and Mori, T and Sakuda, M and Toyota, H and Kuno,
Y and Yoshida, M and Kim, SB and Yang, BS and Okazawa, H and Choi, Y and Nishijima, K and Koshiba, M and Yokoyama, M and Totsuka, Y and Martens,
K and Schuemann, J and Vagins, MR and Chen, S and Heng, Y and Yang, Z and Zhang, H and Kielczewska, D and Mijakowski, P and Connolly, K and Dziomba, M and Thrane, E and Wilkes, RJ and Super-Kamiokande
Collaboration},
Title = {Evidence for the appearance of atmospheric tau neutrinos in
super-Kamiokande.},
Journal = {Physical review letters},
Volume = {110},
Number = {18},
Pages = {181802},
Year = {2013},
Month = {May},
url = {http://www.ncbi.nlm.nih.gov/pubmed/23683190},
Abstract = {Super-Kamiokande atmospheric neutrino data were fit with an
unbinned maximum likelihood method to search for the
appearance of tau leptons resulting from the interactions of
oscillation-generated tau neutrinos in the detector.
Relative to the expectation of unity, the tau normalization
is found to be 1.42 ± 0.35(stat)(-0.12)(+0.14)(syst)
excluding the no-tau-appearance hypothesis, for which the
normalization would be zero, at the 3.8σ level. We estimate
that 180.1 ± 44.3(stat)(-15.2)(+17.8) (syst) tau leptons
were produced in the 22.5 kton fiducial volume of the
detector by tau neutrinos during the 2806 day running
period. In future analyses, this large sample of selected
tau events will allow the study of charged current tau
neutrino interaction physics with oscillation produced tau
neutrinos.},
Doi = {10.1103/physrevlett.110.181802},
Key = {Abe:2012jj}
}
@article{Abe:2013jth,
Author = {Abe, K and Abgrall, N and Aihara, H and Akiri, T and Albert, JB and Andreopoulos, C and Aoki, S and Ariga, A and Ariga, T and Assylbekov, S and Autiero, D and Barbi, M and Barker, GJ and Barr, G and Bass, M and Batkiewicz, M and Bay, F and Bentham, SW and Berardi, V and Berger, BE and Berkman, S and Bertram, I and Beznosko, D and Bhadra, S and Blaszczyk,
FDM and Blondel, A and Bojechko, C and Boyd, S and Brailsford, D and Bravar, A and Bronner, C and Brook-Roberge, DG and Buchanan, N and Calland, RG and Caravaca Rodríguez and J and Cartwright, SL and Castillo, R and Catanesi, MG and Cervera, A and Cherdack, D and Christodoulou, G and Clifton, A and Coleman, J and Coleman, SJ and Collazuol, G and Connolly, K and Cremonesi, L and Curioni, A and Dabrowska, A and Danko, I and Das, R and Davis, S and Day, M and De André,
JPAM and De Perio and P and De Rosa and G and Dealtry, T and Dennis, SR and Densham, C and Di Lodovico and F and Di Luise and S and Dobson, J and Drapier,
O and Duboyski, T and Dufour, F and Dumarchez, J and Dytman, S and Dziewiecki, M and Dziomba, M and Emery, S and Ereditato, A and Escudero,
L and Finch, AJ and Frank, E and Friend, M and Fujii, Y and Fukuda, Y and Furmanski, AP and Galymov, V and Gaudin, A and Giffin, S and Giganti, C and Gilje, K and Golan, T and Gomez-Cadenas, JJ and Gonin, M and Grant, N and Gudin, D and Guzowski, P and Hadley, DR and Haesler, A and Haigh, MD and Hamilton, P and Hansen, D and Hara, T and Hartz, M and Hasegawa, T and Hastings, NC and Hayato, Y and Hearty, C},
Title = {Measurement of the inclusive νμ charged current
cross section on carbon in the near detector of the T2K
experiment},
Journal = {Physical Review D - Particles, Fields, Gravitation and
Cosmology},
Volume = {87},
Number = {9},
Pages = {092003},
Publisher = {American Physical Society (APS)},
Year = {2013},
Month = {May},
url = {http://arxiv.org/abs/1302.4908v2},
Abstract = {T2K has performed the first measurement of νμ inclusive
charged current interactions on carbon at neutrino energies
of ∼1 GeV where the measurement is reported as a
flux-averaged double differential cross section in muon
momentum and angle. The flux is predicted by the beam Monte
Carlo and external data, including the results from the
NA61/SHINE experiment. The data used for this measurement
were taken in 2010 and 2011, with a total of 10.8×1019
protons-on-target. The analysis is performed on 4485
inclusive charged current interaction candidates selected in
the most upstream fine-grained scintillator detector of the
near detector. The flux-averaged total cross section is
σCC=(6.91±0.13(stat)±0.84(syst) )×10-39 cm2nucleon for a
mean neutrino energy of 0.85 GeV. © 2013 American Physical
Society.},
Doi = {10.1103/PhysRevD.87.092003},
Key = {Abe:2013jth}
}
@article{Abe:2013xua,
Author = {Abe, K and Abgrall, N and Aihara, H and Akiri, T and Albert, JB and Andreopoulos, C and Aoki, S and Ariga, A and Ariga, T and Assylbekov, S and Autiero, D and Barbi, M and Barker, GJ and Barr, G and Bass, M and Batkiewicz, M and Bay, F and Bentham, SW and Berardi, V and Berger, BE and Berkman, S and Bertram, I and Beznosko, D and Bhadra, S and Blaszczyk,
FDM and Blondel, A and Bojechko, C and Boyd, S and Brailsford, D and Bravar, A and Bronner, C and Brook-Roberge, DG and Buchanan, N and Calland, RG and Caravaca Rodríguez and J and Cartwright, SL and Castillo, R and Catanesi, MG and Cervera, A and Cherdack, D and Christodoulou, G and Clifton, A and Coleman, J and Coleman, SJ and Collazuol, G and Connolly, K and Cremonesi, L and Curioni, A and Dabrowska, A and Danko, I and Das, R and Davis, S and Day, M and De André,
JPAM and De Perio and P and De Rosa and G and Dealtry, T and Dennis, S and Densham, C and Di Lodovico and F and Di Luise and S and Dobson, J and Drapier,
O and Duboyski, T and Dufour, F and Dumarchez, J and Dytman, S and Dziewiecki, M and Dziomba, M and Emery, S and Ereditato, A and Escudero,
L and Finch, AJ and Frank, E and Friend, M and Fujii, Y and Fukuda, Y and Furmanski, A and Galymov, V and Gaudin, A and Giffin, S and Giganti, C and Gilje, K and Golan, T and Gomez-Cadenas, JJ and Gonin, M and Grant, N and Gudin, D and Hadley, DR and Haesler, A and Haigh, MD and Hamilton, P and Hansen, D and Hara, T and Hartz, M and Hasegawa, T and Hastings, NC and Hayato, Y and Hearty, C and Helmer, RL},
Title = {Evidence of electron neutrino appearance in a muon neutrino
beam},
Journal = {Physical Review D - Particles, Fields, Gravitation and
Cosmology},
Volume = {88},
Number = {3},
Pages = {032002},
Publisher = {American Physical Society (APS)},
Year = {2013},
Month = {August},
url = {http://arxiv.org/abs/1304.0841v2},
Abstract = {The T2K Collaboration reports evidence for electron neutrino
appearance at the atmospheric mass splitting,
|Δm322|≈2.4×10-3 eV2. An excess of electron neutrino
interactions over background is observed from a muon
neutrino beam with a peak energy of 0.6 GeV at the
Super-Kamiokande (SK) detector 295 km from the beam's
origin. Signal and background predictions are constrained by
data from near detectors located 280 m from the neutrino
production target. We observe 11 electron neutrino candidate
events at the SK detector when a background of
3.3±0.4(syst) events is expected. The background-only
hypothesis is rejected with a p value of 0.0009 (3.1σ), and
a fit assuming νμ→νe oscillations with sinâ¡22θ23=1,
δCP=0 and |Δm322|=2.4×10-3 eV2 yields
sinâ¡22θ13=0.088-0.039+0. 049(stat+syst). © 2013
American Physical Society.},
Doi = {10.1103/PhysRevD.88.032002},
Key = {Abe:2013xua}
}
@article{deGouvea:2013onf,
Author = {Gouvea, AD and Pitts, K and Scholberg, K and Zeller, GP and Alonso, J and Bernstein, A and Bishai, M and Elliott, S and Heeger, K and Hoffman, K and Huber, P and Kaufman, LJ and Kayser, B and Link, J and Lunardini, C and Monreal, B and Morfin, JG and Robertson, H and Tayloe, R and Tolich, N and Abazajian, K and Akiri, T and Albright, C and Asaadi, J and Babu, KS and Balantekin, AB and Barbeau, P and Bass, M and Blake, A and Blondel, A and Blucher, E and Bowden, N and Brice, SJ and Bross, A and Carls, B and Cavanna, F and Choudhary, B and Coloma, P and Connolly, A and Conrad, J and Convery, M and Cooper, RL and Cowen, D and Motta, HD and Young, TD and Lodovico, FD and Diwan, M and Djurcic, Z and Dracos, M and Dodelson, S and Efremenko, Y and Ekelof, T and Feng, JL and Fleming, B and Formaggio, J and Friedland, A and Fuller, G and Gallagher, H and Geer, S and Gilchriese,
M and Goodman, M and Grant, D and Gratta, G and Hall, C and Halzen, F and Harris, D and Heffner, M and Henning, R and Hewett, JL and Hill, R and Himmel, A and Horton-Smith, G and Karle, A and Katori, T and Kearns, E and Kettell, S and Klein, J and Kim, Y and Kim, YK and Kolomensky, Y and Kordosky, M and Kudenko, Y and Kudryavtsev, VA and Lande, K and Lang, K and Lanza, R and Lau, K and Lee, H and Li, Z and Littlejohn, BR and Lin, CJ and Liu, D and Liu, H and Long, K and Louis, W and Luk, KB and Marciano, W and Mariani, C and Marshak, M and Mauger, C and McDonald, KT and McFarland,
K and McKeown, R and Messier, M and Mishra, SR and Mosel, U and Mumm, P and Nakaya, T and Nelson, JK and Nygren, D and Gann, GDO and Osta, J and Palamara, O and Paley, J and Papadimitriou, V and Parke, S and Parsa, Z and Patterson, R and Piepke, A and Plunkett, R and Poon, A and Qian, X and Raaf, J and Rameika, R and Ramsey-Musolf, M and Rebel, B and Roser, R and Rosner, J and Rott, C and Rybka, G and Sahoo, H and Sangiorgio, S and Schmitz, D and Shrock, R and Shaevitz, M and Smith, N and Smy, M and Sobel,
H and Sorensen, P and Sousa, A and Spitz, J and Strauss, T and Svoboda, R and Tanaka, HA and Thomas, J and Tian, X and Tschirhart, R and Tully, C and Bibber, KV and Water, RGVD and Vahle, P and Vogel, P and Walter, CW and Wark, D and Wascko, M and Webber, D and Weerts, H and White, C and White,
H and Whitehead, L and Wilson, RJ and Winslow, L and Wongjirad, T and Worcester, E and Yokoyama, M and Yoo, J and Zimmerman,
ED},
Title = {Neutrinos},
Year = {2013},
Month = {October},
url = {http://arxiv.org/pdf/1310.4340},
Abstract = {This document represents the response of the Intensity
Frontier Neutrino Working Group to the Snowmass charge. We
summarize the current status of neutrino physics and
identify many exciting future opportunities for studying the
properties of neutrinos and for addressing important physics
and astrophysics questions with neutrinos.},
Key = {deGouvea:2013onf}
}
@article{fds248700,
Author = {Abe, K and others},
Title = {Measurement of the Inclusive Electron Neutrino Charged
Current Cross Section on Carbon with the T2K Near
Detector},
Journal = {Phys. Rev. Lett.},
Volume = {113},
Number = {24},
Pages = {241803-241803},
Year = {2014},
ISSN = {0031-9007},
url = {http://dx.doi.org/10.1103/PhysRevLett.113.241803},
Abstract = {The T2K off-axis near detector ND280 is used to make the
first differential cross-section measurements of electron
neutrino charged current interactions at energies
∼1 GeV as a function of electron momentum, electron
scattering angle, and four-momentum transfer of the
interaction. The total flux-averaged ν(e) charged current
cross section on carbon is measured to be
⟨σ⟩(ϕ)=1.11±0.10(stat)±0.18(syst)×10⁻³⁸
cm²/nucleon. The differential and total cross-section
measurements agree with the predictions of two leading
neutrino interaction generators, NEUT and GENIE. The NEUT
prediction is 1.23×10⁻³⁸ cm²/nucleon and the GENIE
prediction is 1.08×10⁻³⁸ cm²/nucleon. The total ν(e)
charged current cross-section result is also in agreement
with data from the Gargamelle experiment.},
Doi = {10.1103/PhysRevLett.113.241803},
Key = {fds248700}
}
@article{Abe:2014dyd,
Author = {Abe, K and others},
Title = {Measurement of the neutrino-oxygen neutral-current
interaction cross section by observing nuclear deexcitation
γ rays},
Journal = {Phys. Rev.},
Volume = {D90},
Number = {7},
Pages = {072012-072012},
Year = {2014},
ISSN = {1550-7998},
url = {http://arxiv.org/pdf/1403.3140},
Abstract = {We report the first measurement of the neutrino-oxygen
neutral-current quasielastic (NCQE) cross section. It is
obtained by observing nuclear deexcitation γ rays which
follow neutrino-oxygen interactions at the Super-Kamiokande
water Cherenkov detector. We use T2K data corresponding to
3.01×1020 protons on target. By selecting only events
during the T2K beam window and with well-reconstructed
vertices in the fiducial volume, the large background rate
from natural radioactivity is dramatically reduced. We
observe 43 events in the 4-30 MeV reconstructed energy
window, compared with an expectation of 51.0, which includes
an estimated 16.2 background events. The background is
primarily nonquasielastic neutral-current interactions and
has only 1.2 events from natural radioactivity. The
flux-averaged NCQE cross section we measure is
1.55×10-38cm2 with a 68% confidence interval of
(1.22,2.20)×10-38cm2 at a median neutrino energy of 630
MeV, compared with the theoretical prediction of
2.01×10-38cm2.},
Doi = {10.1103/PhysRevD.90.072012},
Key = {Abe:2014dyd}
}
@article{fds248702,
Author = {Abe, K and others},
Title = {Search for proton decay via $p\toννK^+$ using 260
kiloton·year data of Super-Kamiokande},
Journal = {Phys. Rev.},
Volume = {D90},
Number = {7},
Pages = {072005-072005},
Publisher = {American Physical Society (APS)},
Year = {2014},
ISSN = {1550-7998},
url = {http://dx.doi.org/10.1103/PhysRevD.90.072005},
Abstract = {We have searched for proton decay via p→νK+ using
Super-Kamiokande data from April 1996 to February 2013,
260kiloton·year exposure in total. No evidence for this
proton decay mode is found. A lower limit of the proton
lifetime is set to τ/B(p→νK+)>5.9×1033 years at 90%
confidence level.},
Doi = {10.1103/PhysRevD.90.072005},
Key = {fds248702}
}
@article{Abe:2014nox,
Author = {Abe, K and others},
Title = {Measurement of the inclusive $ν_μ$ charged current cross
section on iron and hydrocarbon in the T2K on-axis neutrino
beam},
Journal = {Phys. Rev.},
Volume = {D90},
Number = {5},
Pages = {052010-052010},
Publisher = {American Physical Society (APS)},
Year = {2014},
ISSN = {1550-7998},
url = {http://arxiv.org/pdf/1407.4256},
Abstract = {We report a measurement of the νμ inclusive charged
current cross sections on iron and hydrocarbon in the
Tokai-to-Kamioka (T2K) on-axis neutrino beam. The measured
inclusive charged current cross sections on iron and
hydrocarbon averaged over the T2K on-axis flux with a mean
neutrino energy of 1.51 GeV are (1.444±0.002(stat)-0.157+0.189(syst))×10-38cm2/nucleon
and (1.379±0.009(stat)-0.147+0.178(syst))×10-38cm2/nucleon,
respectively, and their cross-section ratio is
1.047±0.007(stat)±0.035(syst). These results agree well
with the predictions of the neutrino interaction model, and
thus we checked the correct treatment of the nuclear effect
for iron and hydrocarbon targets in the model within the
measurement precisions.},
Doi = {10.1103/PhysRevD.90.052010},
Key = {Abe:2014nox}
}
@article{Abe:2014usb,
Author = {Abe, K and others},
Title = {Measurement of the intrinsic electron neutrino component in
the T2K neutrino beam with the ND280 detector},
Journal = {Phys. Rev.},
Volume = {D89},
Number = {9},
Pages = {092003-092003},
Publisher = {American Physical Society (APS)},
Year = {2014},
ISSN = {1550-7998},
url = {http://arxiv.org/pdf/1403.2552},
Abstract = {The T2K experiment has reported the first observation of the
appearance of electron neutrinos in a muon neutrino beam.
The main and irreducible background to the appearance signal
comes from the presence in the neutrino beam of a small
intrinsic component of electron neutrinos originating from
muon and kaon decays. In T2K, this component is expected to
represent 1.2% of the total neutrino flux. A measurement of
this component using the near detector (ND280), located 280
m from the target, is presented. The charged current
interactions of electron neutrinos are selected by combining
the particle identification capabilities of both the time
projection chambers and electromagnetic calorimeters of
ND280. The measured ratio between the observed electron
neutrino beam component and the prediction is 1.01±0.10
providing a direct confirmation of the neutrino fluxes and
neutrino cross section modeling used for T2K neutrino
oscillation analyses. Electron neutrinos coming from muons
and kaons decay are also separately measured, resulting in a
ratio with respect to the prediction of 0.68±0.30 and
1.10±0.14, respectively.},
Doi = {10.1103/PhysRevD.89.092003},
Key = {Abe:2014usb}
}
@article{Abe:2014ugx,
Author = {Abe, K and others},
Title = {Precise Measurement of the Neutrino Mixing Parameter θ_23
from Muon Neutrino Disappearance in an Off-Axis
Beam},
Journal = {Phys. Rev. Lett.},
Volume = {112},
Number = {18},
Pages = {181801-181801},
Year = {2014},
ISSN = {0031-9007},
url = {http://arxiv.org/pdf/1403.1532},
Abstract = {New data from the T2K neutrino oscillation experiment
produce the most precise measurement of the neutrino mixing
parameter θ23. Using an off-axis neutrino beam with a peak
energy of 0.6 GeV and a data set corresponding to
6.57×10(20) protons on target, T2K has fit the
energy-dependent νμ oscillation probability to determine
oscillation parameters. The 68% confidence limit on
sin(2)(θ23) is 0.514(-0.056)(+0.055) (0.511±0.055),
assuming normal (inverted) mass hierarchy. The best-fit
mass-squared splitting for normal hierarchy is
Δm32(2)=(2.51±0.10)×10(-3) eV(2)/c(4) (inverted
hierarchy: Δm13(2)=(2.48±0.10)×10(-3) eV(2)/c(4)).
Adding a model of multinucleon interactions that affect
neutrino energy reconstruction is found to produce only
small biases in neutrino oscillation parameter extraction at
current levels of statistical uncertainty.},
Doi = {10.1103/PhysRevLett.112.181801},
Key = {Abe:2014ugx}
}
@article{fds248710,
Author = {Litos, M and others},
Title = {Search for Dinucleon Decay into Kaons in
Super-Kamiokande},
Journal = {Phys. Rev. Lett.},
Volume = {112},
Number = {13},
Pages = {131803-131803},
Year = {2014},
ISSN = {0031-9007},
url = {http://dx.doi.org/10.1103/PhysRevLett.112.131803},
Abstract = {A search for the dinucleon decay pp → K+ K+ has been
performed using 91.6 kton·yr data from
Super-Kamiokande-I. This decay provides a sensitive probe of
the R-parity-violating parameter λ112''. A boosted decision
tree analysis found no signal candidates in the data. The
expected background was 0.28±0.19 atmospheric neutrino
induced events and the estimated signal detection efficiency
was 12.6%±3.2%. A lower limit of 1.7×10(32) years has
been placed on the partial lifetime of the decay O16 →
C14K+ K+ at 90% C.L. A corresponding upper limit of
7.8×10(-9) has been placed on the parameter
λ112''.},
Doi = {10.1103/PhysRevLett.112.131803},
Key = {fds248710}
}
@article{Renshaw:2013dzu,
Author = {Renshaw, A and others},
Title = {First Indication of Terrestrial Matter Effects on Solar
Neutrino Oscillation},
Journal = {Phys. Rev. Lett.},
Volume = {112},
Number = {9},
Pages = {091805-091805},
Year = {2014},
ISSN = {0031-9007},
url = {http://arxiv.org/pdf/1312.5176},
Abstract = {We report an indication that the elastic scattering rate of
solar B8 neutrinos with electrons in the Super-Kamiokande
detector is larger when the neutrinos pass through Earth
during nighttime. We determine the day-night asymmetry,
defined as the difference of the average day rate and
average night rate divided by the average of those two
rates, to be [-3.2 ± 1.1(stat) ± 0.5(syst)]%, which
deviates from zero by 2.7 σ. Since the elastic scattering
process is mostly sensitive to electron-flavored solar
neutrinos, a nonzero day-night asymmetry implies that the
flavor oscillations of solar neutrinos are affected by the
presence of matter within the neutrinos' flight path.
Super-Kamiokande's day-night asymmetry is consistent with
neutrino oscillations for 4 × 10(-5) eV(2) ≤ Δm 2(21)
≤ 7 × 10(-5) eV(2) and large mixing values of θ12, at
the 68% C.L.},
Doi = {10.1103/PhysRevLett.112.091805},
Key = {Renshaw:2013dzu}
}
@article{Abe:2013hdq,
Author = {Abe, K and others},
Title = {Observation of Electron Neutrino Appearance in a Muon
Neutrino Beam},
Journal = {Phys. Rev. Lett.},
Volume = {112},
Number = {6},
Pages = {061802-061802},
Year = {2014},
ISSN = {0031-9007},
url = {http://arxiv.org/pdf/1311.4750},
Abstract = {The T2K experiment has observed electron neutrino appearance
in a muon neutrino beam produced 295 km from the
Super-Kamiokande detector with a peak energy of 0.6 GeV. A
total of 28 electron neutrino events were detected with an
energy distribution consistent with an appearance signal,
corresponding to a significance of 7.3σ when compared to
4.92±0.55 expected background events. In the
Pontecorvo-Maki-Nakagawa-Sakata mixing model, the electron
neutrino appearance signal depends on several parameters
including three mixing angles θ12, θ23, θ13, a mass
difference Δm(32)(2) and a CP violating phase δ(CP). In
this neutrino oscillation scenario, assuming
|Δm(32)(2)|=2.4×10(-3) eV(2), sin(2)θ(23)=0.5, and
Δm322>0 (Δm(32)(2)<0), a best-fit value of
sin(2)2θ(13)=0.140(-0.032)(+0.038) (0.170(-0.037)(+0.045))
is obtained at δ(CP)=0. When combining the result with the
current best knowledge of oscillation parameters including
the world average value of θ(13) from reactor experiments,
some values of δ(CP) are disfavored at the 90%
C.L.},
Doi = {10.1103/PhysRevLett.112.061802},
Key = {Abe:2013hdq}
}
@article{fds248713,
Author = {Abe, K and others},
Title = {Recent Results from the T2K Experiment},
Journal = {Nucl. Phys. Proc. Suppl.},
Volume = {246-247},
Pages = {23-28},
Publisher = {Elsevier BV},
Year = {2014},
ISSN = {0920-5632},
url = {http://dx.doi.org/10.1016/j.nuclphysbps.2013.10.060},
Abstract = {The Tokai to Kamioka (T2K) experiment studies neutrino
oscillations using a beam of muon neutrinos produced by an
accelerator. The neutrinos travel from J-PARC on the east
coast of Japan and are detected 295 kilometers further away
in the Super-Kamiokande detector. A complex of near
detectors located 280 meters away from the neutrino
production target is used to better characterize the
neutrino beam and reduce systematic uncertainties. The
experiment aims at measuring electronic neutrino appearance
(νμ→νe oscillation) to measure the neutrino mixing
angle θ13, and muon neutrino disappearance to measure the
neutrino mixing angle θ23 and mass splitting |δm322|. We
report here electron neutrino appearance results using three
years of data, recorded until the 2012 summer, as well as
muon neutrino disappearance results based on the data coming
from the first two years of the experiment. © 2013 Elsevier
B.V.},
Doi = {10.1016/j.nuclphysbps.2013.10.060},
Key = {fds248713}
}
@article{Abe:2013gga,
Author = {Abe, K and others},
Title = {Calibration of the Super-Kamiokande Detector},
Journal = {Nucl. Instrum. Meth.},
Volume = {A737},
Pages = {253-272},
Publisher = {Elsevier BV},
Year = {2014},
url = {http://arxiv.org/abs/1307.0162v2},
Abstract = {Procedures and results on hardware-level detector
calibration in Super-Kamiokande (SK) are presented in this
paper. In particular, we report improvements made in our
calibration methods for the experimental phase IV in which
new readout electronics have been operating since 2008. The
topics are separated into two parts. The first part
describes the determination of constants needed to interpret
the digitized output of our electronics so that we can
obtain physical numbers such as photon counts and their
arrival times for each photomultiplier tube (PMT). In this
context, we developed an in situ procedure to determine
high-voltage settings for PMTs in large detectors like SK,
as well as a new method for measuring PMT quantum efficiency
and gain in such a detector. The second part describes
modeling of the detector in Monte Carlo simulations,
including, in particular, the optical properties of the
water target and their variability over time. Detailed
studies on water quality are also presented. As a result of
this work, we have achieved a precision sufficient for
physics analyses over a wide energy range (from a few MeV to
above 1 TeV). For example, charge determination was at the
level of 1%, and the timing resolution was 2.1 ns at the
one-photoelectron charge level and 0.5 ns at the
100-photoelectron charge level. © 2013 Elsevier
B.V.},
Doi = {10.1016/j.nima.2013.11.081},
Key = {Abe:2013gga}
}
@article{Agashe:2014kda,
Author = {Olive, KA and others},
Title = {Review of Particle Physics},
Journal = {Chin. Phys.},
Volume = {C38},
Number = {9},
Pages = {090001-090001},
Publisher = {IOP Publishing},
Year = {2014},
url = {http://dx.doi.org/10.1088/1674-1137/38/9/090001},
Abstract = {The Review summarizes much of particle physics and
cosmology. Using data from previous editions, plus 3,283 new
measurements from 899 papers, we list, evaluate, and average
measured properties of gauge bosons and the recently
discovered Higgs boson, leptons, quarks, mesons, and
baryons. We summarize searches for hypothetical particles
such as heavy neutrinos, supersymmetric and technicolor
particles, axions, dark photons, etc. All the particle
properties and search limits are listed in Summary Tables.
We also give numerous tables, figures, formulae, and reviews
of topics such as Supersymmetry, Extra Dimensions, Particle
Detectors, Probability, and Statistics. Among the 112
reviews are many that are new or heavily revised including
those on: Dark Energy, Higgs Boson Physics, Electroweak
Model, Neutrino Cross Section Measurements, Monte Carlo
Neutrino Generators, Top Quark, Dark Matter, Dynamical
Electroweak Symmetry Breaking, Accelerator Physics of
Colliders, High-Energy Collider Parameters, Big Bang
Nucleosynthesis, Astrophysical Constants and Cosmological
Parameters. A booklet is available containing the Summary
Tables and abbreviated versions of some of the other
sections of this full Review. All tables, listings, and
reviews (and errata) are also available on the Particle Data
Group website: http://pdg.Ibi.gov.},
Doi = {10.1088/1674-1137/38/9/090001},
Key = {Agashe:2014kda}
}
@article{Takhistov:2014pfw,
Author = {Takhistov, V and others},
Title = {Search for Trilepton Nucleon Decay via $p \rightarrow e^+ ν
ν$ and $p \rightarrow μ^+ ν ν$ in the Super-Kamiokande
Experiment},
Journal = {Phys. Rev. Lett.},
Volume = {113},
Pages = {101801-101801},
Year = {2014},
url = {http://arxiv.org/pdf/1409.1947},
Abstract = {http://arxiv.org/abs/1409.1947},
Doi = {10.1103/PhysRevLett.113.101801},
Key = {Takhistov:2014pfw}
}
@article{fds347831,
Author = {Abe, K and others},
Title = {A Long Baseline Neutrino Oscillation Experiment Using J-PARC
Neutrino Beam and Hyper-Kamiokande},
Year = {2014},
Key = {fds347831}
}
@article{fds326726,
Author = {Abe, K},
Title = {Publisher’s Note: Measurement of the intrinsic electron
neutrino component in the T2K neutrino beam with the ND280
detector [Phys. Rev. D 89, 092003 (2014)]},
Journal = {Physical Review D},
Volume = {89},
Number = {9},
Publisher = {American Physical Society (APS)},
Year = {2014},
Month = {May},
url = {http://dx.doi.org/10.1103/physrevd.89.099902},
Doi = {10.1103/physrevd.89.099902},
Key = {fds326726}
}
@article{fds248706,
Author = {Abe, K and Hayato, Y and Iida, T and Iyogi, K and Kameda, J and Koshio, Y and Kozuma, Y and Marti, L and Miura, M and Moriyama, S and Nakahata, M and Nakayama, S and Obayashi, Y and Sekiya, H and Shiozawa, M and Suzuki, Y and Takeda, A and Takenaga, Y and Ueno, K and Ueshima, K and Yamada, S and Yokozawa, T and Ishihara, C and Kaji, H and Kajita, T and Kaneyuki, K and Lee, KP and McLachlan, T and Okumura, K and Shimizu, Y and Tanimoto, N and Labarga, L and Kearns, E and Litos, M and Raaf, JL and Stone, JL and Sulak,
LR and Goldhaber, M and Bays, K and Kropp, WR and Mine, S and Regis, C and Renshaw, A and Smy, MB and Sobel, HW and Ganezer, KS and Hill, J and Keig,
WE and Jang, JS and Kim, JY and Lim, IT and Albert, JB and Scholberg, K and Walter, CW and Wendell, R and Wongjirad, TM and Ishizuka, T and Tasaka,
S and Learned, JG and Matsuno, S and Smith, SN and Hasegawa, T and Ishida,
T and Ishii, T and Kobayashi, T and Nakadaira, T and Nakamura, K and Nishikawa, K and Oyama, Y and Sakashita, K and Sekiguchi, T and Tsukamoto, T and Suzuki, AT and Takeuchi, Y and Ikeda, M and Minamino,
A and Nakaya, T and Fukuda, Y and Itow, Y and Mitsuka, G and Tanaka, T and Jung, CK and Lopez, GD and Taylor, I and Yanagisawa, C and Ishino, H and Kibayashi, A and Mino, S and Mori, T and Sakuda, M and Toyota, H and Kuno,
Y and Yoshida, M and Kim, SB and Yang, BS and Okazawa, H and Choi, Y and Nishijima, K and Koshiba, M and Yokoyama, M and Totsuka, Y and Martens,
K and Schuemann, J and Vagins, MR and Chen, S and Heng, Y and Yang, Z and Zhang, H and Kielczewska, D and Mijakowski, P and Connolly, K and Dziomba, M and Thrane, E and Wilkes, RJ and Super-Kamiokande
Collaboration},
Title = {Search for nucleon decay via n→ν[over ¯]π0 and
p→ν[over ¯]π+ in Super-Kamiokande.},
Journal = {Physical review letters},
Volume = {113},
Number = {12},
Pages = {121802},
Year = {2014},
Month = {September},
ISSN = {0031-9007},
url = {http://dx.doi.org/10.1103/physrevlett.113.121802},
Abstract = {We present the results of searches for nucleon decay via
n→ν[over ¯]π0 and p→ν[over ¯]π+ using data from a
combined 172.8 kt·yr exposure of Super-Kamiokande-I,-II,
and-III. We set lower limits on the partial lifetime for
each of these modes: τn→ν[over ¯]π0>1.1×10(33) years
and τp→ν[over ¯]π+>3.9×10(32) years at a 90%
confidence level.},
Doi = {10.1103/physrevlett.113.121802},
Key = {fds248706}
}
@article{fds318494,
Author = {Abe, K and others},
Title = {Neutrino oscillation physics potential of the T2K
experiment},
Journal = {PTEP},
Volume = {2015},
Number = {4},
Pages = {043C01-043C01},
Publisher = {Oxford University Press (OUP)},
Year = {2015},
url = {http://dx.doi.org/10.1093/ptep/ptv031},
Abstract = {The observation of the recent electron neutrino appearance
in a muon neutrino beam and the high-precision measurement
of the mixing angle Θ13 have led to a re-evaluation of the
physics potential of the T2K long-baseline neutrino
oscillation experiment. Sensitivities are explored for CP
violation in neutrinos, non-maximal sin2 2Θ23, the octant
of Θ23, and the mass hierarchy, in addition to the
measurements of δCP, sin2 Θ23, and Δm232, for various
combinations of ν-mode and ν-mode data-taking. With an
exposure of 7.8 × 1021 protons-on-target, T2K can achieve 1
σ resolution of 0.050 (0.054) on sin2 Θ23 and 0.040
(0.045) × 10-3 eV2 on Δm232 for 100% (50%) neutrino beam
mode running assuming sin2 Θ23 = 0.5 and Δm232 = 2.4 ×
10-3 eV2. T2K will have sensitivity to the CP-violating
phase δCP at 90% C.L. or better over a significant range.
For example, if sin2 2Θ23 is maximal (i.e. Θ23 = 45°) the
range is -115° < δCP < -60° for normal hierarchy and
+50° < δCP < +130° for inverted hierarchy. When T2K data
is combined with data from the NOνA experiment, the region
of oscillation parameter space where there is sensitivity to
observe a non-zero δCP is substantially increased compared
to if each experiment is analyzed alone.},
Doi = {10.1093/ptep/ptv031},
Key = {fds318494}
}
@article{fds318489,
Author = {Takhistov, V and others},
Title = {Search for Nucleon and Dinucleon Decays with an Invisible
Particle and a Charged Lepton in the Final State at the
Super-Kamiokande Experiment},
Journal = {Phys. Rev. Lett.},
Volume = {115},
Number = {12},
Pages = {121803-121803},
Year = {2015},
url = {http://dx.doi.org/10.1103/PhysRevLett.115.121803},
Abstract = {Search results for nucleon decays p→e^{+}X, p→μ^{+}X,
n→νγ (where X is an invisible, massless particle) as
well as dinucleon decays np→e^{+}ν, np→μ^{+}ν, and
np→τ^{+}ν in the Super-Kamiokande experiment are
presented. Using single-ring data from an exposure of
273.4 kton·yr, a search for these decays yields a
result consistent with no signal. Accordingly, lower limits
on the partial lifetimes of τ_{p→e^{+}X}>7.9×10^{32} yr,
τ_{p→μ^{+}X}>4.1×10^{32} yr, τ_{n→νγ}>5.5×10^{32}
yr, τ_{np→e^{+}ν}>2.6×10^{32} yr,
τ_{np→μ^{+}ν}>2.2×10^{32} yr, and τ_{np→τ^{+}ν}>2.9×10^{31}
yr at a 90% confidence level are obtained. Some of these
searches are novel.},
Doi = {10.1103/PhysRevLett.115.121803},
Key = {fds318489}
}
@article{fds318490,
Author = {Abe, K and others},
Title = {Measurement of the $ν_μ$ charged current quasielastic
cross section on carbon with the T2K on-axis neutrino
beam},
Journal = {Phys. Rev.},
Volume = {D91},
Number = {11},
Pages = {112002-112002},
Publisher = {American Physical Society (APS)},
Year = {2015},
url = {http://dx.doi.org/10.1103/PhysRevD.91.112002},
Abstract = {We report a measurement of the νμcharged current
quasielastic cross-sections on carbon in the T2K on-axis
neutrino beam. The measured charged current quasielastic
cross-sections on carbon at mean neutrino energies of 1.94
GeVand 0.93 GeVare (11.95 ± 0.19(stat)-1.47+1.82(syst)) ×
10-39cm2/neutron, and (10.64 ± 0.37(stat)-1.65+2.03(syst))
× 10-39cm2/neutron, respectively. These results agree well
with the predictions of neutrino interaction models. In
addition, we investigated the effects of the nuclear model
and the multi-nucleon interaction.},
Doi = {10.1103/PhysRevD.91.112002},
Key = {fds318490}
}
@article{fds318491,
Author = {Abe, K and others},
Title = {Measurement of the electron neutrino charged-current
interaction rate on water with the T2K ND280 $π^0$
detector},
Journal = {Phys. Rev.},
Volume = {D91},
Number = {11},
Pages = {112010-112010},
Publisher = {American Physical Society (APS)},
Year = {2015},
url = {http://dx.doi.org/10.1103/PhysRevD.91.112010},
Abstract = {This paper presents a measurement of the charged current
interaction rate of the electron neutrino beam component of
the beam above 1.5 GeV using the large fiducial mass of the
T2K π0 detector. The predominant portion of the νe flux
(∼85%) at these energies comes from kaon decays. The
measured ratio of the observed beam interaction rate to the
predicted rate in the detector with water targets filled is
0.89±0.08(stat)±0.11(sys), and with the water targets
emptied is 0.90±0.09(stat)±0.13(sys). The ratio obtained
for the interactions on water only from an event subtraction
method is 0.87±0.33(stat)±0.21(sys). This is the first
measurement of the interaction rate of electron neutrinos on
water, which is particularly of interest to experiments with
water Cherenkov detectors.},
Doi = {10.1103/PhysRevD.91.112010},
Key = {fds318491}
}
@article{fds318492,
Author = {Abe, K and others},
Title = {Physics potential of a long-baseline neutrino oscillation
experiment using a J-PARC neutrino beam and
Hyper-Kamiokande},
Journal = {PTEP},
Volume = {2015},
Number = {5},
Pages = {053C02-053C02},
Year = {2015},
url = {http://dx.doi.org/10.1093/ptep/ptv061},
Abstract = {Hyper-Kamiokande will be a next-generation underground water
Cherenkov detector with a total (fiducial) mass of 0.99
(0.56) million metric tons, approximately 20 (25) times
larger than that of Super-Kamiokande. One of the main goals
of Hyper-Kamiokande is the study of CP asymmetry in the
lepton sector using accelerator neutrino and anti-neutrino
beams. In this paper, the physics potential of a
long-baseline neutrino experiment using the Hyper-
Kamiokande detector and a neutrino beam from the J-PARC
proton synchrotron is presented. The analysis uses the
framework and systematic uncertainties derived from the
ongoing T2K experiment. With a total exposure of 7.5MW
×107s integrated proton beam power (corresponding to 1.56
× 1022protons on target with a 30 GeV proton beam) to a
2.5° off-axis neutrino beam, it is expected that the
leptonic CP phase δCPcan be determined to better than 19
degrees for all possible values of δCP, and CP violation
can be established with a statistical significance of more
than 3 σ (5 σ) for 76% (58%) of the δCPparameter space.
Using both νeappearance and νμ disappearance data, the
expected 1 σ uncertainty of sin2Θ23is 0.015(0.006) for
sin2Θ23= 0.5(0.45).},
Doi = {10.1093/ptep/ptv061},
Key = {fds318492}
}
@article{fds318488,
Author = {Abe, K and others},
Title = {Measurement of the ν$_μ$ charged-current quasielastic
cross section on carbon with the ND280 detector at
T2K},
Journal = {Phys. Rev.},
Volume = {D92},
Number = {11},
Pages = {112003-112003},
Year = {2015},
url = {http://dx.doi.org/10.1103/PhysRevD.92.112003},
Abstract = {This paper reports a measurement by the T2K experiment of
the νμ charged current quasielastic (CCQE) cross section
on a carbon target with the off-axis detector based on the
observed distribution of muon momentum (pμ) and angle with
respect to the incident neutrino beam (θμ). The
flux-integrated CCQE cross section was measured to be
«σ},
Doi = {10.1103/PhysRevD.92.112003},
Key = {fds318488}
}
@article{fds248695,
Author = {Abe, K and others},
Title = {Measurements of neutrino oscillation in appearance and
disappearance channels by the T2K experiment with
6.6×10$^20$ protons on target},
Journal = {Phys. Rev.},
Volume = {D91},
Number = {7},
Pages = {072010-072010},
Year = {2015},
ISSN = {1550-7998},
url = {http://dx.doi.org/10.1103/PhysRevD.91.072010},
Abstract = {We report on measurements of neutrino oscillation using data
from the T2K long-baseline neutrino experiment collected
between 2010 and 2013. In an analysis of muon neutrino
disappearance alone, we find the following estimates and 68%
confidence intervals for the two possible mass hierarchies:
normal hierarchy: sin2θ23= 0.514-0.056+0.055and Δm322=
(2.51 ± 0.10) × 10-3eV2/c4and inverted hierarchy:
sin2θ23= 0.511 ± 0.055 and Δm132= (2.48 ± 0.10) ×
10-3eV2/c4. The analysis accounts for multinucleon
mechanisms in neutrino interactions which were found to
introduce negligible bias. We describe our first analyses
that combine measurements of muon neutrino disappearance and
electron neutrino appearance to estimate four oscillation
parameters, |Δm2|, sin2θ23, sin2θ13, δCP, and the mass
hierarchy. Frequentist and Bayesian intervals are presented
for combinations of these parameters, with and without
including recent reactor measurements. At 90% confidence
level and including reactor measurements, we exclude the
region δCP= [0.15; 0.83]π for normal hierarchy and δCP=
[-0.08; 1.09]π for inverted hierarchy. The T2K and reactor
data weakly favor the normal hierarchy with a Bayes factor
of 2.2. The most probable values and 68% one-dimensional
credible intervals for the other oscillation parameters,
when reactor data are included, are sin2θ23=
0.528-0.038+0.055and |Δm322| = (2.51 ± 0.11) ×
10-3eV2/c4.},
Doi = {10.1103/PhysRevD.91.072010},
Key = {fds248695}
}
@article{fds248696,
Author = {Gustafson, J and Abe, K and Haga, Y and Hayato, Y and Ikeda, M and Iyogi,
K and Kameda, J and Kishimoto, Y and Miura, M and Moriyama, S and Nakahata,
M and Nakajima, T and Nakano, Y and Nakayama, S and Orii, A and Sekiya, H and Shiozawa, M and Takeda, A and Tanaka, H and Tomura, T and Wendell, RA and Irvine, T and Kajita, T and Kametani, I and Kaneyuki, K and Nishimura,
Y and Richard, E and Okumura, K and Labarga, L and Fernandez, P and Berkman, S and Tanaka, HA and Tobayama, S and Kearns, E and Raaf, JL and Stone, JL and Sulak, LR and Goldhaber, M and Carminati, G and Kropp, WR and Mine, S and Weatherly, P and Renshaw, A and Smy, MB and Sobel, HW and Takhistov, V and Ganezer, KS and Hartfiel, BL and Hill, J and Hong, N and Kim, JY and Lim, IT and Akiri, T and Himmel, A and Scholberg, K and Walter,
CW and Wongjirad, T and Ishizuka, T and Tasaka, S and Jang, JS and Learned,
JG and Matsuno, S and Smith, SN and Hasegawa, T and Ishida, T and Ishii, T and Kobayashi, T and Nakadaira, T and Nakamura, K and Oyama, Y and Sakashita, K and Sekiguchi, T and Tsukamoto, T and Suzuki, AT and Takeuchi, Y and Yano, T and Hirota, S and Huang, K and Ieki, K and Kikawa,
T and Minamino, A and Nakaya, T and Suzuki, K and Takahashi, S and Fukuda,
Y and Choi, K and Itow, Y and Mitsuka, G and Suzuki, T and Mijakowski, P and Hignight, J and Imber, J and Jung, CK and Palomino, JL and Yanagisawa,
C and Ishino, H and Kayano, T and Kibayashi, A and Koshio, Y and Mori, T and Sakuda, M and Kuno, Y and Tacik, R and Kim, SB and Okazawa, H and Choi, Y and Nishijima, K and Koshiba, M and Suda, Y and Totsuka, Y and Yokoyama, M and Bronner, C and Martens, K and Marti, L and Suzuki, Y and Vagins, MR and Martin, JF and Perio, PD and Konaka, A and Wilking, MJ and Chen, S and Zhang, Y and Wilkes, RJ},
Title = {Search for dinucleon decay into pions at
Super-Kamiokande},
Journal = {Physical Review D - Particles, Fields, Gravitation and
Cosmology},
Volume = {91},
Number = {7},
Year = {2015},
ISSN = {1550-7998},
url = {http://dx.doi.org/10.1103/PhysRevD.91.072009},
Abstract = {© 2015 American Physical Society.A search for dinucleon
decay into pions with the Super-Kamiokande detector has been
performed with an exposure of 282.1 kiloton-years. Dinucleon
decay is a process that violates baryon number by two units.
We present the first search for dinucleon decay to pions in
a large water-Cherenkov detector. The modes
O16(pp)→C14π+π+, O16(pn)→N14π+π0, and
O16(nn)→O14π0π0 are investigated. No significant excess
in the Super-Kamiokande data has been found, so a lower
limit on the lifetime of the process per oxygen nucleus is
determined. These limits are τpp→π+π+>7.22×1031years,
τpn→π+π0>1.70×1032years, and τnn→π0π0>4.04×1032years.
The lower limits on each mode are about 2 orders of
magnitude better than previous limits from searches for
dinucleon decay in iron.},
Doi = {10.1103/PhysRevD.91.072009},
Key = {fds248696}
}
@article{fds248697,
Author = {Abe, K and others},
Title = {Limits on sterile neutrino mixing using atmospheric
neutrinos in Super-Kamiokande},
Journal = {Phys. Rev.},
Volume = {D91},
Number = {5},
Pages = {052019-052019},
Publisher = {American Physical Society (APS)},
Year = {2015},
ISSN = {1550-7998},
url = {http://dx.doi.org/10.1103/PhysRevD.91.052019},
Abstract = {We present limits on sterile neutrino mixing using 4,438
live-days of atmospheric neutrino data from the
Super-Kamiokande experiment. We search for fast oscillations
driven by an eV2-scale mass splitting and for oscillations
into sterile neutrinos instead of tau neutrinos at the
atmospheric mass splitting. When performing both of these
searches we assume that the sterile mass splitting is large,
allowing sin2(Δm2L/4E) to be approximated as 0.5, and we
assume that there is no mixing between electron neutrinos
and sterile neutrinos (|Ue4|2=0). No evidence of sterile
oscillations is seen and we limit |Uμ4|2 to less than 0.041
and |Uτ4|2 to less than 0.18 for Δm2>0.1eV2 at the 90%
C.L. in a 3+1 framework. The approximations that can be made
with atmospheric neutrinos allow these limits to be easily
applied to 3+N models, and we provide our results in a
generic format to allow comparisons with other sterile
neutrino models.},
Doi = {10.1103/PhysRevD.91.052019},
Key = {fds248697}
}
@article{fds248698,
Author = {Abe, K and others},
Title = {Search for short baseline $ν_e$ disappearance with the T2K
near detector},
Journal = {Phys. Rev.},
Volume = {D91},
Number = {5},
Pages = {051102-051102},
Publisher = {American Physical Society (APS)},
Year = {2015},
ISSN = {1550-7998},
url = {http://dx.doi.org/10.1103/PhysRevD.91.051102},
Abstract = {The T2K experiment has performed a search for νe
disappearance due to sterile neutrinos using 5.9×1020
protons on target for a baseline of 280 m in a neutrino beam
peaked at about 500 MeV. A sample of νe CC interactions in
the off-axis near detector has been selected with a purity
of 63% and an efficiency of 26%. The p-value for the null
hypothesis is 0.085 and the excluded region at 95% C.L. is
approximately sin22θee>0.3 for Δmeff2>7eV2/c4.},
Doi = {10.1103/PhysRevD.91.051102},
Key = {fds248698}
}
@article{fds248699,
Author = {Abe, K and others},
Title = {Test of Lorentz invariance with atmospheric
neutrinos},
Journal = {Phys. Rev.},
Volume = {D91},
Number = {5},
Pages = {052003-052003},
Publisher = {American Physical Society (APS)},
Year = {2015},
ISSN = {1550-7998},
url = {http://dx.doi.org/10.1103/PhysRevD.91.052003},
Abstract = {A search for neutrino oscillations induced by Lorentz
violation has been performed using 4,438 live-days of
Super-Kamiokande atmospheric neutrino data. The Lorentz
violation is included in addition to standard three-flavor
oscillations using the nonperturbative standard model
extension (SME), allowing the use of the full range of
neutrino path lengths, ranging from 15 to 12,800 km, and
energies ranging from 100 MeV to more than 100 TeV in the
search. No evidence of Lorentz violation was observed, so
limits are set on the renormalizable isotropic SME
coefficients in the eμ, μτ, and eτ sectors, improving
the existing limits by up to 7 orders of magnitude and
setting limits for the first time in the neutrino μτ
sector of the SME.},
Doi = {10.1103/PhysRevD.91.052003},
Key = {fds248699}
}
@article{Zhang:2013tua,
Author = {Zhang, H and others},
Title = {Supernova Relic Neutrino Search with Neutron Tagging at
Super-Kamiokande-IV},
Journal = {Astropart. Phys.},
Volume = {60},
Pages = {41-46},
Publisher = {Elsevier BV},
Year = {2015},
ISSN = {0927-6505},
url = {http://arxiv.org/pdf/1311.3738},
Abstract = {A search for Supernova Relic Neutrinos ν̄e's is first
conducted via inverse-beta-decay by tagging neutron capture
on hydrogen at Super-Kamiokande-IV. The neutron tagging
efficiency is determined to be (17.74±0.04stat.±1.05sys.)%,
while the corresponding accidental background probability is
(1.06±0.01 stat.±0.18sys.)%. Using 960 days of data, we
obtain 13 inverse-beta-decay candidates in the range of
Eν̄e between 13.3 MeV and 31.3 MeV. All of the observed
candidates are attributed to background. Upper limits at 90%
C.L. are calculated in the absence of a signal. © 2014
Elsevier B.V. All rights reserved.},
Doi = {10.1016/j.astropartphys.2014.05.004},
Key = {Zhang:2013tua}
}
@article{fds318493,
Author = {Choi, K and others},
Title = {Search for neutrinos from annihilation of captured low-mass
dark matter particles in the Sun by Super-Kamiokande},
Journal = {Phys. Rev. Lett.},
Volume = {114},
Number = {14},
Pages = {141301-141301},
Year = {2015},
url = {http://dx.doi.org/10.1103/PhysRevLett.114.141301},
Abstract = {Super-Kamiokande (SK) can search for weakly interacting
massive particles (WIMPs) by detecting neutrinos produced
from WIMP annihilations occurring inside the Sun. In this
analysis, we include neutrino events with interaction
vertices in the detector in addition to upward-going muons
produced in the surrounding rock. Compared to the previous
result, which used the upward-going muons only, the signal
acceptances for light (few-GeV/c^{2}-200-GeV/c^{2}) WIMPs
are significantly increased. We fit 3903 days of SK data to
search for the contribution of neutrinos from WIMP
annihilation in the Sun. We found no significant excess over
expected atmospheric-neutrino background and the result is
interpreted in terms of upper limits on WIMP-nucleon elastic
scattering cross sections under different assumptions about
the annihilation channel. We set the current best limits on
the spin-dependent WIMP-proton cross section for WIMP masses
below 200 GeV/c^{2} (at 10 GeV/c^{2},
1.49×10^{-39} cm^{2} for χχ→bb[over ¯] and
1.31×10^{-40} cm^{2} for χχ→τ^{+}τ^{-}
annihilation channels), also ruling out some fraction of
WIMP candidates with spin-independent coupling in the
few-GeV/c^{2} mass range.},
Doi = {10.1103/PhysRevLett.114.141301},
Key = {fds318493}
}
@article{fds248694,
Author = {Abe, K and Hayato, Y and Iida, T and Ishihara, K and Kameda, J and Koshio,
Y and Minamino, A and Mitsuda, C and Miura, M and Moriyama, S and Nakahata,
M and Obayashi, Y and Ogawa, H and Sekiya, H and Shiozawa, M and Suzuki, Y and Takeda, A and Takeuchi, Y and Ueshima, K and Watanabe, H and Higuchi, I and Ishihara, C and Ishitsuka, M and Kajita, T and Kaneyuki, K and Mitsuka,
G and Nakayama, S and Nishino, H and Okumura, K and Saji, C and Takenaga,
Y and Clark, S and Desai, S and Dufour, F and Herfurth, A and Kearns, E and Likhoded, S and Litos, M and Raaf, JL and Stone, JL and Sulak, LR and Wang,
W and Goldhaber, M and Casper, D and Cravens, JP and Dunmore, J and Griskevich, J and Kropp, WR and Liu, DW and Mine, S and Regis, C and Smy,
MB and Sobel, HW and Vagins, MR and Ganezer, KS and Hartfiel, B and Hill,
J and Keig, WE and Jang, JS and Jeoung, IS and Kim, JY and Lim, IT and Scholberg, K and Tanimoto, N and Walter, CW and Wendell, R and Ellsworth, RW and Tasaka, S and Guillian, G and Learned, JG and Matsuno,
S and Messier, MD and Ichikawa, AK and Ishida, T and Ishii, T and Iwashita,
T and Kobayashi, T and Nakadaira, T and Nakamura, K and Nishikawa, K and Nitta, K and Oyama, Y and Suzuki, AT and Hasegawa, M and Maesaka, H and Nakaya, T and Sasaki, T and Sato, H and Tanaka, H and Yamamoto, S and Yokoyama, M and Haines, TJ and Dazeley, S and Hatakeyama, S and Svoboda,
R and Sullivan, GW and Gran, R and Habig, A and Fukuda, Y and Itow,
Y},
Title = {Search for n-n ¯ oscillation in Super-Kamiokande SEARCH FOR
n-n ¯ OSCILLATION IN SUPER-⋯ K. ABE et
al.},
Journal = {Physical Review D - Particles, Fields, Gravitation and
Cosmology},
Volume = {91},
Number = {7},
Pages = {072006},
Publisher = {American Physical Society (APS)},
Year = {2015},
Month = {April},
ISSN = {1550-7998},
url = {http://dx.doi.org/10.1103/PhysRevD.91.072006},
Abstract = {A search for neutron-antineutron (n-n¯) oscillation was
undertaken in Super-Kamiokande using the 1489 live-day or
2.45×1034 neutron-year exposure data. This process violates
both baryon and baryon minus lepton numbers by an absolute
value of two units and is predicted by a large class of
hypothetical models where the seesaw mechanism is
incorporated to explain the observed tiny neutrino masses
and the matter-antimatter asymmetry in the Universe. No
evidence for n-n¯ oscillation was found; the lower limit of
the lifetime for neutrons bound in O16, in an analysis that
included all of the significant sources of experimental
uncertainties, was determined to be 1.9×1032years at the
90% confidence level. The corresponding lower limit for the
oscillation time of free neutrons was calculated to be
2.7×108s using a theoretical value of the nuclear
suppression factor of 0.517×1023s-1 and its
uncertainty.},
Doi = {10.1103/PhysRevD.91.072006},
Key = {fds248694}
}
@article{fds248693,
Author = {Walter, CW},
Title = {The brighter-fatter and other sensor effects in CCD
simulations for precision astronomy},
Journal = {Journal of Instrumentation},
Volume = {10},
Number = {5},
Pages = {C05015-C05015},
Publisher = {IOP Publishing},
Year = {2015},
Month = {May},
url = {http://dx.doi.org/10.1088/1748-0221/10/05/C05015},
Abstract = {Upcoming and current large astronomical survey experiments
often seek to constrain cosmological parameters via
measurements of subtle effects such as weak lensing, which
can only be measured statistically. In these cases,
instrumental effects in the image plane CCDs need to be
accounted and/or corrected for in measurement algorithms.
Otherwise, the systematic errors induced in the measurements
might overwhelm the size of the desired effects. Lateral
electric fields in the bulk of the CCDs caused by field
shaping potentials or space charge build up as the electrons
in the image are acquired can cause lateral deflections of
the electrons drifting in the CCD bulk. Here, I report on
the LSST effort to model these effects on a photon-by-photon
basis by the use of a Monte Carlo technique. The eventual
goal of this work is to produce a CCD model validated by
laboratory data which can then be used to evaluate its
effects on weak lensing science.},
Doi = {10.1088/1748-0221/10/05/C05015},
Key = {fds248693}
}
@article{fds318483,
Author = {Abe, K and others},
Title = {Measurement of double-differential muon neutrino
charged-current interactions on C$_8$H$_8$ without pions in
the final state using the T2K off-axis beam},
Journal = {Phys. Rev.},
Volume = {D93},
Number = {11},
Pages = {112012-112012},
Publisher = {American Physical Society (APS)},
Year = {2016},
url = {http://dx.doi.org/10.1103/PhysRevD.93.112012},
Abstract = {We report the measurement of muon neutrino charged-current
interactions on carbon without pions in the final state at
the T2K beam energy using 5.734×1020 protons on target. For
the first time the measurement is reported as a
flux-integrated, double-differential cross section in muon
kinematic variables (cosθμ, pμ), without correcting for
events where a pion is produced and then absorbed by final
state interactions. Two analyses are performed with
different selections, background evaluations and
cross-section extraction methods to demonstrate the
robustness of the results against biases due to
model-dependent assumptions. The measurements compare
favorably with recent models which include nucleon-nucleon
correlations but, given the present precision, the
measurement does not distinguish among the available models.
The data also agree with Monte Carlo simulations which use
effective parameters that are tuned to external data to
describe the nuclear effects. The total cross section in the
full phase space is σ=(0.417±0.047(syst)±0.005(stat))×10-38
cm2 nucleon-1 and the cross section integrated in the region
of phase space with largest efficiency and best
signal-over-background ratio (cosθμ>0.6 and pμ>200 MeV)
is σ=(0.202±0.036(syst)±0.003(stat))×10-38 cm2
nucleon-1.},
Doi = {10.1103/PhysRevD.93.112012},
Key = {fds318483}
}
@article{fds318482,
Author = {Abe, K and others},
Title = {Real-Time Supernova Neutrino Burst Monitor at
Super-Kamiokande},
Journal = {Astropart. Phys.},
Volume = {81},
Pages = {39-48},
Publisher = {Elsevier BV},
Year = {2016},
url = {http://dx.doi.org/10.1016/j.astropartphys.2016.04.003},
Abstract = {We present a real-time supernova neutrino burst monitor at
Super-Kamiokande (SK). Detecting supernova explosions by
neutrinos in real time is crucial for giving a clear picture
of the explosion mechanism. Since the neutrinos are expected
to come earlier than light, a fast broadcasting of the
detection may give astronomers a chance to make
electromagnetic radiation observations of the explosions
right at the onset. The role of the monitor includes a fast
announcement of the neutrino burst detection to the world
and a determination of the supernova direction. We present
the online neutrino burst detection system and studies of
the direction determination accuracy based on simulations at
SK.},
Doi = {10.1016/j.astropartphys.2016.04.003},
Key = {fds318482}
}
@article{fds318484,
Author = {Abe, K and others},
Title = {Measurement of Muon Antineutrino Oscillations with an
Accelerator-Produced Off-Axis Beam},
Journal = {Phys. Rev. Lett.},
Volume = {116},
Number = {18},
Pages = {181801-181801},
Year = {2016},
url = {http://dx.doi.org/10.1103/PhysRevLett.116.181801},
Abstract = {T2K reports its first measurements of the parameters
governing the disappearance of ν[over ¯]_{μ} in an
off-axis beam due to flavor change induced by neutrino
oscillations. The quasimonochromatic ν[over ¯]_{μ} beam,
produced with a peak energy of 0.6 GeV at J-PARC, is
observed at the far detector Super-Kamiokande, 295 km away,
where the ν[over ¯]_{μ} survival probability is expected
to be minimal. Using a data set corresponding to
4.01×10^{20} protons on target, 34 fully contained μ-like
events were observed. The best-fit oscillation parameters
are sin^{2}(θ[over ¯]_{23})=0.45 and |Δm[over
¯]_{32}^{2}|=2.51×10^{-3} eV^{2} with 68% confidence
intervals of 0.38-0.64 and 2.26-2.80×10^{-3} eV^{2},
respectively. These results are in agreement with existing
antineutrino parameter measurements and also with the
ν_{μ} disappearance parameters measured by
T2K.},
Doi = {10.1103/PhysRevLett.116.181801},
Key = {fds318484}
}
@article{fds318487,
Author = {Abe, K and others},
Title = {Upper bound on neutrino mass based on T2K neutrino timing
measurements},
Journal = {Phys. Rev.},
Volume = {D93},
Number = {1},
Pages = {012006-012006},
Publisher = {American Physical Society (APS)},
Year = {2016},
url = {http://dx.doi.org/10.1103/PhysRevD.93.012006},
Abstract = {The Tokai to Kamioka (T2K) long-baseline neutrino experiment
consists of a muon neutrino beam, produced at the J-PARC
accelerator, a near detector complex and a large
295-km-distant far detector. The present work utilizes the
T2K event timing measurements at the near and far detectors
to study neutrino time of flight as a function of derived
neutrino energy. Under the assumption of a relativistic
relation between energy and time of flight, constraints on
the neutrino rest mass can be derived. The sub-GeV neutrino
beam in conjunction with timing precision of order tens of
ns provide sensitivity to neutrino mass in the few MeV/c2
range. We study the distribution of relative arrival times
of muon and electron neutrino candidate events at the T2K
far detector as a function of neutrino energy. The 90% C.L.
upper limit on the mixture of neutrino mass eigenstates
represented in the data sample is found to be mν2<5.6
MeV2/c4.},
Doi = {10.1103/PhysRevD.93.012006},
Key = {fds318487}
}
@article{fds318486,
Author = {Zhang, Y and others},
Title = {First measurement of radioactive isotope production through
cosmic-ray muon spallation in Super-Kamiokande
IV},
Journal = {Phys. Rev.},
Volume = {D93},
Number = {1},
Pages = {012004-012004},
Publisher = {American Physical Society (APS)},
Year = {2016},
url = {http://dx.doi.org/10.1103/PhysRevD.93.012004},
Abstract = {Cosmic-ray-muon spallation-induced radioactive isotopes with
β decays are one of the major backgrounds for solar,
reactor, and supernova relic neutrino experiments. Unlike in
scintillator, production yields for cosmogenic backgrounds
in water have not been exclusively measured before, yet they
are becoming more and more important in next generation
neutrino experiments designed to search for rare signals. We
have analyzed the low-energy trigger data collected at
Super-Kamiokande IV in order to determine the production
rates of B12, N12, N16, Be11, Li9, He8, C9, Li8, B8, and
C15. These rates were extracted from fits to time
differences between parent muons and subsequent daughter
β's by fixing the known isotope lifetimes. Since Li9 can
fake an inverse-beta-decay reaction chain via a β+n cascade
decay, producing an irreducible background with detected
energy up to a dozen MeV, a dedicated study is needed for
evaluating its impact on future measurements; the
application of a neutron tagging technique using correlated
triggers was found to improve this Li9 measurement. The
measured yields were generally found to be comparable with
theoretical calculations, except the cases of the isotopes
Li8/B8 and Li9.},
Doi = {10.1103/PhysRevD.93.012004},
Key = {fds318486}
}
@article{fds318485,
Author = {Abe, K and others},
Title = {Measurement of the muon neutrino inclusive charged-current
cross section in the energy range of 1–3 GeV with the T2K
INGRID detector},
Journal = {Phys. Rev.},
Volume = {D93},
Number = {7},
Pages = {072002-072002},
Publisher = {American Physical Society (APS)},
Year = {2016},
url = {http://dx.doi.org/10.1103/PhysRevD.93.072002},
Abstract = {We report a measurement of the νμ-nucleus inclusive
charged-current cross section (=σcc) on iron using data
from the INGRID detector exposed to the J-PARC neutrino
beam. The detector consists of 14 modules in total, which
are spread over a range of off-axis angles from 0° to
1.1°. The variation in the neutrino energy spectrum as a
function of the off-axis angle, combined with event topology
information, is used to calculate this cross section as a
function of neutrino energy. The cross section is measured
to be σcc(1.1 GeV)=1.10±0.15 (10-38 cm2/nucleon), σcc(2.0
GeV)=2.07±0.27 (10-38 cm2/nucleon), and σcc(3.3
GeV)=2.29±0.45 (10-38 cm2/nucleon), at energies of 1.1,
2.0, and 3.3 GeV, respectively. These results are consistent
with the cross section calculated by the neutrino
interaction generators currently used by T2K. More
importantly, the method described here opens up a new way to
determine the energy dependence of neutrino-nucleus cross
sections.},
Doi = {10.1103/PhysRevD.93.072002},
Key = {fds318485}
}
@article{fds326488,
Author = {Patrignani, C and others},
Title = {Review of Particle Physics},
Journal = {Chin. Phys.},
Volume = {C40},
Number = {10},
Pages = {100001-100001},
Publisher = {IOP Publishing},
Year = {2016},
url = {http://dx.doi.org/10.1088/1674-1137/40/10/100001},
Abstract = {The Review summarizes much of particle physics and
cosmology. Using data from previous editions, plus 3,062 new
measurements from 721 papers, we list, evaluate, and average
measured properties of gauge bosons and the recently
discovered Higgs boson, leptons, quarks, mesons, and
baryons. We summarize searches for hypothetical particles
such as supersymmetric particles, heavy bosons, axions, dark
photons, etc. All the particle properties and search limits
are listed in Summary Tables. We also give numerous tables,
figures, formulae, and reviews of topics such as Higgs Boson
Physics, Supersymmetry, Grand Unified Theories, Neutrino
Mixing, Dark Energy, Dark Matter, Cosmology, Particle
Detectors, Colliders, Probability and Statistics. Among the
117 reviews are many that are new or heavily revised,
including those on Pentaquarks and Inflation. The complete
Review is published online in a journal and on the website
of the Particle Data Group (http://pdg.lbl.gov). The printed
PDG Book contains the Summary Tables and all review articles
but no longer includes the detailed tables from the Particle
Listings. A Booklet with the Summary Tables and abbreviated
versions of some of the review articles is also
available.},
Doi = {10.1088/1674-1137/40/10/100001},
Key = {fds326488}
}
@article{fds326463,
Author = {Abe, K and others},
Title = {Measurement of Coherent $π^+$ Production in Low Energy
Neutrino-Carbon Scattering},
Journal = {Phys. Rev. Lett.},
Volume = {117},
Number = {19},
Pages = {192501-192501},
Year = {2016},
url = {http://dx.doi.org/10.1103/PhysRevLett.117.192501},
Abstract = {We report the first measurement of the flux-averaged cross
section for charged current coherent π^{+} production on
carbon for neutrino energies less than 1.5 GeV, and with a
restriction on the final state phase space volume in the T2K
near detector, ND280. Comparisons are made with predictions
from the Rein-Sehgal coherent production model and the model
by Alvarez-Ruso et al., the latter representing the first
implementation of an instance of the new class of
microscopic coherent models in a neutrino interaction
Monte Carlo event generator. We observe a clear event
excess above background, disagreeing with the null results
reported by K2K and SciBooNE in a similar neutrino energy
region. The measured flux-averaged cross sections are below
those predicted by both the Rein-Sehgal and Alvarez-Ruso
et al.<h4>Models</h4>},
Doi = {10.1103/PhysRevLett.117.192501},
Key = {fds326463}
}
@article{fds326464,
Author = {Abe, K and others},
Title = {Search for Neutrinos in Super-Kamiokande associated with
Gravitational Wave Events GW150914 and GW151226},
Journal = {Astrophys. J.},
Volume = {830},
Number = {1},
Pages = {L11-L11},
Publisher = {American Astronomical Society},
Year = {2016},
url = {http://dx.doi.org/10.3847/2041-8205/830/1/L11},
Abstract = {We report the results from a search in Super-Kamiokande for
neutrino signals coincident with the first detected
gravitational-wave events, GW150914 and GW151226, as well as
LVT151012, using a neutrino energy range from 3.5 MeV to 100
PeV. We searched for coincident neutrino events within a
time window of ±500 s around the gravitational-wave
detection time. Four neutrino candidates are found for
GW150914, and no candidates are found for GW151226. The
remaining neutrino candidates are consistent with the
expected background events. We calculated the 90% confidence
level upper limits on the combined neutrino fluence for both
gravitational-wave events, which depends on event energy and
topologies. Considering the upward-going muon data set (1.6
GeV-100 PeV), the neutrino fluence limit for each
gravitational-wave event is 14-37 (19-50) cm-2 for muon
neutrinos (muon antineutrinos), depending on the zenith
angle of the event. In the other data sets, the combined
fluence limits for both gravitational-wave events range from
2.4 ×104 to 7.0 ×109 cm-2.},
Doi = {10.3847/2041-8205/830/1/L11},
Key = {fds326464}
}
@article{fds326465,
Author = {Richard, E and others},
Title = {Measurements of the atmospheric neutrino flux by
Super-Kamiokande: energy spectra, geomagnetic effects, and
solar modulation},
Journal = {Phys. Rev.},
Volume = {D94},
Number = {5},
Pages = {052001-052001},
Publisher = {American Physical Society (APS)},
Year = {2016},
url = {http://dx.doi.org/10.1103/PhysRevD.94.052001},
Abstract = {A comprehensive study of the atmospheric neutrino flux in
the energy region from sub-GeV up to several TeV using the
Super-Kamiokande (SK) water Cherenkov detector is presented
in this paper. The energy and azimuthal spectra, and
variation over time, of the atmospheric νe+νe and
νμ+νμ fluxes are measured. The energy spectra are
obtained using an iterative unfolding method by combining
various event topologies with differing energy responses.
The azimuthal spectra depending on energy and zenith angle,
and their modulation by geomagnetic effects, are also
studied. A predicted east-west asymmetry is observed in both
the νe and νμ samples at 8.0σ and 6.0σ significance,
respectively, and an indication that the asymmetry dipole
angle changes depending on the zenith angle was seen at the
2.2σ level. The measured energy and azimuthal spectra are
consistent with the current flux models within the estimated
systematic uncertainties. A study of the long-term
correlation between the atmospheric neutrino flux and the
solar magnetic activity cycle is performed, and a weak
preference for a correlation was seen at the 1.1σ level,
using SK-I-SK-IV data spanning a 20-year period. For several
particularly strong solar activity periods, corresponding to
Forbush decrease events, no theoretical prediction is
available but a deviation below the typical neutrino event
rate is seen at the 2.4σ level. The seasonal modulation of
the neutrino flux is also examined, but the change in flux
at the SK site is predicted to be negligible, and, as
expected, no evidence for a seasonal correlation is
seen.},
Doi = {10.1103/PhysRevD.94.052001},
Key = {fds326465}
}
@article{fds326466,
Author = {Abe, K and others},
Title = {Solar Neutrino Measurements in Super-Kamiokande-IV},
Journal = {Phys. Rev.},
Volume = {D94},
Number = {5},
Pages = {052010-052010},
Publisher = {American Physical Society (APS)},
Year = {2016},
url = {http://dx.doi.org/10.1103/PhysRevD.94.052010},
Abstract = {Upgraded electronics, improved water system dynamics, better
calibration and analysis techniques allowed
Super-Kamiokande-IV to clearly observe very low-energy B8
solar neutrino interactions, with recoil electron kinetic
energies as low as ∼3.5 MeV. Super-Kamiokande-IV
data-taking began in September of 2008; this paper includes
data until February 2014, a total livetime of 1664 days. The
measured solar neutrino flux is (2.308±0.020(stat)-0.040+0.039(syst))×106/(cm2
sec) assuming no oscillations. The observed recoil electron
energy spectrum is consistent with no distortions due to
neutrino oscillations. An extended maximum likelihood fit to
the amplitude of the expected solar zenith angle variation
of the neutrino-electron elastic scattering rate in SK-IV
results in a day/night asymmetry of (-3.6±1.6(stat)±0.6(syst))%.
The SK-IV solar neutrino data determine the solar mixing
angle as sin2θ12=0.327-0.031+0.026, all SK solar data
(SK-I, SK-II, SK III and SK-IV) measures this angle to be
sin2θ12=0.334-0.023+0.027, the determined mass-squared
splitting is Δm212=4.8-0.8+1.5×10-5 eV2.},
Doi = {10.1103/PhysRevD.94.052010},
Key = {fds326466}
}
@article{fds347830,
Author = {Abe, K and others},
Title = {Sensitivity of the T2K accelerator-based neutrino experiment
with an Extended run to $20\times10^21$ POT},
Year = {2016},
Key = {fds347830}
}
@article{fds347829,
Author = {Abe, K and others},
Title = {Proposal for an Extended Run of T2K to $20\times10^21$
POT},
Year = {2016},
Key = {fds347829}
}
@article{fds326489,
Author = {Rasmussen, A and Guyonnet, A and Lage, C and Antilogus, P and Astier, P and Doherty, P and Gilmore, K and Kotov, I and Lupton, R and Nomerotski, A and O'Connor, P and Stubbs, C and Tyson, A and Walter,
C},
Title = {High fidelity point-spread function retrieval in the
presence of electrostatic, hysteretic pixel
response},
Journal = {Proceedings of SPIE - The International Society for Optical
Engineering},
Volume = {9915},
Publisher = {SPIE},
Year = {2016},
Month = {January},
ISBN = {9781510602090},
url = {http://dx.doi.org/10.1117/12.2234482},
Abstract = {We employ electrostatic conversion drift calculations to
match CCD pixel signal covariances observed in at field
exposures acquired using candidate sensor devices for the
LSST Camera.1, 2 We thus constrain pixel geometry
distortions present at the end of integration, based on
signal images recorded. We use available data from several
operational voltage parameter settings to validate our
understanding. Our primary goal is to optimize flux point
spread function (FPSF) estimation quantitatively, and
thereby minimize sensor-induced errors which may limit
performance in precision astronomy applications. We consider
alternative compensation scenarios that will take maximum
advantage of our understanding of this underlying mechanism
in data processing pipelines currently under development. To
quantitatively capture the pixel response in
high-contrast/high dynamic range operational extrema, we
propose herein some straightforward laboratory tests that
involve altering the time order of source illumination on
sensors, within individual test exposures. Hence the word
hysteretic in the title of this paper.},
Doi = {10.1117/12.2234482},
Key = {fds326489}
}
@article{fds330710,
Author = {Abdel Maksoud and W and Allard, J and Bargueden, P and Belorgey, J and Bounab, A and Bouty, A and Donati, A and Durand, G and Eppelle, D and Faict-Bastin, S and Genini, L and Guiho, P and Guihard, Q and Joubert,
JM and Kuster, O and Kante, A and Medioni, D and Molinie, F and Solenne, N and Vieillard, L and Walter, C},
Title = {Commissioning of the Cold Test Facility for the JT-60SA
Tokamak Toroidal Field Coils},
Journal = {IEEE Transactions on Applied Superconductivity},
Volume = {26},
Number = {4},
Pages = {1-6},
Publisher = {Institute of Electrical and Electronics Engineers
(IEEE)},
Year = {2016},
Month = {June},
url = {http://dx.doi.org/10.1109/TASC.2015.2510225},
Abstract = {JT-60SA is a fusion experiment, which is jointly constructed
by Japan and Europe and which shall contribute to the early
realization of fusion energy, by providing support to the
operation of ITER and by addressing key physics issues for
ITER and DEMO. The 18 superconducting toroidal field (TF)
coils of the JT-60SA device will be provided by the European
laboratories ENEA and CEA and tested in a cold test facility
(CTF) at CEA Saclay. The coils will be cooled with
supercritical helium and tested at the nominal current of
25.7 kA, at temperatures between 5 and 7.5 K, to check the
temperature margin against a quench. The main objective of
these tests is to validate the TF coil performance and hence
mitigate fabrication risks. During the CTF commissioning
phase, the cooling down and warming up capacities have been
checked, the main thermal and hydraulic performances of the
cryogenic loop have been measured, and the electrical
circuit including the magnet safety system has been tested
in quench conditions. This paper will give an overview of
the main results from the commissioning tests of the
CTF.},
Doi = {10.1109/TASC.2015.2510225},
Key = {fds330710}
}
@article{fds328442,
Author = {Abe, K and others},
Title = {Search for nucleon decay into charged antilepton plus meson
in 0.316 megaton$\cdot$years exposure of the
Super-Kamiokande water Cherenkov detector},
Journal = {Phys. Rev.},
Volume = {D96},
Number = {1},
Pages = {012003-012003},
Publisher = {American Physical Society (APS)},
Year = {2017},
url = {http://dx.doi.org/10.1103/PhysRevD.96.012003},
Abstract = {We have searched for proton decays into a charged antilepton
(e+, μ+) plus a meson (η, ρ0, ω) and for neutron decays
into a charged antilepton (e+, μ+) plus a meson (π-, ρ-)
using Super-Kamiokande I-IV data, corresponding to 0.316
megaton·years of exposure. This measurement updates the
previous published result by using 2.26 times more data and
improved analysis methods. No significant evidence for
nucleon decay is observed and lower limits on the partial
lifetime of the nucleon are obtained. The limits range from
3×1031 to 1×1034 years at 90% confidence level, depending
on the decay mode.},
Doi = {10.1103/PhysRevD.96.012003},
Key = {fds328442}
}
@article{fds330901,
Author = {Abe, K and others},
Title = {Search for an excess of events in the Super-Kamiokande
detector in the directions of the astrophysical neutrinos
reported by the IceCube Collaboration},
Journal = {Astrophys. J.},
Volume = {850},
Number = {2},
Pages = {166-166},
Publisher = {American Astronomical Society},
Year = {2017},
url = {http://dx.doi.org/10.3847/1538-4357/aa951b},
Abstract = {We present the results of a search in the Super-Kamiokande
(SK) detector for excesses of neutrinos with energies above
a few GeV that are in the direction of the track events
reported in IceCube. Data from all SK phases (SK-I through
SK-IV) were used, spanning a period from 1996 April to 2016
April and corresponding to an exposure of 225 kiloton-years.
We considered the 14 IceCube track events from a data set
with 1347 livetime days taken from 2010 to 2014. We use
Poisson counting to determine if there is an excess of
neutrinos detected in SK in a 10° search cone (5° for the
highest energy data set) around the reconstructed direction
of the IceCube event. No significant excess was found in any
of the search directions we examined. We also looked for
coincidences with a recently reported IceCube multiplet
event. No events were detected within a ±500 s time window
around the first detected event, and no significant excess
was seen from that direction over the lifetime of
SK.},
Doi = {10.3847/1538-4357/aa951b},
Key = {fds330901}
}
@article{fds329105,
Author = {Abe, K and others},
Title = {Measurement of $\barν_μ$ and $ν_μ$ charged current
inclusive cross sections and their ratio with the T2K
off-axis near detector},
Journal = {Phys. Rev.},
Volume = {D96},
Number = {5},
Pages = {052001-052001},
Publisher = {American Physical Society (APS)},
Year = {2017},
url = {http://dx.doi.org/10.1103/PhysRevD.96.052001},
Abstract = {We report a measurement of cross section
σ(νμ+nucleus→μ-+X) and the first measurements of the
cross section σ(ν-μ+nucleus→μ++X) and their ratio
R(σ(ν-)σ(ν)) at (anti) neutrino energies below 1.5 GeV.
We determine the single momentum bin cross section
measurements, averaged over the T2K ν-/ν-flux, for the
detector target material (mainly carbon, oxygen, hydrogen
and copper) with phase space restricted laboratory frame
kinematics of θμ<32° and pμ>500 MeV/c. The results are
σ(ν-)=(0.900±0.029(stat)±0.088(syst))×10-39 and
σ(ν)=(2.41±0.022(stat)±0.231(syst))×10-39 in units of
cm2/nucleon and R(σ(ν-)σ(ν))=0.373±0.012(stat)±0.015(syst).},
Doi = {10.1103/PhysRevD.96.052001},
Key = {fds329105}
}
@article{fds326487,
Author = {Abe, K and others},
Title = {Search for proton decay via $p \to e^+π^0$ and $p \to
μ^+π^0$ in 0.31 megaton·years exposure of the
Super-Kamiokande water Cherenkov detector},
Journal = {Phys. Rev.},
Volume = {D95},
Number = {1},
Pages = {012004-012004},
Publisher = {American Physical Society (APS)},
Year = {2017},
url = {http://dx.doi.org/10.1103/PhysRevD.95.012004},
Abstract = {We have searched for proton decay via p→e+π0 and
p→μ+π0 using Super-Kamiokande data from April 1996 to
March 2015, 0.306 megaton·years exposure in total. The
atmospheric neutrino background rate in Super-Kamiokande IV
is reduced to almost half that of phase I-III by tagging
neutrons associated with neutrino interactions. The reach of
the proton lifetime is further enhanced by introducing new
signal criteria that select the decay of a proton in a
hydrogen atom. No candidates were seen in the p→e+π0
search. Two candidates that passed all of the selection
criteria for p→μ+π0 have been observed, but these are
consistent with the expected number of background events of
0.87. Lower limits on the proton lifetime are set at
τ/B(p→e+π0)>1.6×1034 years and τ/B(p→μ+π0)>7.7×1033
years at 90% confidence level.},
Doi = {10.1103/PhysRevD.95.012004},
Key = {fds326487}
}
@article{fds328443,
Author = {Abe, K and others},
Title = {Updated T2K measurements of muon neutrino and antineutrino
disappearance using 1.5$\times$10$^21$ protons on
target},
Journal = {Phys. Rev.},
Volume = {D96},
Number = {1},
Pages = {011102-011102},
Publisher = {American Physical Society (APS)},
Year = {2017},
url = {http://dx.doi.org/10.1103/PhysRevD.96.011102},
Abstract = {We report measurements by the T2K experiment of the
parameters θ23 and Δm322 governing the disappearance of
muon neutrinos and antineutrinos in the three-flavor
neutrino oscillation model. Utilizing the ability of the
experiment to run with either a mainly neutrino or a mainly
antineutrino beam, the parameters are measured separately
for neutrinos and antineutrinos. Using 7.482×1020 POT in
neutrino running mode and 7.471×1020 POT in antineutrino
mode, T2K obtained sin2(θ23)=0.51-0.07+0.08 and
Δm322=2.53-0.13+0.15×10-3 eV2/c4 for neutrinos, and
sin2(θ-23)=0.42-0.07+0.25 and Δm-232=2.55-0.27+0.33×10-3
eV2/c4 for antineutrinos (assuming normal mass ordering). No
significant differences between the values of the parameters
describing the disappearance of muon neutrinos and
antineutrinos were observed.},
Doi = {10.1103/PhysRevD.96.011102},
Key = {fds328443}
}
@article{fds330708,
Author = {Abe, K and others},
Title = {Measurement of neutrino and antineutrino oscillations by the
T2K experiment including a new additional sample of $ν_e$
interactions at the far detector},
Journal = {Phys. Rev.},
Volume = {D96},
Number = {9},
Pages = {092006-092006},
Publisher = {American Physical Society (APS)},
Year = {2017},
url = {http://dx.doi.org/10.1103/PhysRevD.96.092006},
Abstract = {The T2K experiment reports an updated analysis of neutrino
and antineutrino oscillations in appearance and
disappearance channels. Asample of electron neutrino
candidates at Super-Kamiokande in which a pion decay has
been tagged is added to the four single-ring samples used in
previous T2K oscillation analyses. Through combined analyses
of these five samples, simultaneous measurements of four
oscillation parameters, j?m2 32j, sin2 ?23, sin2 ?13, and
dCP and of the mass ordering are made. A set of studies of
simulated data indicates that the sensitivity to the
oscillation parameters is not limited by neutrino
interaction model uncertainty. Multiple oscillation analyses
are performed, and frequentist and Bayesian intervals are
presented for combinations of the oscillation parameters
with and without the inclusion of reactor constraints on
sin2 ?13.When combined with reactor measurements, the
hypothesis of CP conservation (dCP 0 or p) is excluded at
90% confidence level. The 90% confidence region for dCP is
-2.95;-0.44(-1.47;-1.27) for normal (inverted) ordering. The
central values and 68% confidence intervals for the other
oscillation parameters for normal (inverted) ordering are
?m2 32 2.540.082.510.08 10-3 eV2=c4 and sin2?23 0.55+0.05
-0.09 (0.55+0.05 -0.08 ), compatible with maximal mixing. In
the Bayesian analysis, the data weakly prefer normal
ordering (Bayes factor 3.7) and the upper octant for sin2
?23 (Bayes factor 2.4).},
Doi = {10.1103/PhysRevD.96.092006},
Key = {fds330708}
}
@article{fds327380,
Author = {Abe, K and others},
Title = {Search for Lorentz and CPT violation using sidereal time
dependence of neutrino flavor transitions over a short
baseline},
Journal = {Phys. Rev.},
Volume = {D95},
Number = {11},
Pages = {111101-111101},
Publisher = {American Physical Society (APS)},
Year = {2017},
url = {http://dx.doi.org/10.1103/PhysRevD.95.111101},
Abstract = {A class of extensions of the Standard Model allows Lorentz
and CPT violations, which can be identified by the
observation of sidereal modulations in the neutrino
interaction rate. A search for such modulations was
performed using the T2K on-axis near detector. Two
complementary methods were used in this study, both of which
resulted in no evidence of a signal. Limits on associated
Lorentz and CPT-violating terms from the Standard Model
extension have been derived by taking into account their
correlations in this model for the first time. These results
imply such symmetry violations are suppressed by a factor of
more than 1020 at the GeV scale.},
Doi = {10.1103/PhysRevD.95.111101},
Key = {fds327380}
}
@article{fds326461,
Author = {Abe, K and others},
Title = {Combined Analysis of Neutrino and Antineutrino Oscillations
at T2K},
Journal = {Phys. Rev. Lett.},
Volume = {118},
Number = {15},
Pages = {151801-151801},
Year = {2017},
url = {http://dx.doi.org/10.1103/PhysRevLett.118.151801},
Abstract = {T2K reports its first results in the search for CP violation
in neutrino oscillations using appearance and disappearance
channels for neutrino- and antineutrino-mode beams. The data
include all runs from January 2010 to May 2016 and comprise
7.482×10^{20} protons on target in neutrino mode, which
yielded in the far detector 32 e-like and 135 μ-like
events, and 7.471×10^{20} protons on target in antineutrino
mode, which yielded 4 e-like and 66 μ-like events.
Reactor measurements of sin^{2}2θ_{13} have been used as an
additional constraint. The one-dimensional confidence
interval at 90% for the phase δ_{CP} spans the range
(-3.13, -0.39) for normal mass ordering. The CP conservation
hypothesis (δ_{CP}=0, π) is excluded at
90% C.L.},
Doi = {10.1103/PhysRevLett.118.151801},
Key = {fds326461}
}
@article{fds326462,
Author = {Abe, K and Andreopoulos, C and Antonova, M and Aoki, S and Ariga, A and Assylbekov, S and Autiero, D and Ban, S and Barbi, M and Barker, GJ and Barr, G and Bartet-Friburg, P and Batkiewicz, M and Bay, F and Berardi,
V and Berkman, S and Bhadra, S and Bienstock, S and Blondel, A and Bolognesi, S and Bordoni, S and Boyd, SB and Brailsford, D and Bravar,
A and Bronner, C and Buizza Avanzini and M and Calland, RG and Campbell, T and Cao, S and Caravaca Rodríguez and J and Cartwright, SL and Castillo, R and Catanesi, MG and Cervera, A and Cherdack, D and Chikuma, N and Christodoulou, G and Clifton, A and Coleman, J and Collazuol, G and Coplowe, D and Cremonesi, L and Dabrowska, A and De Rosa and G and Dealtry,
T and Denner, PF and Dennis, SR and Densham, C and Dewhurst, D and Di
Lodovico, F and Di Luise and S and Dolan, S and Drapier, O and Duffy, KE and Dumarchez, J and Dytman, S and Dziewiecki, M and Emery-Schrenk, S and Ereditato, A and Feusels, T and Finch, AJ and Fiorentini, GA and Friend,
M and Fujii, Y and Fukuda, D and Fukuda, Y and Furmanski, AP and Galymov,
V and Garcia, A and Giffin, SG and Giganti, C and Gilje, K and Gizzarelli,
F and Gonin, M and Grant, N and Hadley, DR and Haegel, L and Haigh, MD and Hamilton, P and Hansen, D and Harada, J and Hara, T and Hartz, M and Hasegawa, T and Hastings, NC and Hayashino, T and Hayato, Y and Helmer,
RL and Hierholzer, M and Hillairet, A and Himmel, A and Hiraki, T and Hirota, S and Hogan, M and Holeczek, J and Horikawa, S and Hosomi, F and Huang, K and Ichikawa, AK and Ieki, K},
Title = {First measurement of the muon neutrino charged current
single pion production cross section on water with the T2K
near detector},
Journal = {Physical Review D},
Volume = {95},
Number = {1},
Publisher = {American Physical Society (APS)},
Year = {2017},
Month = {January},
url = {http://dx.doi.org/10.1103/PhysRevD.95.012010},
Abstract = {The T2K off-axis near detector, ND280, is used to make the
first differential cross section measurements of muon
neutrino charged current single positive pion production on
a water target at energies ∼0.8 GeV. The differential
measurements are presented as a function of the muon and
pion kinematics, in the restricted phase space defined by
pπ+>200 MeV/c, pμ>200 MeV/c, cos(θπ+)>0.3 and
cos(θμ)>0.3. The total flux integrated νμ charged
current single positive pion production cross section on
water in the restricted phase space is measured to be
σ},
Doi = {10.1103/PhysRevD.95.012010},
Key = {fds326462}
}
@article{fds338354,
Author = {Tanabashi, M and others},
Title = {Review of Particle Physics},
Journal = {Phys. Rev.},
Volume = {D98},
Number = {3},
Pages = {030001-030001},
Publisher = {American Physical Society (APS)},
Year = {2018},
url = {http://dx.doi.org/10.1103/PhysRevD.98.030001},
Abstract = {The Review summarizes much of particle physics and
cosmology. Using data from previous editions, plus 2,873 new
measurements from 758 papers, we list, evaluate, and average
measured properties of gauge bosons and the recently
discovered Higgs boson, leptons, quarks, mesons, and
baryons. We summarize searches for hypothetical particles
such as supersymmetric particles, heavy bosons, axions, dark
photons, etc. Particle properties and search limits are
listed in Summary Tables. We give numerous tables, figures,
formulae, and reviews of topics such as Higgs Boson Physics,
Supersymmetry, Grand Unified Theories, Neutrino Mixing, Dark
Energy, Dark Matter, Cosmology, Particle Detectors,
Colliders, Probability and Statistics. Among the 118 reviews
are many that are new or heavily revised, including a new
review on Neutrinos in Cosmology.Starting with this edition,
the Review is divided into two volumes. Volume 1 includes
the Summary Tables and all review articles. Volume 2
consists of the Particle Listings. Review articles that were
previously part of the Listings are now included in volume
1.The complete Review (both volumes) is published online on
the website of the Particle Data Group (http://pdg.lbl.gov)
and in a journal. Volume 1 is available in print as the PDG
Book. A Particle Physics Booklet with the Summary Tables and
essential tables, figures, and equations from selected
review articles is also available.The 2018 edition of the
Review of Particle Physics should be cited as: M. Tanabashi
(Particle Data Group), Phys. Rev. D 98, 030001
(2018).},
Doi = {10.1103/PhysRevD.98.030001},
Key = {fds338354}
}
@article{fds338423,
Author = {Li, Z and others},
Title = {Measurement of the tau neutrino cross section in atmospheric
neutrino oscillations with Super-Kamiokande},
Journal = {Phys. Rev.},
Volume = {D98},
Number = {5},
Pages = {052006-052006},
Publisher = {American Physical Society (APS)},
Year = {2018},
url = {http://dx.doi.org/10.1103/PhysRevD.98.052006},
Abstract = {Using 5326 days of atmospheric neutrino data, a search for
atmospheric tau neutrino appearance has been performed in
the Super-Kamiokande experiment. Super-Kamiokande measures
the tau normalization to be 1.47±0.32 under the assumption
of normal neutrino hierarchy, relative to the expectation of
unity with neutrino oscillation. The result excludes the
hypothesis of no-tau appearance with a significance level of
4.6σ. The inclusive charged-current tau neutrino cross
section averaged by the tau neutrino flux at
Super-Kamiokande is measured to be (0.94±0.20)×10-38 cm2.
The measurement is consistent with the Standard Model
prediction, agreeing to within 1.5σ.},
Doi = {10.1103/PhysRevD.98.052006},
Key = {fds338423}
}
@article{fds332875,
Author = {Abe, K and others},
Title = {Measurement of the single $π^0$ production rate in neutral
current neutrino interactions on water},
Journal = {Phys. Rev.},
Volume = {D97},
Number = {3},
Pages = {032002-032002},
Publisher = {American Physical Society (APS)},
Year = {2018},
url = {http://dx.doi.org/10.1103/PhysRevD.97.032002},
Abstract = {The single π0 production rate in neutral current neutrino
interactions on water in a neutrino beam with a peak
neutrino energy of 0.6 GeV has been measured using the PØD,
one of the subdetectors of the T2K near detector. The
production rate was measured for data taking periods when
the PØD contained water (2.64×1020 protons-on-target) and
also periods without water (3.49×1020 protons-on-target). A
measurement of the neutral current single π0 production
rate on water is made using appropriate subtraction of the
production rate with water in from the rate with water out
of the target region. The subtraction analysis yields
106±41±69 signal events where the uncertainties are
statistical (stat.) and systematic (sys.) respectively. This
is consistent with the prediction of 157 events from the
nominal simulation. The measured to expected ratio is
0.68±0.26(stat)±0.44(sys)±0.12(flux). The nominal
simulation uses a flux integrated cross section of
7.63×10-39 cm2 per nucleon with an average neutrino
interaction energy of 1.3 GeV.},
Doi = {10.1103/PhysRevD.97.032002},
Key = {fds332875}
}
@article{fds337338,
Author = {Abe, K and others},
Title = {Characterization of nuclear effects in muon-neutrino
scattering on hydrocarbon with a measurement of final-state
kinematics and correlations in charged-current pionless
interactions at T2K},
Journal = {Phys. Rev.},
Volume = {D98},
Number = {3},
Pages = {032003-032003},
Publisher = {American Physical Society (APS)},
Year = {2018},
url = {http://dx.doi.org/10.1103/PhysRevD.98.032003},
Abstract = {This paper reports measurements of final-state proton
multiplicity, muon and proton kinematics, and their
correlations in charged-current pionless neutrino
interactions, measured by the T2K ND280 near detector in its
plastic scintillator (C8H8) target. The data were taken
between years 2010 and 2013, corresponding to approximately
6×1020 protons on target. Thanks to their exploration of
the proton kinematics and of imbalances between the proton
and muon kinematics, the results offer a novel probe of the
nuclear-medium effects most pertinent to the (sub-)GeV
neutrino-nucleus interactions that are used in
accelerator-based long-baseline neutrino oscillation
measurements. These results are compared to many
neutrino-nucleus interaction models which all fail to
describe at least part of the observed phase space. In case
of events without a proton above a detection threshold in
the final state, a fully consistent implementation of the
local Fermi gas model with multinucleon interactions gives
the best description of the data. In the case of at least
one proton in the final state, the spectral function model
agrees well with the data, most notably when measuring the
kinematic imbalance between the muon and the proton in the
plane transverse to the incoming neutrino. Within the models
considered, only the existence of multinucleon interactions
are able to describe the extracted cross section within
regions of high transverse kinematic imbalance. The effect
of final-state interactions is also discussed.},
Doi = {10.1103/PhysRevD.98.032003},
Key = {fds337338}
}
@article{fds337016,
Author = {Abe, K and others},
Title = {Measurement of inclusive double-differential $ν_μ$
charged-current cross section with improved acceptance in
the T2K off-axis near detector},
Journal = {Phys. Rev.},
Volume = {D98},
Number = {1},
Pages = {012004-012004},
Publisher = {American Physical Society (APS)},
Year = {2018},
url = {http://dx.doi.org/10.1103/PhysRevD.98.012004},
Abstract = {We report a measurement of the flux-integrated cross section
for inclusive muon neutrino charged-current interactions on
carbon. The double-differential measurements are given as a
function of the muon momentum and angle. Relative to our
previous publication on this topic, these results have an
increased angular acceptance and higher statistics. The data
sample presented here corresponds to 5.7×1020 protons on
target. The total flux-integrated cross section is measured
to be (6.950±0.662)×10-39 cm2 nucleon-1 and is consistent
with our simulation.},
Doi = {10.1103/PhysRevD.98.012004},
Key = {fds337016}
}
@article{fds335619,
Author = {Hayato, Y and others},
Title = {Search for Neutrinos in Super-Kamiokande Associated with the
GW170817 Neutron-star Merger},
Journal = {Astrophys. J.},
Volume = {857},
Number = {1},
Pages = {L4-L4},
Publisher = {American Astronomical Society},
Year = {2018},
url = {http://dx.doi.org/10.3847/2041-8213/aabaca},
Abstract = {We report the results of a neutrino search in
Super-Kamiokande (SK) for coincident signals with the first
detected gravitational wave (GW) produced by a binary
neutron-star merger, GW170817, which was followed by a short
gamma-ray burst, GRB170817A, and a kilonova/macronova. We
searched for coincident neutrino events in the range from
3.5 MeV to ∼100 PeV, in a time window ±500 s around the
gravitational wave detection time, as well as during a
14-day period after the detection. No significant neutrino
signal was observed for either time window. We calculated
90% confidence level upper limits on the neutrino fluence
for GW170817. From the upward-going-muon events in the
energy region above 1.6 GeV, the neutrino fluence limit is
() cm-2 for muon neutrinos (muon antineutrinos), with an
error range of ±5around the zenith angle of NGC4993, and
the energy spectrum is under the assumption of an index
of-2. The fluence limit for neutrino energies less than 100
MeV, for which the emission mechanism would be different
than for higher-energy neutrinos, is also calculated. It is
6.6 × 107 cm-2 for anti-electron neutrinos under the
assumption of a Fermi-Dirac spectrum with average energy of
20 MeV.},
Doi = {10.3847/2041-8213/aabaca},
Key = {fds335619}
}
@article{fds335620,
Author = {Abe, K and others},
Title = {Atmospheric neutrino oscillation analysis with external
constraints in Super-Kamiokande I-IV},
Journal = {Phys. Rev.},
Volume = {D97},
Number = {7},
Pages = {072001-072001},
Publisher = {American Physical Society (APS)},
Year = {2018},
url = {http://dx.doi.org/10.1103/PhysRevD.97.072001},
Abstract = {An analysis of atmospheric neutrino data from all four run
periods of Super-Kamiokande optimized for sensitivity to the
neutrino mass hierarchy is presented. Confidence intervals
for Δm322, sin2θ23, sin2θ13 and δCP are presented for
normal neutrino mass hierarchy and inverted neutrino mass
hierarchy hypotheses, based on atmospheric neutrino data
alone. Additional constraints from reactor data on θ13 and
from published binned T2K data on muon neutrino
disappearance and electron neutrino appearance are added to
the atmospheric neutrino fit to give enhanced constraints on
the above parameters. Over the range of parameters allowed
at 90% confidence level, the normal mass hierarchy is
favored by between 91.9% and 94.5% based on the combined
Super-Kamiokande plus T2K result.},
Doi = {10.1103/PhysRevD.97.072001},
Key = {fds335620}
}
@article{fds335618,
Author = {Kachulis, C and others},
Title = {Search for Boosted Dark Matter Interacting With Electrons in
Super-Kamiokande},
Journal = {Phys. Rev. Lett.},
Volume = {120},
Number = {22},
Pages = {221301-221301},
Year = {2018},
url = {http://dx.doi.org/10.1103/PhysRevLett.120.221301},
Abstract = {A search for boosted dark matter using 161.9 kt yr of
Super-Kamiokande IV data is presented. We search for an
excess of elastically scattered electrons above the
atmospheric neutrino background, with a visible energy
between 100 MeV and 1 TeV, pointing back to the Galactic
center or the Sun. No such excess is observed. Limits on
boosted dark matter event rates in multiple angular cones
around the Galactic center and Sun are calculated. Limits
are also calculated for a baseline model of boosted dark
matter produced from cold dark matter annihilation or decay.
This is the first experimental search for boosted dark
matter from the Galactic center or the Sun interacting in a
terrestrial detector.},
Doi = {10.1103/PhysRevLett.120.221301},
Key = {fds335618}
}
@article{fds332876,
Author = {Abe, K and others},
Title = {First measurement of the $ν_μ$ charged-current cross
section on a water target without pions in the final
state},
Journal = {Phys. Rev.},
Volume = {D97},
Number = {1},
Pages = {012001-012001},
Publisher = {American Physical Society (APS)},
Year = {2018},
url = {http://dx.doi.org/10.1103/PhysRevD.97.012001},
Abstract = {This paper reports the first differential measurement of the
charged-current interaction cross section of νμ on water
with no pions in the final state. This flux-averaged
measurement has been made using the T2K experiment's
off-axis near detector, and is reported in doubly
differential bins of muon momentum and angle. The
flux-averaged total cross section in a restricted region of
phase space was found to be σ=(0.95±0.08(stat)±0.06(det
syst)±0.04(model syst)±0.08(flux))×10-38
cm2/n.},
Doi = {10.1103/PhysRevD.97.012001},
Key = {fds332876}
}
@article{fds348029,
Author = {Sussman, S and others},
Title = {Dinucleon and Nucleon Decay to Two-Body Final States with no
Hadrons in Super-Kamiokande},
Year = {2018},
url = {http://dx.doi.org/10.3847/2041-8213/ab5863},
Doi = {10.3847/2041-8213/ab5863},
Key = {fds348029}
}
@article{fds347284,
Author = {Abe, K and Abe, K and Ahn, SH and Aihara, H and Aimi, A and Akutsu, R and Andreopoulos, C and Anghel, I and Anthony, LHV and Antonova, M and Ashida, Y and Aushev, V and Barbi, M and Barker, GJ and Barr, G and Beltrame, P and Berardi, V and Bergevin, M and Berkman, S and Berns, L and Berry, T and Bhadra, S and Blaszczyk, FDM and Blondel, A and Bolognesi,
S and Boyd, SB and Bravar, A and Bronner, C and Buizza Avanzini and M and Cafagna, FS and Calland, R and Cao, S and Cartwright, SL and Catanesi,
MG and Checchia, C and Chen-Wishart, Z and Cheon, BG and Cheoun, MK and Cho, K and Choi, JH and Choi, K and Choi, KY and Chun, EJ and Cole, A and Coleman, J and Collazuol, G and Cowan, G and Cremonesi, L and Dealtry,
T and De Rosa and G and Densham, C and Dewhurst, D and Drakopoulou, E and Di
Lodovico, F and Drapier, O and Dumarchez, J and Dunne, P and Dziewiecki,
M and Emery, S and Esmaili, A and Evangelisti, A and Fernández-Martinez, E and Feusels, T and Finch, A and Fiorentini,
GA and Fiorillo, G and Fitton, M and Frankiewicz, K and Friend, M and Fujii, Y and Fukuda, Y and Fukuda, D and Ganezer, K and Ghosh, M and Giganti, C and Gonin, M and Grant, N and Gumplinger, P and Hadley, DR and Hartfiel, B and Hartz, M and Hayato, Y and Hayrapetyan, K and Hill, J and Hirota, S and Horiuchi, S and Ichikawa, AK and Iijima, T and Ikeda, M and Imber, J and Inoue, K and Insler, J and Intonti, RA and Ioannisian, A and Ishida, T and Ishino, H and Ishitsuka, M and Itow, Y and Iwamoto, K and Izmaylov, A and Jamieson, B and Jang, HI and Jang, JS and Jeon, SH and Jeong, KS and Jiang, M and Jonsson, P and Joo, KK and Kaboth, A and Kachulis, C and Kajita, T and Kang, SK and Kameda, J and Kataoka, Y and Katori, T and Kayrapetyan, K and Kearns, E and Khabibullin, M and Khotjantsev, A and Kim, CS and Kim, HB and Kim, HJ and Kim, JH and Kim,
J-S and Kim, JY and Kim, SB and Kim, SC and Kim, S-W and Kim, SY and Kim, TJ and Kim, W and King, S and Kishimoto, Y and Ko, P and Kobayashi, T and Koga, M and Konaka, A and Kormos, LL and Koshio, Y and Korzenev, A and Kowalik, KL and Kropp, WR and Kudenko, Y and Kurjata, R and Kutter, T and Kuze, M and Kwak,
K and Kwon, EH and Labarga, L and Lagoda, J and Lasorak, PJJ and Laveder,
M and Lawe, M and Learned, JG and Lee, CH and Lee, SJ and Lee, WJ and Lim, IT and Lindner, T and Litchfield, RP and Longhin, A and Loverre, P and Lou, T and Ludovici, L and Ma, W and Magaletti, L and Mahn, K and Malek, M and Maret,
L and Mariani, C and Martens, K and Marti, L and Martin, JF and Marzec, J and Matsuno, S and Mazzucato, E and McCarthy, M and McCauley, N and McFarland, KS and McGrew, C and Mefodiev, A and Mermod, P and Metelko,
C and Mezzetto, M and Migenda, J and Mijakowski, P and Minakata, H and Minamino, A and Mine, S and Mineev, O and Mitra, A and Miura, M and Mochizuki, T and Monroe, J and Moon, CS and Moon, DH and Moriyama, S and Mueller, T and Muheim, F and Murase, K and Muto, F and Nakahata, M and Nakajima, Y and Nakamura, K and Nakaya, T and Nakayama, S and Nantais,
C and Needham, M and Nicholls, T and Nishimura, Y and Noah, E and Nova, F and Nowak, J and Nunokawa, H and Obayashi, Y and Oh, YD and Oh, Y and O’Keeffe, HM and Okajima, Y and Okumura, K and Onishchuk, Y and O’Sullivan, E and O’Sullivan, L and Ovsiannikova, T and Owen, RA and Oyama, Y and Pérez, J and Pac, MY and Palladino, V and Palomino, JL and Paolone, V and Park, HS and Park, JC and Park, MG and Park, SC and Parker,
W and Parsa, S and Payne, D and Perkin, JD and Pidcott, C and Pinzon
Guerra, E and Playfer, S and Popov, B and Posiadala-Zezula, M and Poutissou, J-M and Pritchard, A and Prouse, NW and Pronost, G and Przewlocki, P and Quilain, B and Quinto, M and Radicioni, E and Ratoff,
PN and Retiere, F and Riccio, C and Richards, B and Rondio, E and Rose, HJ and Rott, C and Rountree, SD and Ruggeri, AC and Rychter, A and Ryu, D and Sacco, R and Sakuda, M and Sanchez, MC and Scantamburlo, E and Scott, M and Molina Sedgwick and S and Seiya, Y and Sekiguchi, T and Sekiya, H and Seo,
H and Seo, SH and Sgalaberna, D and Shah, R and Shaikhiev, A and Shimizu,
I and Shiozawa, M and Shitov, Y and Short, S and Simpson, C and Sinnis, G and Smy, MB and Snow, S and Sobczyk, J and Sobel, HW and Son, DC and Sonoda, Y and Spina, R and Stewart, T and Stone, JL and Suda, Y and Suwa, Y and Suzuki,
Y and Suzuki, AT and Svoboda, R and Taani, M and Tacik, R and Takeda, A and Takenaka, A and Taketa, A and Takeuchi, Y and Takhistov, V and Tanaka,
HA and Tanaka, HKM and Tanaka, H and Terri, R and Thiesse, M and Thompson,
LF and Thorpe, M and Tobayama, S and Touramanis, C and Towstego, T and Tsukamoto, T and Tsui, KM and Tzanov, M and Uchida, Y and Vagins, MR and Vasseur, G and Vilela, C and Vogelaar, RB and Walding, J and Walker, J and Ward, M and Wark, D and Wascko, MO and Weber, A and Wendell, R and Wilkes,
RJ and Wilking, MJ and Wilson, JR and Won, E and Xin, T and Yamamoto, K and Yanagisawa, C and Yano, T and Yasuda, O and Yen, S and Yershov, N and Yeum,
DN and Yokoyama, M and Yoo, HD and Yoo, J and Yoon, SC and Yoon, TS and Yoshida, T and Yu, I and Yu, M and Zalipska, J and Zaremba, K and Ziembicki, M and Zito, M and Zsoldos, S},
Title = {Physics potentials with the second Hyper-Kamiokande detector
in Korea},
Journal = {Progress of Theoretical and Experimental
Physics},
Volume = {2018},
Number = {6},
Publisher = {Oxford University Press (OUP)},
Year = {2018},
Month = {June},
url = {http://dx.doi.org/10.1093/ptep/pty044},
Doi = {10.1093/ptep/pty044},
Key = {fds347284}
}
@article{fds342147,
Author = {Wan, L and others},
Title = {Measurement of the neutrino-oxygen neutral-current
quasielastic cross section using atmospheric neutrinos at
Super-Kamiokande},
Journal = {Phys. Rev.},
Volume = {D99},
Number = {3},
Pages = {032005-032005},
Year = {2019},
url = {http://dx.doi.org/10.1103/PhysRevD.99.032005},
Abstract = {Neutral current (NC) interactions of atmospheric neutrinos
on oxygen form one of the major backgrounds in the search
for supernova relic neutrinos with water-based Cherenkov
detectors. The NC channel is dominated by neutrino
quasielastic (NCQE) scattering off nucleons inside O16
nuclei. In this paper we report the first measurement of
NCQE cross section using atmospheric neutrinos at
Super-Kamiokande (SK). The measurement used 2,778 live days
of SK-IV data with a fiducial volume of 22.5 kiloton water.
Within the visible energy window of 7.5-29.5 MeV, we
observed 117 events compared to the expected 71.9 NCQE
signal and 53.1 background events. Weighted by the
atmospheric neutrino spectrum from 160 MeV to 10 GeV, the
flux averaged NCQE cross section is measured to be
(1.01±0.17(stat.)-0.30+0.78(sys.))×10-38
cm2.},
Doi = {10.1103/PhysRevD.99.032005},
Key = {fds342147}
}
@article{fds345330,
Author = {Jiang, M and others},
Title = {Atmospheric Neutrino Oscillation Analysis with Improved
Event Reconstruction in Super-Kamiokande
IV},
Journal = {PTEP},
Volume = {2019},
Number = {5},
Pages = {053F01-053F01},
Year = {2019},
url = {http://dx.doi.org/10.1093/ptep/ptz015},
Abstract = {A new event reconstruction algorithm based on a maximum
likelihood method has been developed for Super-Kamiokande.
Its improved kinematic and particle identification
capabilities enable the analysis of atmospheric neutrino
data in a detector volume 32% larger than previous analyses
and increase the sensitivity to the neutrino mass
hierarchy.Analysis of a 253.9 kton•year exposure of the
Super-Kamiokande IV atmospheric neutrino data has yielded a
weak preference for the normal hierarchy, disfavoring the
inverted hierarchy at 74% assuming oscillations at the best
fit of the analysis.},
Doi = {10.1093/ptep/ptz015},
Key = {fds345330}
}
@article{fds347184,
Author = {Simpson, C and others},
Title = {Sensitivity of Super-Kamiokande with Gadolinium to Low
Energy Anti-neutrinos from Pre-supernova
Emission},
Journal = {Astrophys. J.},
Volume = {885},
Number = {2},
Pages = {133-133},
Year = {2019},
url = {http://dx.doi.org/10.3847/1538-4357/ab4883},
Abstract = {Supernova detection is a major objective of the
Super-Kamiokande (SK) experiment. In the next stage of SK
(SK-Gd), gadolinium (Gd) sulfate will be added to the
detector, which will improve the ability of the detector to
identify neutrons. A core-collapse supernova (CCSN) will be
preceded by an increasing flux of neutrinos and
antineutrinos, from thermal and weak nuclear processes in
the star, over a timescale of hours; some of which may be
detected at SK-Gd. This could provide an early warning of an
imminent CCSN, hours earlier than the detection of the
neutrinos from core collapse. Electron antineutrino
detection will rely on inverse beta decay events below the
usual analysis energy threshold of SK, so Gd loading is
vital to reduce backgrounds while maximizing detection
efficiency. Assuming normal neutrino mass ordering, more
than 200 events could be detected in the final 12 hr before
core collapse for a 15-25 solar mass star at around 200 pc,
which is representative of the nearest red supergiant to
Earth, α-Ori (Betelgeuse). At a statistical false alarm
rate of 1 per century, detection could be up to 10 hr before
core collapse, and a pre-supernova star could be detected by
SK-Gd up to 600 pc away. A pre-supernova alert could be
provided to the astrophysics community following gadolinium
loading.},
Doi = {10.3847/1538-4357/ab4883},
Key = {fds347184}
}
@article{fds348469,
Author = {Abe, K and others},
Title = {J-PARC Neutrino Beamline Upgrade Technical Design
Report},
Year = {2019},
Key = {fds348469}
}
@article{fds348389,
Author = {Hagiwara, K and others},
Title = {Search for Astronomical Neutrinos from Blazar TXS0506+056 in
Super-Kamiokande},
Journal = {Astrophys. J.},
Volume = {887},
Number = {1},
Pages = {L6-L6},
Year = {2019},
url = {http://dx.doi.org/10.3847/2041-8213/ab5863},
Abstract = {We report a search for astronomical neutrinos in the energy
region from several GeV to TeV in the direction of the
blazar TXS 0506+056 using the Super-Kamiokande detector
following the detection of a 100 TeV neutrinos from the same
location by the IceCube collaboration. Using
Super-Kamiokande neutrino data across several data samples
observed from 1996 April to 2018 February we have searched
for both a total excess above known backgrounds across the
entire period as well as localized excesses on smaller
timescales in that interval. No significant excess nor
significant variation in the observed event rate are found
in the blazar direction. Upper limits are placed on the
electron-and muon-neutrino fluxes at the 90% confidence
level as 6.0 × 10-7 and 4.5 × 10-7-9.3 × 10-10 [erg cm-2
s-1], respectively.},
Doi = {10.3847/2041-8213/ab5863},
Key = {fds348389}
}
@article{fds348641,
Author = {Abe, K and others},
Title = {Measurement of the muon neutrino charged-current single
$π^+$ production on hydrocarbon using the T2K off-axis near
detector ND280},
Volume = {101},
Number = {1},
Year = {2019},
url = {http://dx.doi.org/10.1103/PhysRevD.101.012007},
Abstract = {We report the measurements of the single and double
differential cross section of muon neutrino charged-current
interactions on carbon with a single positively charged pion
in the final state at the T2K off-axis near detector using
5.56×1020 protons on target. The analysis uses data control
samples for the background subtraction and the cross section
signal, defined as a single negatively charged muon and a
single positively charged pion exiting from the target
nucleus, is extracted using an unfolding method. The
model-dependent cross section, integrated over the T2K
off-axis neutrino beam spectrum peaking at 0.6 GeV, is
measured to be σ=(11.76±0.44(stat)±2.39(syst))×10-40 cm2
nucleon-1. Various differential cross sections are measured,
including the first measurement of the Adler angles for
single charged pion production in neutrino interactions with
heavy nuclei target.},
Doi = {10.1103/PhysRevD.101.012007},
Key = {fds348641}
}
@article{fds347929,
Author = {Walter, CW and Scolnic, DM and Slosar, A},
Title = {LSST Target of Opportunity proposal for locating a core
collapse supernova in our galaxy triggered by a neutrino
supernova alert},
Year = {2019},
Month = {January},
Abstract = {A few times a century, a core collapse supernova (CCSN)
occurs in our galaxy. When such galactic CCSNe happen, over
99\% of its gravitational binding energy is released in the
form of neutrinos. Over a period of tens of seconds, a
powerful neutrino flux is emitted from the collapsing star.
When the exploding shock wave finally reaches the surface of
the star, optical photons escaping the expanding stellar
envelope leave the star and eventually arrive at Earth as a
visible brightening. Crucially, although the neutrino signal
is prompt, the time to the shock wave breakout can be
minutes to many hours later. This means that the neutrino
signal will serve as an alert, warning the optical astronomy
community the light from the explosion is coming. Quickly
identifying the location of the supernova on the sky and
disseminating it to the all available ground and
spaced-based instruments will be critical to learn as much
as possible about the event. Some neutrino experiments can
report pointing information for these galactic CCSNe. In
particular, the Super-Kamiokande experiment can point to a
few degrees for CCSNe near the center of our galaxy. A CCSN
located 10 kpc from Earth is expected to result in a
pointing resolution on the order of 3 degrees. LSST's field
of view (FOV) is well matched to this initial search box.
LSSTs depth is also uniquely suited for identifying CCSNe
even if they fail or are obscured by the dust of the
galactic plane. This is a proposal to, upon receipt of such
an alert, prioritize the use of LSST for a full day of
observing to continuously monitor a pre-identified region of
sky and, by using difference imaging, identify and announce
the location of the supernova.},
Key = {fds347929}
}
@article{fds361363,
Author = {Abe, K and Aihara, H and Ajmi, A and Andreopoulos, C and Antonova, M and Aoki, S and Asada, Y and Ashida, Y and Atherton, A and Atkin, E and Attié,
D and Ban, S and Barbi, M and Barker, GJ and Barr, G and Batkiewicz, M and Beloshapkin, A and Berardi, V and Berns, L and Bhadra, S and Bian, J and Bienstock, S and Blondel, A and Boix, J and Bolognesi, S and Borg, J and Bordoni, S and Bourguille, B and Boyd, SB and Brailsford, D and Bravar,
A and Bronner, C and Browning, D and Avanzini, MB and Cadoux, F and Calabria, NF and Calcutt, J and Calland, RG and Calvet, D and Campbell,
T and Cao, S and Cartwright, SL and Castillo, R and Catanesi, MG and Ceria,
W and Cervera, A and Chappell, A and Cherdack, D and Chikuma, N and Christodoulou, G and Cicerchia, M and Clifton, A and Cogo, G and Colas,
P and Coleman, J and Collazuol, G and Coplowe, D and Cudd, A and Dabrowska,
A and Delbart, A and Roeck, AD and Rosa, GD and Dealtry, T and Denner, PF and Dennis, SR and Densham, C and Oliveira, RD and Dewhurst, D and Lodovico,
FD and Dokania, N and Dolan, S and Douqa, D and Drapier, O and Duffy, KE and Dumarchez, J and Dunne, PJ and Dziewiecki, M and Emery-Schrenk, S and Evangelisti, A and Favre, Y and Fedotov, S and Fernandez, P and Feusels,
T and Finch, AJ and Fiorentini, GA and Fiorillo, G and Fitton, M and Friend, M and Fujii, Y and Fujita, R and Fukuda, D and Fukuda, R and Fukuda, Y and Garcia, A and Giganti, C and Gizzarelli, F and Gonin, M and Gorin, A and Gramegna, F and Guida, M and Guigue, M and Hadley, DR and Haegel, L and Haigh, JT and Hamacher-Baumann, P and Hansen, D and Harada, J and Hartz, M and Hasegawa, T and Hastings, NC and Hayato, Y and Hiramoto, A and Hogan, M and Howell, R and Holeczek, J and Iacob, F and Ichikawa, AK and Ikeda, M and Imber, J and Intonti, RA and Ishida, T and Ishii, T and Ishitsuka, M and Iwai, E and Iwamoto, K and Izmaylov, A and Jamieson, B and Jesus-Valls, C and Jiang, M and Johnson, S and Jo, JH and Jonsson, P and Jung, CK and Kabirnezhad, M and Kaboth, AC and Kajita, T and Kakuno, H and Kameda, J and Kasetti, S and Kataoka, Y and Katori, T and Kearns, E and Khabibullin, M and Khotjantsev, A and Kikawa, T and Kim,
H and King, S and Kisiel, J and Knight, A and Knox, A and Kobayashi, T and Koch, L and Konaka, A and Kormos, LL and Korzenev, A and Kose, U and Kostin, A and Koshio, Y and Kowalik, K and Kropp, W and Kudenko, Y and Kuribayashi, S and Kurjata, R and Kutter, T and Kuze, M and Labarga, L and Lagoda, J and Lamont, I and Lamoureux, M and Laveder, M and Lawe, M and Lindner, T and Liptak, ZJ and Litchfield, RP and Li, X and Liu, S and Long,
KR and Longhin, A and Lopez, JP and Loverre, PF and Ludovici, L and Lu, X and Lux, T and Magaletti, L and Magro, L and Mahn, K and Malek, M and Manly, S and Marchi, T and Maret, L and Marino, AD and Martin, JF and Martynenko, S and Maruyama, T and Marzec, J and Matsubara, T and Matsushita, K and Matveev, V and Mavrokoridis, K and Mazzucato, E and McCarthy, M and McCauley, N and McFarland, KS and McGrew, C and Mefodiev, A and Mehl, B and Mermod, P and Metelko, C and Mezzetto, M and Michalowski, J and Mijakowski, P and Minamino, A and Mineev, O and Mine, S and Missert, A and Miura, M and Mladenov, D and Monsalvo, S and Moriyama, S and Morrison,
J and Mueller, TA and Mundet, J and Munteanu, L and Nagai, Y and Nakadaira,
T and Nakahata, M and Nakajima, Y and Nakamura, A and Nakamura, KG and Nakamura, K and Nakayama, S and Nakaya, T and Nakayoshi, K and Nantais,
C and Machado, LN and Nessi, M and Ngoc, TV and Nishikawa, K and Nishimura,
Y and Noah, E and Nonnenmacher, T and Novella, P and Nowak, J and O'Keeffe,
HM and Odagawa, T and Ohta, R and Okamoto, K and Okumura, K and Okusawa, T and Orain, Y and Ovsyannikova, T and Owen, RA and Oyama, Y and Palladino, V and Palomino, JL and Paolone, V and Parraud, JM and Pari, M and Parker, W and Parsa, S and Pasternak, J and Pastore, C and Pavin, M and Payne, D and Pepato, A and Perkin, JD and Pietropaolo, F and Pickard, L and Pickering, L and Guerra, ESP and Pizzirusso, O and Popov, B and Porthault, J and Posiadala-Zezula, M and Poutissou, J-M and Poutissou, R and Pozimski, J and Przewlocki, P and Przybilski, H and Quilain, B and Radermacher, T and Radicioni, E and Ratoff, PN and Ravonel, M and Rayner, MAM and Reinherz-Aronis, E and Resnati, F and Riallot, M and Riccio, C and Rojas, P and Romanino, G and Rondio, E and Rossi, F and Roth, S and Rychter, A and Sakashita, K and Sánchez, F and Scantamburlo, E and Scholberg, K and Schwehr, J and Scott, M and Seiya,
Y and Sekiguchi, T and Sekiya, H and Sgalaberna, D and Shaikina, A and Shah, R and Shaikhiev, A and Shaker, F and Shaw, D and Shiozawa, M and Shirahige, T and Shorrock, W and Smirnov, A and Smy, M and Sobczyk, JT and Sobel, H and Southwell, L and Spina, R and Steinmann, J and Stewart, T and Stowell, P and Suvorov, S and Suzuki, A and Suzuki, SY and Suzuki, Y and Szeptycka, M and Szoldos, S and Sztuc, A and Swierblewski, J and Tacik,
R and Tada, M and Tajima, M and Takeda, A and Takeuchi, Y and Tanaka, HK and Tanaka, HA and Teklu, A and Thompson, LF and Toki, W and Tomura, T and Touramanis, C and Tsukamoto, T and Tzanov, M and Uchida, MA and Uchida,
Y and Vagins, M and Vallari, Z and Van, NH and Vargas, D and Vasseur, G and Wachala, T and Walter, CW and Wark, D and Wascko, MO and Weber, A and Wendell, R and Whitehead, L and Wilkes, RJ and Wilking, MJ and Wilson,
JR and Wilson, RJ and Wret, C and Yamada, Y and Yamamoto, K and Yanagisawa,
C and Yang, G and Yano, T and Yasutome, K and Yen, S and Yershov, N and Yokoyama, M and Yoshida, T and Yuan, T and Yu, M and Zalewska, A and Zalipska, J and Zambelli, L and Zaremba, K and Ziembicki, M and Zilberman, P and Zimmerman, ED and Zito, M},
Title = {T2K ND280 Upgrade -- Technical Design Report},
Year = {2019},
Month = {January},
Abstract = {In this document, we present the Technical Design Report of
the Upgrade of the T2K Near Detector ND280. The goal of this
upgrade is to improve the Near Detector performance to
measure the neutrino interaction rate and to constrain the
neutrino interaction cross-sections so that the uncertainty
in the number of predicted events at Super-Kamiokande is
reduced to about 4%. This will allow to improve the physics
reach of the T2K-II project. This goal is achieved by
modifying the upstream part of the detector, adding a new
highly granular scintillator detector (Super-FGD), two new
TPCs (High-Angle TPC) and six TOF planes. Details about the
detector concepts, design and construction methods are
presented, as well as a first look at the test-beam data
taken in Summer 2018. An update of the physics studies is
also presented.},
Key = {fds361363}
}
@article{fds342536,
Author = {Ivezić, Ž and Kahn, SM and Tyson, JA and Abel, B and Acosta, E and Allsman, R and Alonso, D and Alsayyad, Y and Anderson, SF and Andrew, J and Angel, JRP and Angeli, GZ and Ansari, R and Antilogus, P and Araujo, C and Armstrong, R and Arndt, KT and Astier, P and Aubourg, E and Auza, N and Axelrod, TS and Bard, DJ and Barr, JD and Barrau, A and Bartlett, JG and Bauer, AE and Bauman, BJ and Baumont, S and Bechtol, E and Bechtol, K and Becker, AC and Becla, J and Beldica, C and Bellavia, S and Bianco, FB and Biswas, R and Blanc, G and Blazek, J and Blandford, RD and Bloom, JS and Bogart, J and Bond, TW and Booth, MT and Borgland, AW and Borne, K and Bosch, JF and Boutigny, D and Brackett, CA and Bradshaw, A and Brandt,
WN and Brown, ME and Bullock, JS and Burchat, P and Burke, DL and Cagnoli,
G and Calabrese, D and Callahan, S and Callen, AL and Carlin, JL and Carlson, EL and Chandrasekharan, S and Charles-Emerson, G and Chesley, S and Cheu, EC and Chiang, HF and Chiang, J and Chirino, C and Chow, D and Ciardi, DR and Claver, CF and Cohen-Tanugi, J and Cockrum,
JJ and Coles, R and Connolly, AJ and Cook, KH and Cooray, A and Covey, KR and Cribbs, C and Cui, W and Cutri, R and Daly, PN and Daniel, SF and Daruich,
F and Daubard, G and Daues, G and Dawson, W and Delgado, F and Dellapenna,
A and Peyster, RD and Val-Borro, MD and Digel, SW and Doherty, P and Dubois, R and Dubois-Felsmann, GP and Durech, J and Economou, F and Eifler, T and Eracleous, M and Emmons, BL and Neto,
AF},
Title = {LSST: From Science Drivers to Reference Design and
Anticipated Data Products},
Journal = {Astrophysical Journal},
Volume = {873},
Number = {2},
Year = {2019},
Month = {March},
url = {http://dx.doi.org/10.3847/1538-4357/ab042c},
Abstract = {We describe here the most ambitious survey currently planned
in the optical, the Large Synoptic Survey Telescope (LSST).
The LSST design is driven by four main science themes:
probing dark energy and dark matter, taking an inventory of
the solar system, exploring the transient optical sky, and
mapping the Milky Way. LSST will be a large, wide-field
ground-based system designed to obtain repeated images
covering the sky visible from Cerro Pachón in northern
Chile. The telescope will have an 8.4 m (6.5 m effective)
primary mirror, a 9.6 deg 2 field of view, a 3.2-gigapixel
camera, and six filters (ugrizy) covering the wavelength
range 320-1050 nm. The project is in the construction phase
and will begin regular survey operations by 2022. About 90%
of the observing time will be devoted to a deep-wide-fast
survey mode that will uniformly observe a 18,000 deg 2
region about 800 times (summed over all six bands) during
the anticipated 10 yr of operations and will yield a
co-added map to r ∼27.5. These data will result in
databases including about 32 trillion observations of 20
billion galaxies and a similar number of stars, and they
will serve the majority of the primary science programs. The
remaining 10% of the observing time will be allocated to
special projects such as Very Deep and Very Fast time domain
surveys, whose details are currently under discussion. We
illustrate how the LSST science drivers led to these choices
of system parameters, and we describe the expected data
products and their characteristics.},
Doi = {10.3847/1538-4357/ab042c},
Key = {fds342536}
}
@article{fds353919,
Author = {Slosar, A and Davis, T and Eisenstein, D and Hložek, R and Ishak-Boushaki, M and Mandelbaum, R and Marshall, P and Sakstein, J and White, M},
Title = {Dark Energy and Modified Gravity},
Year = {2019},
Month = {March},
Abstract = {Despite two decades of tremendous experimental and
theoretical progress, the riddle of the accelerated
expansion of the Universe remains to be solved. On the
experimental side, our understanding of the possibilities
and limitations of the major dark energy probes has evolved;
here we summarize the major probes and their crucial
challenges. On the theoretical side, the taxonomy of
explanations for the accelerated expansion rate is better
understood, providing clear guidance to the relevant
observables. We argue that: i) improving statistical
precision and systematic control by taking more data,
supporting research efforts to address crucial challenges
for each probe, using complementary methods, and relying on
cross-correlations is well motivated; ii) blinding of
analyses is difficult but ever more important; iii) studies
of dark energy and modified gravity are related; and iv) it
is crucial that R&D for a vibrant dark energy program in the
2030s be started now by supporting studies and technical R&D
that will allow embryonic proposals to mature. Understanding
dark energy, arguably the biggest unsolved mystery in both
fundamental particle physics and cosmology, will remain one
of the focal points of cosmology in the forthcoming
decade.},
Key = {fds353919}
}
@article{fds353918,
Author = {Drlica-Wagner, A and Mao, Y-Y and Adhikari, S and Armstrong, R and Banerjee, A and Banik, N and Bechtol, K and Bird, S and Boddy, KK and Bonaca, A and Bovy, J and Buckley, MR and Bulbul, E and Chang, C and Chapline, G and Cohen-Tanugi, J and Cuoco, A and Cyr-Racine, F-Y and Dawson, WA and Rivero, AD and Dvorkin, C and Erkal, D and Fassnacht, CD and García-Bellido, J and Giannotti, M and Gluscevic, V and Golovich, N and Hendel, D and Hezaveh, YD and Horiuchi, S and Jee, MJ and Kaplinghat, M and Keeton, CR and Koposov, SE and Lam, CY and Li, TS and Lu, JR and Mandelbaum, R and McDermott, SD and McNanna, M and Medford, M and Meyer,
M and Marc, M and Murgia, S and Nadler, EO and Necib, L and Nuss, E and Pace,
AB and Peter, AHG and Polin, DA and Prescod-Weinstein, C and Read, JI and Rosenfeld, R and Shipp, N and Simon, JD and Slatyer, TR and Straniero,
O and Strigari, LE and Tollerud, E and Tyson, JA and Wang, M-Y and Wechsler, RH and Wittman, D and Yu, H-B and Zaharijas, G and Ali-Haïmoud, Y and Annis, J and Birrer, S and Biswas, R and Blazek, J and Brooks, AM and Buckley-Geer, E and Caputo, R and Charles, E and Digel,
S and Dodelson, S and Flaugher, B and Frieman, J and Gawiser, E and Hearin,
AP and Hložek, R and Jain, B and Jeltema, TE and Koushiappas, SM and Lisanti, M and LoVerde, M and Mishra-Sharma, S and Newman, JA and Nord,
B and Nourbakhsh, E and Ritz, S and Robertson, BE and Sánchez-Conde,
MA and Slosar, A and Tait, TMP and Verma, A and Vilalta, R and Walter, CW and Yanny, B and Zentner, AR},
Title = {Probing the Fundamental Nature of Dark Matter with the Large
Synoptic Survey Telescope},
Year = {2019},
Month = {April},
Abstract = {Astrophysical and cosmological observations currently
provide the only robust, empirical measurements of dark
matter. Future observations with Large Synoptic Survey
Telescope (LSST) will provide necessary guidance for the
experimental dark matter program. This white paper
represents a community effort to summarize the science case
for studying the fundamental physics of dark matter with
LSST. We discuss how LSST will inform our understanding of
the fundamental properties of dark matter, such as particle
mass, self-interaction strength, non-gravitational couplings
to the Standard Model, and compact object abundances.
Additionally, we discuss the ways that LSST will complement
other experiments to strengthen our understanding of the
fundamental characteristics of dark matter. More information
on the LSST dark matter effort can be found at
https://lsstdarkmatter.github.io/ .},
Key = {fds353918}
}
@article{fds348028,
Author = {Bechtol, K and Drlica-Wagner, A and Abazajian, KN and Abidi, M and Adhikari, S and Ali-Ha\i\ensuremath\ddotmoud, Y and Annis, J and Ansarinejad, B and Armstrong, R and Asorey, J and Baccigalupi, C and Banerjee, A and Banik, N and Bennett, C and Beutler, F and Bird, S and Birrer, S and Biswas, R and Biviano, A and Blazek, J and Boddy, KK and Bonaca, A and Borrill, J and Bose, S and Bovy, J and Frye, B and Brooks,
AM and Buckley, MR and Buckley-Geer, E and Bulbul, E and Burchat, PR and Burgess, C and Calore, F and Caputo, R and Castorina, E and Chang, C and Chapline, G and Charles, E and Chen, X and Clowe, D and Cohen-Tanugi, J and Comparat, J and Croft, RAC and Cuoco, A and Cyr-Racine, F-Y and D’Amico, G and Davis, TM and Dawson, WA and de la Macorra, A and Di
Valentino, E and Rivero, AD and Digel, S and Dodelson, S and Doré, O and Dvorkin, C and Eckner, C and Ellison, J and Erkal, D and Farahi, A and Fassnacht, CD and Ferreira, PG and Flaugher, B and Foreman, S and Friedrich, O and Frieman, J and García-Bellido, J and Gawiser, E and Gerbino, M and Giannotti, M and Gill, MSS and Gluscevic, V and Golovich,
N and Gontcho, SGA and González-Morales, AX and Grin, D and Gruen, D and Hearin, AP and Hendel, D and Hezaveh, YD and Hirata, CM and Hlo\vzek, R and Horiuchi, S and Jain, B and Jee, MJ and Jeltema, TE and Kamionkowski, M and Kaplinghat, M and Keeley, RE and Keeton, CR and Khatri, R and Koposov,
SE and Koushiappas, SM and Kovetz, ED and Lahav, O and Lam, C and Lee, C-H and Li, TS and Liguori, M and Lin, T and Lisanti, M and LoVerde, M and Lu, JR and Mandelbaum, R and Mao, Y-Y and McDermott, SD and McNanna, M and Medford,
M and Meerburg, PD and Meyer, M and Mirbabayi, M and Mishra-Sharma, S and Marc, M and More, S and Moustakas, J and Mu noz, JB and Murgia, S and Myers, AD and Nadler, EO and Necib, L and Newburgh, L and Newman, JA and Nord, B and Nourbakhsh, E and Nuss, E and O’Connor, P and Pace, AB and Padmanabhan, H and Palmese, A and Peiris, HV and Peter, AHG and Piacentni, F and Plazas, A and Polin, DA and Prakash, A and Prescod-Weinstein, C and Read, JI and Ritz, S and Robertson, BE and Rose, B and Rosenfeld, R and Rossi, G and Samushia, L and Sánchez, J and Sánchez-Conde, MA and Schaan, E and Sehgal, N and Senatore, L and Seo,
H-J and Shafieloo, A and Shan, H and Shipp, N and Simon, JD and Simon, S and Slatyer, TR and Slosar, AV and Sridhar, S and Stebbins, A and Straniero,
O and Strigari, LE and Tait, TMP and Tollerud, E and Troxel, MA and Tyson,
JA and Uhlemann, C and Uren na-López, LA and Verma, A and Vilalta, R and Walter, CW and Wang, M-Y and Watson, S and Wechsler, RH and Wittman, D and Xu, W and Yanny, B and Young, S and Yu, H-B and Zaharijas, G and Zentner,
AR and Zuntz, J},
Title = {Dark Matter Science in the Era of LSST},
Journal = {\baas},
Volume = {51},
Pages = {207-207},
Year = {2019},
Month = {May},
Key = {fds348028}
}
@article{fds353878,
Author = {Zyla, PA and Barnett, RM and Beringer, J and Dahl, O and Dwyer, DA and Groom, DE and Lin, CJ and Lugovsky, KS and Pianori, E and Robinson, DJ and Wohl, CG and Yao, WM and Agashe, K and Aielli, G and Allanach, BC and Amsler, C and Antonelli, M and Aschenauer, EC and Asner, DM and Baer, H and Banerjee, S and Baudis, L and Bauer, CW and Beatty, JJ and Belousov, VI and Bethke, S and Bettini, A and Biebel, O and Black, KM and Blucher, E and Buchmuller, O and Burkert, V and Bychkov, MA and Cahn, RN and Carena, M and Ceccucci, A and Cerri, A and Chakraborty, D and Sekhar Chivukula and R and Cowan, G and D'Ambrosio, G and Damour, T and de Florian, D and de
Gouvêa, A and DeGrand, T and de Jong, P and Dissertori, G and Dobrescu,
BA and D'Onofrio, M and Doser, M and Drees, M and Dreiner, HK and Eerola,
P and Egede, U and Eidelman, S and Ellis, J and Erler, J and Ezhela, VV and Fetscher, W and Fields, BD and Foster, B and Freitas, A and Gallagher,
H and Garren, L and Gerber, HJ and Gerbier, G and Gershon, T and Gershtein,
Y and Gherghetta, T and Godizov, AA and Gonzalez-Garcia, MC and Goodman,
M and Grab, C and Gritsan, AV and Grojean, C and Grünewald, M and Gurtu,
A and Gutsche, T and Haber, HE and Hanhart, C and Hashimoto, S and Hayato,
Y and Hebecker, A and Heinemeyer, S and Heltsley, B and Hernández-Rey,
JJ and Hikasa, K and Hisano, J and Höcker, A and Holder, J and Holtkamp,
A and Huston, J and Hyodo, T and Johnson, KF and Kado, M and Karliner, M and Katz, UF and Kenzie, M and Khoze, VA and Klein, SR},
Title = {Review of particle physics},
Journal = {Progress of Theoretical and Experimental
Physics},
Volume = {2020},
Number = {8},
Pages = {1-2093},
Year = {2020},
Month = {January},
url = {http://dx.doi.org/10.1093/ptep/ptaa104},
Abstract = {The Review summarizes much of particle physics and
cosmology. Using data from previous editions, plus 3,324 new
measurements from 878 papers, we list, evaluate, and average
measured properties of gauge bosons and the recently
discovered Higgs boson, leptons, quarks, mesons, and
baryons. We summarize searches for hypothetical particles
such as supersymmetric particles, heavy bosons, axions, dark
photons, etc. Particle properties and search limits are
listed in Summary Tables. We give numerous tables, figures,
formulae, and reviews of topics such as Higgs Boson Physics,
Supersymmetry, Grand Unified Theories, Neutrino Mixing, Dark
Energy, Dark Matter, Cosmology, Particle Detectors,
Colliders, Probability and Statistics. Among the 120 reviews
are many that are new or heavily revised, including a new
review on High Energy Soft QCD and Diffraction and one on
the Determination of CKM Angles from B Hadrons. The Review
is divided into two volumes. Volume 1 includes the Summary
Tables and 98 review articles. Volume 2 consists of the
Particle Listings and contains also 22 reviews that address
specific aspects of the data presented in the Listings. The
complete Review (both volumes) is published online on the
website of the Particle Data Group (pdg.lbl.gov) and in a
journal. Volume 1 is available in print as the PDG Book. A
Particle Physics Booklet with the Summary Tables and
essential tables, figures, and equations from selected
review articles is available in print and as a web version
optimized for use on phones as well as an Android
app.},
Doi = {10.1093/ptep/ptaa104},
Key = {fds353878}
}
@article{fds349341,
Author = {Tanaka, M and Abe, K and Bronner, C and Hayato, Y and Ikeda, M and Imaizumi, S and Ito, H and Kameda, J and Kataoka, Y and Kato, Y and Kishimoto, Y and Marti, L and Miura, M and Moriyama, S and Mochizuki, T and Nakahata, M and Nakajima, Y and Nakayama, S and Okada, T and Okamoto, K and Orii, A and Pronost, G and Sekiya, H and Shiozawa, M and Sonoda, Y and Takeda, A and Takenaka, A and Tanaka, H and Yano, T and Akutsu, R and Kajita, T and Okumura, K and Wang, R and Xia, J and Bravo-Berguno, D and Labarga, L and Fernandez, P and Blaszczyk, FDM and Kearns, E and Raaf,
JL and Stone, JL and Wan, L and Wester, T and Bian, J and Griskevich, NJ and Kropp, WR and Locke, S and Mine, S and Smy, MB and Sobel, HW and Takhistov,
V and Weatherly, P and Hill, J and Kim, JY and Lim, IT and Park, RG and Bodur,
B and Scholberg, K and Walter, CW and Coffani, A and Drapier, O and El
Hedri, S and Gonin, M and Mueller, TA and Paganini, P and Ishizuka, T and Nakamura, T and Jang, JS and Learned, JG and Matsuno, S and Litchfield,
RP and Sztuc, AA and Uchida, Y and Berardi, V and Catanesi, MG and Radicioni, E and Calabria, NF and De Rosa and G and Collazuol, G and Iacob,
F and Ludovici, L and Nishimura, Y and Cao, S and Friend, M and Hasegawa,
T and Ishida, T and Kobayashi, T and Nakadaira, T and Nakamura, K and Oyama, Y and Sakashita, K and Sekiguchi, T and Tsukamoto, T and Hasegawa, M and Isobe, Y and Miyabe, H and Nakano, Y and Shiozawa, T and Sugimoto, T and Suzuki, AT and Takeuchi, Y and Ali, A and Ashida, Y and Hirota, S and Jiang, M and Kikawa, T and Mori, M and Nakamura, K and Nakaya, T and Wendell, RA and Anthony, LH and McCauley, N and Mehta, P and Pritchard, A and Tsui, KM and Fukuda, Y and Itow, Y and Niwa, T and Taani,
M and Tsukada, M and Mijakowski, P and Frankiewicz, K and Jung, CK and Vilela, C and Wilking, MJ and Yanagisawa, C and Fukuda, D and Harada, M and Hagiwara, K and Horai, T and Ishino, H and Ito, S and Koshio, Y and Sakuda,
M and Takahira, Y and Xu, C and Kuno, Y and Barrow, D and Cook, L and Simpson,
C and Wark, D and Nova, F and Boschi, T and Di Lodovico and F and Sedgwick,
SM and Zsoldos, S and Kim, SB and Yang, JY and Thiesse, M and Thompson, L and Okazawa, H and Choi, Y and Nishijima, K and Koshiba, M and Yokoyama, M and Goldsack, A and Martens, K and Quilain, B and Suzuki, Y and Vagins, MR and Kuze, M and Yoshida, T and Ishitsuka, M and Matsumoto, R and Ohta, K and Martin, JF and Nantais, CM and Tanaka, HA and Towstego, T and Hartz, M and Konaka, A and de Perio, P and Prouse, NW and Chen, S and Xu, BD and Richards, B and Jamieson, B and Walker, J and Minamino, A and Pintaudi,
G},
Title = {Search for proton decay into three charged leptons in 0.37
megaton-years exposure of the Super-Kamiokande},
Journal = {PHYSICAL REVIEW D},
Volume = {101},
Number = {5},
Pages = {12 pages},
Publisher = {AMER PHYSICAL SOC},
Year = {2020},
Month = {March},
url = {http://dx.doi.org/10.1103/PhysRevD.101.052011},
Abstract = {© 2020 authors. A search for proton decay into three
charged leptons has been performed by using 0.37 Mton·years
of data collected in Super-Kamiokande. All possible
combinations of electrons, muons, and their antiparticles
consistent with charge conservation were considered as decay
modes. No significant excess of events has been found over
the background, and lower limits on the proton lifetime
divided by the branching ratio have been obtained. The
limits range between 9.2×1033 and 3.4×1034 years at 90%
confidence level, improving by more than an order of
magnitude upon limits from previous experiments. A first
limit has been set for the p→μ-e+e+ mode.},
Doi = {10.1103/PhysRevD.101.052011},
Key = {fds349341}
}
@article{fds353111,
Author = {Sanchez, J and Walter, CW and Awan, H and Chiang, J and Daniel, SF and Gawiser, E and Glanzman, T and Kirkby, D and Mandelbaum, R and Slosar,
A and Wood-Vasey, WM and Alsayyad, Y and Burke, CJ and Digel, SW and Jarvis, M and Johnson, T and Kelly, H and Krughoff, S and Lupton, RH and Marshall, PJ and Peterson, JR and Price, PA and Sembroski, G and Van
Klaveren, B and Wiesner, MP and Xin, B},
Title = {The LSST DESC data challenge 1: Generation and analysis of
synthetic images for next-generation surveys},
Journal = {Monthly Notices of the Royal Astronomical
Society},
Volume = {497},
Number = {1},
Pages = {210-228},
Publisher = {Oxford University Press (OUP)},
Year = {2020},
Month = {September},
url = {http://dx.doi.org/10.1093/mnras/staa1957},
Abstract = {Data Challenge 1 (DC1) is the first synthetic data set
produced by the Rubin Observatory Legacy Survey of Space and
Time (LSST) Dark Energy Science Collaboration (DESC). DC1 is
designed to develop and validate data reduction and analysis
and to study the impact of systematic effects that will
affect the LSST data set. DC1 is comprised of r-band
observations of 40 deg2 to 10 yr LSST depth. We present each
stage of the simulation and analysis process: (a)
generation, by synthesizing sources from cosmological N-body
simulations in individual sensor-visit images with different
observing conditions; (b) reduction using a development
version of the LSST Science Pipelines; and (c) matching to
the input cosmological catalogue for validation and testing.
We verify that testable LSST requirements pass within the
fidelity of DC1. We establish a selection procedure that
produces a sufficiently clean extragalactic sample for
clustering analyses and we discuss residual sample
contamination, including contributions from inefficiency in
star-galaxy separation and imperfect deblending. We compute
the galaxy power spectrum on the simulated field and
conclude that: (i) survey properties have an impact of 50
per cent of the statistical uncertainty for the scales and
models used in DC1; (ii) a selection to eliminate artefacts
in the catalogues is necessary to avoid biases in the
measured clustering; and (iii) the presence of bright
objects has a significant impact (2-6) in the estimated
power spectra at small scales (> 1200), highlighting the
impact of blending in studies at small angular scales in
LSST.},
Doi = {10.1093/mnras/staa1957},
Key = {fds353111}
}
@article{fds353782,
Author = {Abe, K and Bronner, C and Haga, Y and Hayato, Y and Ikeda, M and Imaizumi,
S and Ito, H and Iyogi, K and Kameda, J and Kataoka, Y and Kato, Y and Kishimoto, Y and Marti, L and Miura, M and Moriyama, S and Mochizuki, T and Nagao, Y and Nakahata, M and Nakajima, Y and Nakajima, T and Nakayama,
S and Okada, T and Okamoto, K and Orii, A and Pronost, G and Sekiya, H and Shiozawa, M and Sonoda, Y and Takeda, A and Takenaka, A and Tanaka, H and Tasaka, S and Tomura, T and Ueno, K and Yano, T and Yokozawa, T and Akutsu,
R and Han, S and Irvine, T and Kajita, T and Kametani, I and Lee, KP and Mclachlan, T and Okumura, K and Richard, E and Tashiro, T and Wang, R and Xia, J and Bravo-Berguño, D and Labarga, L and Fernandez, P and Blaszczyk, FDM and Gustafson, J and Kachulis, C and Kearns, E and Raaf,
JL and Stone, JL and Sulak, LR and Sussman, S and Wan, L and Wester, T and Berkman, S and Tobayama, S and Bian, J and Carminati, G and Elnimr, M and Griskevich, NJ and Kropp, WR and Locke, S and Mine, S and Renshaw, A and Smy, MB and Sobel, HW and Takhistov, V and Weatherly, P and Hartfiel,
BL and Hill, J and Keig, WE and Hong, N and Kim, JY and Lim, IT and Park, RG and Akiri, T and Bodur, B and Himmel, A and Li, Z and O'sullivan, E and Scholberg, K and Walter, CW and Wongjirad, T and Coffani, A and Drapier,
O and El Hedri and S and Giampaolo, A and Gonin, M and Imber, J and Mueller,
TA and Paganini, P and Quilain, B and Ishizuka, T},
Title = {Indirect search for dark matter from the Galactic Center and
halo with the Super-Kamiokande detector},
Journal = {Physical Review D},
Volume = {102},
Number = {7},
Year = {2020},
Month = {October},
url = {http://dx.doi.org/10.1103/PhysRevD.102.072002},
Abstract = {We present a search for an excess of neutrino interactions
due to dark matter in the form of weakly interacting massive
particles (WIMPs) annihilating in the Galactic center or
halo based on the data set of Super-Kamiokande-I, -II, -III
and -IV taken from 1996 to 2016. We model the neutrino flux,
energy, and flavor distributions assuming WIMP
self-annihilation is dominant to νν¯, μ+μ-, bb¯, or
W+W-. The excess is in comparison to atmospheric neutrino
interactions which are modeled in detail and fit to data.
Limits on the self-annihilation cross section σ are derived
for WIMP masses in the range 1 GeV to 10 TeV, reaching as
low as 9.6×10-23 cm3 s-1 for 5 GeV WIMPs in bb¯ mode and
1.2×10-24 cm3 s-1 for 1 GeV WIMPs in νν¯ mode. The
obtained sensitivity of the Super-Kamiokande detector to
WIMP masses below several tens of GeV is the best among
similar indirect searches to date.},
Doi = {10.1103/PhysRevD.102.072002},
Key = {fds353782}
}
@article{fds353534,
Author = {Amon, A and Bechtol, K and Connolly, AJ and Digel, SW and Drlica-Wagner,
A and Gawiser, E and Jarvis, M and Jha, SW and Linden, AVD and Moniez, M and Narayan, G and Regnault, N and Sevilla-Noarbe, I and Schmidt, SJ and Suyu, SH and Walter, CW},
Title = {Recommended Target Fields for Commissioning the Vera C.
Rubin Observatory},
Year = {2020},
Month = {October},
Abstract = {The commissioning team for the Vera C. Rubin observatory is
planning a set of engineering and science verification
observations with the Legacy Survey of Space and Time (LSST)
commissioning camera and then the Rubin Observatory LSST
Camera. The time frame for these observations is not yet
fixed, and the commissioning team will have flexibility in
selecting fields to observe. In this document, the Dark
Energy Science Collaboration (DESC) Commissioning Working
Group presents a prioritized list of target fields
appropriate for testing various aspects of DESC-relevant
science performance, grouped by season for visibility from
Rubin Observatory at Cerro Pachon. Our recommended fields
include Deep-Drilling fields (DDFs) to full LSST depth for
photo-$z$ and shape calibration purposes, HST imaging fields
to full depth for deblending studies, and an $\sim$200
square degree area to 1-year depth in several filters for
higher-level validation of wide-area science cases for DESC.
We also anticipate that commissioning observations will be
needed for template building for transient science over a
broad RA range. We include detailed descriptions of our
recommended fields along with associated references. We are
optimistic that this document will continue to be useful
during LSST operations, as it provides a comprehensive list
of overlapping data-sets and the references describing
them.},
Key = {fds353534}
}
@article{fds354017,
Author = {Collaboration, S-K and Takenaka, A and Abe, K and Bronner, C and Hayato,
Y and Ikeda, M and Imaizumi, S and Ito, H and Kameda, J and Kataoka, Y and Kato, Y and Kishimoto, Y and Marti, L and Miura, M and Moriyama, S and Mochizuki, T and Nagao, Y and Nakahata, M and Nakajima, Y and Nakayama,
S and Okada, T and Okamoto, K and Orii, A and Pronost, G and Sekiya, H and Shiozawa, M and Sonoda, Y and Suzuki, Y and Takeda, A and Takemoto, Y and Tanaka, H and Yano, T and Akutsu, R and Han, S and Kajita, T and Okumura,
K and Tashiro, T and Wang, R and Xia, J and Bravo-Berguno, D and Labarga,
L and Fernandez, P and Zaldivar, B and Blaszczyk, FDM and Kearns, E and Raaf, JL and Stone, JL and Wan, L and Wester, T and Pointon, BW and Bian,
J and Griskevich, NJ and Kropp, WR and Locke, S and Mine, S and Smy, MB and Sobel, HW and Takhistov, V and Weatherly, P and Ganezer, KS and Hill, J and Kim, JY and Lim, IT and Park, RG and Bodur, B and Scholberg, K and Walter,
CW and Coffani, A and Drapier, O and Hedri, SE and Giampaolo, A and Gonin,
M and Mueller, TA and Paganini, P and Quilain, B and Ishizuka, T and Nakamura, T and Jang, JS and Learned, JG and Matsuno, S and Anthony,
LHV and Litchfield, RP and Sztuc, AA and Uchida, Y and Berardi, V and Catanesi, MG and Radicioni, E and Calabria, NF and Machado, LN and Rosa,
GD and Collazuol, G and Iacob, F and Lamoureux, M and Ospina, N and Ludovici, L and Nishimura, Y and Cao, S and Friend, M and Hasegawa, T and Ishida, T and Jakkapu, M and Kobayashi, T and Matsubara, T and Nakadaira, T and Nakamura, K and Oyama, Y and Sakashita, K and Sekiguchi, T and Tsukamoto, T and Hasegawa, M and Isobe, Y and Miyabe,
H and Nakano, Y and Shiozawa, T and Sugimoto, T and Suzuki, AT and Takeuchi, Y and Yamamoto, S and Ali, A and Ashida, Y and Feng, J and Hirota, S and Ichikawa, AK and Jiang, M and Kikawa, T and Mori, M and Nakamura, KE and Nakaya, T and Wendell, RA and Yasutome, K and McCauley,
N and Mehta, P and Pritchard, A and Tsui, KM and Fukuda, Y and Itow, Y and Menjo, H and Niwa, T and Sato, K and Taani, M and Tsukada, M and Mijakowski, P and Frankiewicz, K and Jung, CK and Santucci, G and Vilela, C and Wilking, MJ and Yanagisawa, C and Fukuda, D and Harada, M and Hagiwara, K and Horai, T and Ishino, H and Ito, S and Koshio, Y and Ma, W and Piplani, N and Sakai, S and Sakuda, M and Takahira, Y and Xu, C and Kuno,
Y and Barr, G and Barrow, D and Cook, L and Simpson, C and Wark, D and Nova,
F and Boschi, T and Lodovico, FD and Sedgwick, SM and Zsoldos, S and Yang,
JY and Jenkins, SJ and McElwee, JM and Thiesse, MD and Thompson, LF and Okazawa, H and Choi, Y and Kim, SB and Yu, I and Nishijima, K and Koshiba,
M and Iwamoto, K and Ogawa, N and Yokoyama, M and Goldsack, A and Martens,
K and Vagins, MR and Kuze, M and Tanaka, M and Yoshida, T and Inomoto, M and Ishitsuka, M and Matsumoto, R and Ohta, K and Shinoki, M and Martin, JF and Nantais, CM and Tanaka, HA and Towstego, T and Hartz, M and Konaka, A and Perio, PD and Prouse, NW and Chen, S and Xu, BD and Posiadala-Zezula, M and Richards, B and Jamieson, B and Walker, J and Minamino, A and Pintaudi,
G and Sasaki, R},
Title = {Search for Proton Decay via $p\to e^+π^0$ and $p\to
μ^+π^0$ with an Enlarged Fiducial Volume in
Super-Kamiokande I-IV},
Year = {2020},
Month = {October},
Abstract = {We have searched for proton decay via $p\to e^+\pi^0$ and
$p\to \mu^+\pi^0$ modes with the enlarged fiducial volume
data of Super-Kamiokande from April 1996 to May 2018, which
corresponds to 450 kton$\cdot$years exposure. We have
accumulated about 25% more livetime and enlarged the
fiducial volume of the Super-Kamiokande detector from 22.5
kton to 27.2 kton for this analysis, so that 144
kton$\cdot$years of data, including 78 kton$\cdot$years of
additional fiducial volume data, has been newly analyzed. No
candidates have been found for $p\to e^+\pi^0$ and one
candidate remains for $p\to \mu^+\pi^0$ in the conventional
22.5 kton fiducial volume and it is consistent with the
atmospheric neutrino background prediction. We set lower
limits on the partial lifetime for each of these modes:
$\tau/B(p\to e^+\pi^0) > 2.4 \times 10^{34}$ years and
$\tau/B(p\to \mu^+\pi^0) > 1.6 \times 10^{34}$ years at 90%
confidence level.},
Key = {fds354017}
}
@article{fds354015,
Author = {Collaboration, S-K and Abe, K and Bronner, C and Hayato, Y and Ikeda, M and Imaizumi, S and Ito, H and Kameda, J and Kataoka, Y and Miura, M and Moriyama, S and Nagao, Y and Nakahata, M and Nakajima, Y and Nakayama,
S and Okada, T and Okamoto, K and Orii, A and Pronost, G and Sekiya, H and Shiozawa, M and Sonoda, Y and Suzuki, Y and Takeda, A and Takemoto, Y and Takenaka, A and Tanaka, H and Yano, T and Akutsu, R and Han, S and Kajita,
T and Okumura, K and Tashiro, T and Wang, R and Xia, J and Bravo-Berguño,
D and Labarga, L and Marti, L and Zaldivar, B and Blaszczyk, FDM and Kearns, E and Raaf, JL and Stone, JL and Wan, L and Wester, T and Pointin,
BW and Bian, J and Griskevich, NJ and Kropp, WR and Locke, S and Mine, S and Smy, MB and Sobel, HW and Takhistov, V and Weatherly, P and Hill, J and Kim, JY and Lim, IT and Park, RG and Bodur, B and Scholberg, K and Walter,
CW and Bernard, L and Coffani, A and Drapier, O and Hedri, SE and Giampaolo, A and Gonin, M and Mueller, TA and Paganini, P and Quilain,
B and Ishizuka, T and Nakamura, T and Jang, JS and Learned, JG and Anthony,
LHV and Sztuc, AA and Uchida, Y and Berardi, V and Catanesi, MG and Radicioni, E and Calabria, NF and Machado, LN and Rosa, GD and Collazuol, G and Iacob, F and Lamoureux, M and Ospina, N and Ludovici,
L and Nishimura, Y and Cao, S and Friend, M and Hasegawa, T and Ishida, T and Jakkapu, M and Kobayashi, T and Matsubara, T and Nakadaira, T and Nakamura, K and Oyama, Y and Sakashita, K and Sekiguchi, T and Tsukamoto, T and Nakano, Y and Shiozawa, T and Suzuki, AT and Takeuchi,
Y and Yamamoto, S and Ali, A and Ashida, Y and Feng, J and Hirota, S and Ichikawa, AK and Kikawa, T and Mori, M and Nakaya, T and Wendell, RA and Yasutome, Y and Fernandez, P and McCauley, N and Mehta, P and Pritchard,
A and Tsui, KM and Fukuda, Y and Itow, Y and Menjo, H and Niwa, T and Sato, K and Tsukada, M and Mijakowski, P and Jung, CK and Vilela, C and Wilking, MJ and Yanagisawa, C and Harada, M and Hagiwara, K and Horai, T and Ishino, H and Ito, S and Koshio, Y and Ma, W and Piplani, N and Sakai, S and Kuno, Y and Barr, G and Barrow, D and Cook, L and Goldsack, A and Samani, S and Simpson, C and Wark, D and Nova, F and Boschi, T and Lodovico, FD and Taani, M and Migenda, J and Sedgwick, SM and Zsoldos, S and Yang, JY and Jenkins, SJ and Malek, M and McElwee, JM and Stone, O and Thiesse, MD and Thompson, LF and Okazawa, H and Kim, SB and Yu, I and Nishijima, K and Koshiba, M and Iwamoto, K and Ogawa, N and Yokoyama, M and Martens, K and Vagins, MR and Izumiyama, S and Kuze, M and Tanaka, M and Yoshida, T and Inomoto, M and Ishitsuka, M and Matsumoto, R and Ohta, K and Shinoki, M and Martin, JF and Tanaka, HA and Towstego, T and Hartz, M and Konaka, A and Perio, PD and Prouse, NW and Chen, S and Xu, BD and Richards, B and Jamieson, B and Walker, J and Minamino, A and Pintaudi, G and Sasaki, R and Posiadala-Zezula, M},
Title = {Search for solar electron anti-neutrinos due to spin-flavor
precession in the Sun with Super-Kamiokande-IV},
Year = {2020},
Month = {December},
Abstract = {Due to a very low production rate of electron anti-neutrinos
($\bar{\nu}_e$) via nuclear fusion in the Sun, we expect to
see $\bar{\nu}_e$ from other contribution. An appearance of
$\bar{\nu}_e$ in solar neutrino flux opens a new window for
the new physics beyond the standard model. In particular, a
spin-flavor precession process is expected to convert an
electron neutrino into an electron anti-neutrino
(${\nu_e\to\bar{\nu}_e}$) if neutrino has a finite magnetic
moment. In this work, we have searched for solar
$\bar{\nu}_e$ in the Super-Kamiokande experiment, using
neutron tagging to identify their inverse beta decay
signature. We identified 78 $\bar{\nu}_e$ candidates for
neutrino energies of 9.3 to 17.3 MeV in 2970.1 live days
with a fiducial volume of 22.5 kiloton water (183.0
kton$\cdot$year exposure). The energy spectrum has been
consistent with background predictions and we thus derived a
90\% confidence level upper limit of ${3.6\times10^{-4}}$ on
the $\nu_e\to\bar{\nu}_e$ conversion probability in the Sun.
We used this result to evaluate the sensitivity of future
experiments, notably the Super-Kamiokande Gadolinium (SK-Gd)
upgrade.},
Key = {fds354015}
}
@article{LSSTDarkEnergyScience:2021vfu,
Author = {Collaboration, LSSTDES and Abolfathi, B and Armstrong, R and Awan, H and Babuji, YN and Bauer, FE and Beckett, G and Biswas, R and Bogart, JR and Boutigny, D and Chard, K and Chiang, J and Cohen-Tanugi, J and Connolly,
AJ and Daniel, SF and Digel, SW and Drlica-Wagner, A and Dubois, R and Gawiser, E and Glanzman, T and Habib, S and Hearin, AP and Heitmann, K and Hernandez, F and Hložek, R and Hollowed, J and Jarvis, M and Jha, SW and Kalmbach, JB and Kelly, HM and Kovacs, E and Korytov, D and Krughoff,
KS and Lage, CS and Lanusse, F and Larsen, P and Li, N and Longley, EP and Lupton, RH and Mandelbaum, R and Mao, Y-Y and Marshall, P and Meyers,
JE and Park, JW and Peloton, J and Perrefort, D and Perry, J and Plaszczynski, S and Pope, A and Rykoff, ES and Sánchez, FJ and Schmidt,
SJ and Uram, TD and Villarreal, A and Walter, CW and Wiesner, MP and Wood-Vasey, WM},
Title = {DESC DC2 Data Release Note},
Year = {2021},
Month = {January},
url = {http://arxiv.org/pdf/2101.04855},
Abstract = {In preparation for cosmological analyses of the Vera C.
Rubin Observatory Legacy Survey of Space and Time (LSST),
the LSST Dark Energy Science Collaboration (LSST DESC) has
created a 300 deg$^2$ simulated survey as part of an effort
called Data Challenge 2 (DC2). The DC2 simulated sky survey,
in six optical bands with observations following a reference
LSST observing cadence, was processed with the LSST Science
Pipelines (19.0.0). In this Note, we describe the public
data release of the resulting object catalogs for the
coadded images of five years of simulated observations along
with associated truth catalogs. We include a brief
description of the major features of the available data
sets. To enable convenient access to the data products, we
have developed a web portal connected to Globus data
services. We describe how to access the data and provide
example Jupyter Notebooks in Python to aid first
interactions with the data. We welcome feedback and
questions about the data release via a GitHub
repository.},
Key = {LSSTDarkEnergyScience:2021vfu}
}
@article{fds354016,
Author = {Abe, K and Bronner, C and Hayato, Y and Ikeda, M and Imaizumi, S and Ito,
H and Kameda, J and Kataoka, Y and Miura, M and Moriyama, S and Nagao, Y and Nakahata, M and Nakajima, Y and Nakayama, S and Okada, T and Okamoto, K and Orii, A and Pronost, G and Sekiya, H and Shiozawa, M and Sonoda, Y and Suzuki, Y and Takeda, A and Takemoto, Y and Takenaka, A and Tanaka, H and Yano, T and Akutsu, R and Han, S and Kajita, T and Okumura, K and Tashiro,
T and Wang, R and Xia, J and Bravo-Berguño, D and Labarga, L and Marti, L and Zaldivar, B and Blaszczyk, FDM and Kearns, E and Gustafson, JD and Raaf,
JL and Stone, JL and Wan, L and Wester, T and Bian, J and Griskevich, NJ and Kropp, WR and Locke, S and Mine, S and Smy, MB and Sobel, HW and Takhistov,
V and Weatherly, P and Hill, J and Kim, JY and Lim, IT and Park, RG and Bodur,
B and Scholberg, K and Walter, CW and Coffani, A and Drapier, O and El
Hedri, S and Giampaolo, A and Gonin, M and Mueller, TA and Paganini, P and Quilain, B and Ishizuka, T and Nakamura, T and Jang, JS and Learned, JG and Anthony, LHV and Sztuc, AA and Uchida, Y and Berardi, V and Catanesi,
MG and Radicioni, E and Calabria, NF and Machado, LN and De Rosa and G and Collazuol, G and Iacob, F and Lamoureux, M and Ospina, N and Ludovici,
L and Nishimura, Y and Cao, S and Friend, M and Hasegawa, T and Ishida, T and Kobayashi, T and Matsubara, T and Nakadaira, T and Jakkapu, M and Nakamura, K and Oyama, Y and Sakashita, K and Sekiguchi,
T},
Title = {Neutron-antineutron oscillation search using a 0.37
megaton-years exposure of Super-Kamiokande},
Journal = {Physical Review D},
Volume = {103},
Number = {1},
Year = {2021},
Month = {January},
url = {http://dx.doi.org/10.1103/PhysRevD.103.012008},
Abstract = {As a baryon number violating process with ΔB=2,
neutron-antineutron oscillation (n→n¯) provides a unique
test of baryon number conservation. We have performed a
search for n→n¯ oscillation with bound neutrons in
Super-Kamiokande, with the full dataset from its first four
run periods, representing an exposure of 0.37 Mton-years.
The search used a multivariate analysis trained on simulated
n→n¯ events and atmospheric neutrino backgrounds and
resulted in 11 candidate events with an expected background
of 9.3 events. In the absence of statistically significant
excess, we derived a lower limit on n¯ appearance lifetime
in O16 nuclei of 3.6×1032 years and on the
neutron-antineutron oscillation time of τn→n¯>4.7×108 s
at 90% C.L.},
Doi = {10.1103/PhysRevD.103.012008},
Key = {fds354016}
}
@article{fds360538,
Author = {Abolfathi, B and Alonso, D and Armstrong, R and Aubourg, É and Awan, H and Babuji, YN and Bauer, FE and Bean, R and Beckett, G and Biswas, R and Bogart, JR and Boutigny, D and Chard, K and Chiang, J and Claver, CF and Cohen-Tanugi, J and Combet, C and Connolly, AJ and Daniel, SF and Digel,
SW and Drlica-Wagner, A and Dubois, R and Gangler, E and Gawiser, E and Glanzman, T and Gris, P and Habib, S and Hearin, AP and Heitmann, K and Hernandez, F and Hložek, R and Hollowed, J and Ishak, M and Ivezić,
Ž and Jarvis, M and Jha, SW and Kahn, SM and Kalmbach, JB and Kelly, HM and Kovacs, E and Korytov, D and Krughoff, KS and Lage, CS and Lanusse, F and Larsen, P and Le Guillou and L and Li, N and Longley, EP and Lupton, RH and Mandelbaum, R and Mao, YY and Marshall, P and Meyers, JE and Moniez, M and Morrison, CB and Nomerotski, A and O'Connor, P and Park, HY and Park,
JW and Peloton, J and Perrefort, D and Perry, J and Plaszczynski, S and Pope, A and Rasmussen, A and Reil, K and Roodman, AJ and Rykoff, ES and Sánchez, FJ and Schmidt, SJ and Scolnic, D and Stubbs, CW and Tyson,
JA and Uram, TD and Villarreal, A and Walter, CW and Wiesner, MP and Wood-Vasey, WM and Zuntz, J},
Title = {The LSST DESC DC2 simulated sky survey},
Journal = {Astrophysical Journal, Supplement Series},
Volume = {253},
Number = {1},
Year = {2021},
Month = {March},
url = {http://dx.doi.org/10.3847/1538-4365/abd62c},
Abstract = {We describe the simulated sky survey underlying the second
data challenge (DC2) carried out in preparation for analysis
of the Vera C. Rubin Observatory Legacy Survey of Space and
Time (LSST) by the LSST Dark Energy Science Collaboration
(LSST DESC). Significant connections across multiple science
domains will be a hallmark of LSST; the DC2 program
represents a unique modeling effort that stresses this
interconnectivity in a way that has not been attempted
before. This effort encompasses a full end-to-end approach:
starting from a large N-body simulation, through setting up
LSST-like observations including realistic cadences, through
image simulations, and finally processing with Rubin's LSST
Science Pipelines. This last step ensures that we generate
data products resembling those to be delivered by the Rubin
Observatory as closely as is currently possible. The
simulated DC2 sky survey covers six optical bands in a
wide-fast-deep area of approximately 300 deg2, as well as a
deep drilling field of approximately 1 deg2. We simulate 5
yr of the planned 10 yr survey. The DC2 sky survey has
multiple purposes. First, the LSST DESC working groups can
use the data set to develop a range of DESC analysis
pipelines to prepare for the advent of actual data. Second,
it serves as a realistic test bed for the image processing
software under development for LSST by the Rubin
Observatory. In particular, simulated data provide a
controlled way to investigate certain image-level systematic
effects. Finally, the DC2 sky survey enables the exploration
of new scientific ideas in both static and time domain
cosmology.},
Doi = {10.3847/1538-4365/abd62c},
Key = {fds360538}
}
@article{fds359123,
Author = {Abe, K and Bronner, C and Hayato, Y and Ikeda, M and Imaizumi, S and Kameda, J and Kanemura, Y and Kataoka, Y and Miki, S and Miura, M and Moriyama, S and Nagao, Y and Nakahata, M and Nakayama, S and Okada, T and Okamoto, K and Orii, A and Pronost, G and Sekiya, H and Shiozawa, M and Sonoda, Y and Suzuki, Y and Takeda, A and Takemoto, Y and Takenaka, A and Tanaka, H and Watanabe, S and Yano, T and Han, S and Kajita, T and Okumura,
K and Tashiro, T and Wang, R and Xia, J and Megias, GD and Bravo-Berguño,
D and Labarga, L and Marti, L and Zaldivar, B and Pointon, BW and Blaszczyk, FDM and Kearns, E and Raaf, JL and Stone, JL and Wan, L and Wester, T and Bian, J and Griskevich, NJ and Kropp, WR and Locke, S and Mine, S and Smy, MB and Sobel, HW and Takhistov, V and Weatherly, P and Hill, J and Kim, JY and Lim, IT and Park, RG and Bodur, B and Scholberg, K and Walter, CW and Bernard, L and Coffani, A and Drapier, O and El Hedri and S and Giampaolo, A and Gonin, M and Mueller, TA and Paganini, P and Quilain,
B and Ishizuka, T and Nakamura, T and Jang, JS and Learned, JG and Anthony,
LHV and Martin, DGR and Sztuc, AA and Uchida, Y and Berardi, V and Catanesi, MG and Radicioni, E and Calabria, NF and Machado, LN and de
Rosa, G and Collazuol, G and Iacob, F and Lamoureux, M and Ospina, N and Ludovici, L and Maekawa, Y and Nishimura, Y and Cao, S and Friend, M and Hasegawa, T and Ishida, T and Jakkapu, M and Kobayashi, T and Matsubara,
T and Nakadaira, T},
Title = {Search for neutrinos in coincidence with gravitational wave
events from the LIGO–Virgo O3a observing run with the
Super-Kamiokande detector},
Journal = {Astrophysical Journal},
Volume = {918},
Number = {2},
Pages = {78-78},
Publisher = {American Astronomical Society},
Year = {2021},
Month = {September},
url = {http://dx.doi.org/10.3847/1538-4357/ac0d5a},
Abstract = {The Super-Kamiokande detector can be used to search for
neutrinos in time coincidence with gravitational waves
detected by the LIGO–Virgo Collaboration (LVC). Both
low-energy (7–100 MeV) and high-energy (0.1–105 GeV)
samples were analyzed in order to cover a very wide neutrino
spectrum. Follow-ups of 36 (out of 39) gravitational waves
reported in the GWTC-2 catalog were examined; no significant
excess above the background was observed, with 10 (24)
observed neutrinos compared with 4.8 (25.0) expected events
in the high-energy (low-energy) samples. A statistical
approach was used to compute the significance of potential
coincidences. For each observation, p-values were estimated
using neutrino direction and LVC sky map; the most
significant event (GW190602_175927) is associated with a
post-trial p-value of 7.8% (1.4σ). Additionally, flux
limits were computed independently for each sample and by
combining the samples. The energy emitted as neutrinos by
the identified gravitational wave sources was constrained,
both for given flavors and for all flavors assuming
equipartition between the different flavors, independently
for each trigger and by combining sources of the same
nature.},
Doi = {10.3847/1538-4357/ac0d5a},
Key = {fds359123}
}
@article{fds359890,
Author = {Orii, A and Abe, K and Bronner, C and Hayato, Y and Ikeda, M and Imaizumi,
S and Ito, H and Kameda, J and Kataoka, Y and Kato, Y and Kishimoto, Y and Miura, M and Moriyama, S and Mochizuki, T and Nagao, Y and Nakahata, M and Nakajima, Y and Nakayama, S and Okada, T and Okamoto, K and Pronost, G and Sekiya, H and Shiozawa, M and Sonoda, Y and Suzuki, Y and Takeda, A and Takemoto, Y and Takenaka, A and Tanaka, H and Yano, T and Han, S and Kajita, T and Okumura, K and Tashiro, T and Wang, R and Xia, J and Megias,
GD and Bravo-Berguño, D and Labarga, L and Marti, L and Zaldivar, B and Blaszczyk, FDM and Kearns, E and Raaf, JL and Stone, JL and Wan, L and Wester, T and Pointon, BW and Bian, J and Griskevich, NJ and Kropp, WR and Locke, S and Mine, S and Smy, MB and Sobel, HW and Takhistov, V and Weatherly, P and Ganezer, KS and Hill, J and Kim, JY and Lim, IT and Park,
RG and Bodur, B and Scholberg, K and Walter, CW and Bernard, L and Coffani,
A and Drapier, O and El Hedri and S and Giampaolo, A and Gonin, M and Mueller,
TA and Paganini, P and Quilain, B and Ishizuka, T and Nakamura, T and Jang,
JS and Learned, JG and Matsuno, S and Anthony, LHV and Litchfield, RP and Sztuc, AA and Uchida, Y and Berardi, V and Catanesi, MG and Radicioni,
E and Calabria, NF and Machado, LN and De Rosa and G and Collazuol, G and Iacob, F and Lamoureux, M and Ospina, N and Ludovici, L and Nishimura,
Y and Cao, S and Friend, M and Hasegawa, T and Ishida, T and Kobayashi,
T},
Title = {Search for tens of MeV neutrinos associated with gamma-ray
bursts in Super-Kamiokande},
Journal = {Progress of Theoretical and Experimental
Physics},
Volume = {2021},
Number = {10},
Year = {2021},
Month = {October},
url = {http://dx.doi.org/10.1093/ptep/ptab081},
Abstract = {A search for neutrinos produced in coincidence with
gamma-ray bursts (GRBs) was conducted with the
Super-Kamiokande (SK) detector. Between December 2008 and
March 2017, the Gamma-ray Coordinates Network recorded 2208
GRBs that occurred during normal SK operation. Several time
windows around each GRB were used to search for coincident
neutrino events. No statistically significant signal in
excess of the estimated backgrounds was detected. The νe
fluence in the range from 8 MeV to 100 MeV in positron total
energy for νe+p → e++n was found to be less than 5.07 ×
105 cm-2 per GRB at a 90% confidence level. For all GRBs,
upper bounds were obtained on the fluence as a function of
neutrino energy. Additionally, for GRBs at known distances,
upper limits were set for the neutrino energy emission at
the GRB.},
Doi = {10.1093/ptep/ptab081},
Key = {fds359890}
}
@article{Super-Kamiokande:2021snn,
Author = {Collaboration, S-K and Locke, S and Coffani, A and Abe, K and Bronner,
C and Hayato, Y and Ikeda, M and Imaizumi, S and Ito, H and Kameda, J and Kataoka, Y and Miura, M and Moriyama, S and Nagao, Y and Nakahata, M and Nakajima, Y and Nakayama, S and Okada, T and Okamoto, K and Orii, A and Pronost, G and Sekiya, H and Shiozawa, M and Sonoda, Y and Suzuki, Y and Takeda, A and Takemoto, Y and Takenaka, A and Tanaka, H and Yano, T and Hirade, K and Kanemura, Y and Miki, S and Watabe, S and Han, S and Kajita,
T and Okumura, K and Tashiro, T and Xia, J and Wang, X and Megias, GD and Bravo-Berguño, D and Labarga, L and Marti, L and Zaldivar, B and Pointon, BW and Blaszczyk, FDM and Kearns, E and Raaf, JL and Stone, JL and Wan, L and Wester, T and Bian, J and Griskevich, NJ and Kropp, WR and Mine,
S and Yankelevic, A and Smy, MB and Sobel, HW and Takhistov, V and Hill, J and Kim, JY and Lim, IT and Park, RG and Bodur, B and Scholberg, K and Walter,
CW and Bernard, L and Drapier, O and Hedri, SE and Giampaolo, A and Gonin,
M and Mueller, TA and Paganini, P and Quilain, B and Santos, AD and Ishizuka, T and Nakamura, T and Jang, JS and Learned, JG and Anthony,
LHV and Sztuc, AA and Uchida, Y and Martin, D and Scott, M and Berardi, V and Catanesi, MG and Radicioni, E and Calabria, NF and Machado, LN and Rosa,
GD and Collazuol, G and Iacob, F and Lamoureux, M and Ospina, N and Mattiazzi, M and Ludovici, L and Nishimura, Y and Maewaka, Y and Cao, S and Friend, M and Hasegawa, T and Ishida, T and Kobayashi, T and Jakkapu, M and Matsubara, T and Nakadaira, T and Nakamura, K and Oyama, Y and Sakashita, K and Sekiguchi, T and Tsukamoto, T and Nakano, Y and Shiozawa, T and Suzuki, AT and Takeuchi, Y and Yamamoto, S and Kotsar,
Y and Ozaki, H and Ali, A and Ashida, Y and Feng, J and Hirota, S and Ichikawa, AK and Kikawa, T and Mori, M and Nakaya, T and Wendell, RA and Yasutome, K and Fernandez, P and McCauley, N and Mehta, P and Tsui, KM and Fukuda, Y and Itow, Y and Menjo, H and Niwa, T and Sato, K and Tsukada, M and Mijakowski, P and Lagoda, J and Lakshmi, SM and Zalipska, J and Jung,
CK and Vilela, C and Wilking, MJ and Yanagisawa, C and Jiang, J and Hagiwara, K and Harada, M and Horai, T and Ishino, H and Ito, S and Koshio,
Y and Ma, W and Piplani, N and Sakai, S and Kitagawa, H and Barr, G and Barrow, D and Cook, L and Goldsack, A and Samani, S and Wark, D and Nova,
F and Boschi, T and Lodovico, FD and Taani, M and Zsoldos, S and Gao, J and Migenda, J and Yang, JY and Jenkins, SJ and Malek, M and McElwee, JM and Stone, O and Thiesse, MD and Thompson, LF and Okazawa, H and Kim, SB and Yu, I and Seo, JW and Nishijima, K and Koshiba, M and Iwamoto, K and Ogawa,
N and Yokoyama, M and Martens, K and Vagins, MR and Nakagiri, K and Kuze,
M and Izumiyama, S and Yoshida, T and Inomoto, M and Ishitsuka, M and Matsumoto, R and Ohta, K and Shinoki, M and Suganuma, T and Kinoshita,
T and Martin, JF and Tanaka, HA and Towstego, T and Akutsu, R and Hartz, M and Konaka, A and Perio, PD and Prouse, NW and Chen, S and Xu, BD and Zhang, Y and Posiadala-Zezula, M and Richards, B and Jamieson, B and Walker, J and Minamino, A and Pintaudi, G and Sasaki, R},
Title = {New Methods and Simulations for Cosmogenic Induced
Spallation Removal in Super-Kamiokande-IV},
Year = {2021},
Month = {November},
url = {http://arxiv.org/pdf/2112.00092},
Abstract = {Radioactivity induced by cosmic muon spallation is a
dominant source of backgrounds for $\mathcal{O}(10)~$MeV
neutrino interactions in water Cherenkov detectors. In
particular, it is crucial to reduce backgrounds to measure
the solar neutrino spectrum and find neutrino interactions
from distant supernovae. In this paper we introduce new
techniques to locate muon-induced hadronic showers and
efficiently reject spallation backgrounds. Applying these
techniques to the solar neutrino analysis with an exposure
of $2790\times22.5$~kton.day increases the signal efficiency
by $12.6\%$, approximately corresponding to an additional
year of detector running. Furthermore, we present the first
spallation simulation at SK, where we model hadronic
interactions using FLUKA. The agreement between the isotope
yields and shower pattern in this simulation and in the data
gives confidence in the accuracy of this simulation, and
thus opens the door to use it to optimize muon spallation
removal in new data with gadolinium-enhanced neutron capture
detection.},
Key = {Super-Kamiokande:2021snn}
}
@article{fds360745,
Author = {Sánchez, B and Kessler, R and Scolnic, D and Armstrong, B and Biswas,
R and Bogart, J and Chiang, J and Cohen-Tanugi, J and Fouchez, D and Gris,
P and Heitmann, K and Hložek, R and Jha, S and Kelly, H and Liu, S and Narayan, G and Racine, B and Rykoff, E and Sullivan, M and Walter, C and Wood-Vasey, M and Collaboration, TLSSTDES},
Title = {SNIa-Cosmology Analysis Results from Simulated LSST Images:
from Difference Imaging to Constraints on Dark
Energy},
Year = {2021},
Month = {December},
Abstract = {The Vera Rubin Observatory Legacy Survey of Space and Time
(LSST) is expected to process ${\sim}10^6$ transient
detections per night. For precision measurements of
cosmological parameters and rates, it is critical to
understand the detection efficiency, magnitude limits,
artifact contamination levels, and biases in the selection
and photometry. Here we rigorously test the LSST Difference
Image Analysis (DIA) pipeline using simulated images from
the Rubin Observatory LSST Dark Energy Science Collaboration
(DESC) Data Challenge (DC2) simulation for the
Wide-Fast-Deep (WFD) survey area. DC2 is the first
large-scale (300 deg$^2$) image simulation of a transient
survey that includes realistic cadence, variable observing
conditions, and CCD image artifacts. We analyze ${\sim}$15
deg$^2$ of DC2 over a 5-year time-span in which artificial
point-sources from Type Ia Supernovae (SNIa) light curves
have been overlaid onto the images. We measure the detection
efficiency as a function of Signal-to-Noise Ratio (SNR) and
find a $50\%$ efficiency at $\rm{SNR}=5.8$. The magnitude
limits for each filter are: $u=23.66$, $g=24.69$, $r=24.06$,
$i=23.45$, $z=22.54$, $y=21.62$ $\rm{mag}$. The artifact
contamination is $\sim90\%$ of detections, corresponding to
$\sim1000$ artifacts/deg$^2$ in $g$ band, and falling to 300
per deg$^2$ in $y$ band. The photometry has biases $<1\%$
for magnitudes $19.5 < m <23$. Our DIA performance on
simulated images is similar to that of the Dark Energy
Survey pipeline applied to real images. We also characterize
DC2 image properties to produce catalog-level simulations
needed for distance bias corrections. We find good agreement
between DC2 data and simulations for distributions of SNR,
redshift, and fitted light-curve properties. Applying a
realistic SNIa-cosmology analysis for redshifts $z<1$, we
recover the input cosmology parameters to within statistical
uncertainties.},
Key = {fds360745}
}
@article{Super-Kamiokande:2021jaq,
Author = {Abe, K and Bronner, C and Hayato, Y and Hiraide, K and Ikeda, M and Imaizumi, S and Kameda, J and Kanemura, Y and Kataoka, Y and Miki, S and Miura, M and Moriyama, S and Nagao, Y and Nakahata, M and Nakayama, S and Okada, T and Okamoto, K and Orii, A and Pronost, G and Sekiya, H and Shiozawa, M and Sonoda, Y and Suzuki, Y and Takeda, A and Takemoto, Y and Takenaka, A and Tanaka, H and Watanabe, S and Yano, T and Han, S and Kajita, T and Okumura, K and Tashiro, T and Xia, J and Megias, GD and Bravo-Berguño, D and Labarga, L and Marti, L and Zaldivar, B and Pointon, BW and Blaszczyk, FDM and Kearns, E and Raaf, JL and Stone, JL and Wan, L and Wester, T and Bian, J and Griskevich, NJ and Kropp, WR and Locke, S and Mine, S and Smy, MB and Sobel, HW and Takhistov, V and Hill,
J and Kim, JY and Lim, IT and Park, RG and Bodur, B and Scholberg, K and Walter, CW and Cao, S and Bernard, L and Coffani, A and Drapier, O and El
Hedri, S and Giampaolo, A and Gonin, M and Mueller, TA and Paganini, P and Quilain, B and Ishizuka, T and Nakamura, T and Jang, JS and Learned, JG and Anthony, LHV and Martin, D and Scott, M and Sztuc, AA and Uchida, Y and Berardi, V and Catanesi, MG and Radicioni, E and Calabria, NF and Machado, LN and De Rosa and G and Collazuol, G and Iacob, F and Lamoureux,
M and Mattiazzi, M and Ospina, N and Ludovici, L and Maekawa, Y and Nishimura, Y and Friend, M and Hasegawa, T and Ishida, T and Kobayashi,
T and Jakkapu, M and Matsubara, T},
Title = {Diffuse supernova neutrino background search at
Super-Kamiokande},
Journal = {Physical Review D},
Volume = {104},
Number = {12},
Pages = {122002},
Year = {2021},
Month = {December},
url = {http://dx.doi.org/10.1103/PhysRevD.104.122002},
Abstract = {We have conducted a new search for the diffuse supernova
neutrino background (DSNB) flux at Super-Kamiokande (SK),
with a 22.5×2970-kton·day exposure from its fourth
operational phase IV. With the new analysis we improve on
the existing background reduction techniques and systematic
uncertainties and take advantage of an improved neutron
tagging algorithm to lower the energy threshold compared to
the previous phases of SK. This allows for setting the
world's most stringent upper limit on the extraterrestrial
ν¯e flux, for neutrino energies below 31.3 MeV. The SK-IV
results are combined with the ones from the first three
phases of SK to perform a joint analysis using 22.5×5823
kton·days of data. This analysis has the world's best
sensitivity to the DSNB ν¯e flux, comparable to the
predictions from various models. For neutrino energies
larger than 17.3 MeV, the new combined 90% CL upper limits
on the DSNB ν¯e flux lie around 2.7 cm-2·sec-1, strongly
disfavoring the most optimistic predictions. Finally,
potentialities of the gadolinium phase of SK and the future
Hyper-Kamiokande experiment are discussed.},
Doi = {10.1103/PhysRevD.104.122002},
Key = {Super-Kamiokande:2021jaq}
}
@article{fds367969,
Author = {Stalder, B and Reil, K and Aguilar, C and Araya, C and Borstad, A and Bowdish, B and Cho, M and Cisneros, S and Claver, C and Constanzo, J and Corvetto, G and Dennihy, E and Drass, H and Economou, F and Eisner, A and Fabrega, J and Neto, AF and Fisher-Levine, M and Gonzalez, I and Harris,
R and Hascall, D and Haupt, J and Hoblitt, J and Howard, J and Huffer, M and Jenness, T and Mejias, DJ and Johnson, B and Johnson, T and Krughoff,
KS and Lage, C and Lange, T and Liang, M and Lopez, J and Lopez, M and Lupton,
R and Maulen, G and Menanteau, F and Mills, N and Morris, G and Munoz, F and Neal, H and Neill, D and Newbry, S and Nomerotski, A and Onoprienko, D and Ordenes, I and Orellana, J and Osier, S and Park, HY and Pietrowicz, S and Malagon, AAP and Poczulp, G and Qiu, B and Quint, B and Reinking, H and Reuter, M and Ribeiro, T and Rojas, R and Romero, S and Schindler, R and Schoening, B and Sebag, J and Shugart, A and Silva, C and Sotuela, I and Tache, A and Tapia, D and Thayer, J and Thomas, S and Tighe, R and Tsai,
TW and Turri, M and Tyson, A and Vergara, L and Walter, C and Wiecha, O and Xiong, V},
Title = {Rubin observatory commissioning camera: summit
integration},
Journal = {Proceedings of SPIE - The International Society for Optical
Engineering},
Volume = {12184},
Publisher = {SPIE},
Editor = {Evans, CJ and Bryant, JJ and Motohara, K},
Year = {2022},
Month = {January},
ISBN = {9781510653498},
url = {http://dx.doi.org/10.1117/12.2630184},
Abstract = {The Rubin Observatory Commissioning Camera (ComCam) is a
scaled down (144 Megapixel) version of the 3.2 Gigapixel
LSSTCam which will start the Legacy Survey of Space and Time
(LSST), currently scheduled to start in 2024. The purpose of
the ComCam is to verify the LSSTCam interfaces with the
major subsystems of the observatory as well as evaluate the
overall performance of the system prior to the start of the
commissioning of the LSSTCam hardware on the telescope. With
the delivery of all the telescope components to the summit
site by 2020, the team has already started the high-level
interface verification, exercising the system in a
steady-state model similar to that expected during the
operations phase of the project. Notable activities include
a simulated “slew and expose” sequence that includes
moving the optical components, a settling time to account
for the dynamical environment when on the telescope, and
then taking an actual sequence of images with the ComCam.
Another critical effort is to verify the performance of the
camera refrigeration system, and testing the operational
aspects of running such a system on a moving telescope in
2022. Here we present the status of the interface
verification and the planned sequence of activities
culminating with on-sky performance testing during the
early-commissioning phase.},
Doi = {10.1117/12.2630184},
Key = {fds367969}
}
@article{fds361873,
Author = {Abe, K and Bronner, C and Hayato, Y and Hiraide, K and Ikeda, M and Imaizumi, S and Kameda, J and Kanemura, Y and Kataoka, Y and Miki, S and Miura, M and Moriyama, S and Nagao, Y and Nakahata, M and Nakayama, S and Okada, T and Okamoto, K and Orii, A and Pronost, G and Sekiya, H and Shiozawa, M and Sonoda, Y and Suzuki, Y and Takeda, A and Takemoto, Y and Takenaka, A and Tanaka, H and Watanabe, S and Yano, T and Han, S and Kajita, T and Okumura, K and Tashiro, T and Xia, J and Megias, GD and Bravo-Berguño, D and Labarga, L and Marti, L and Zaldivar, B and Pointon, BW and Blaszczyk, FDM and Kearns, E and Raaf, JL and Stone, JL and Wan, L and Wester, T and Bian, J and Griskevich, NJ and Kropp, WR and Locke, S and Mine, S and Smy, MB and Sobel, HW and Takhistov, V and Hill,
J and Kim, JY and Lim, IT and Park, RG and Bodur, B and Scholberg, K and Walter, CW and Bernard, L and Coffani, A and Drapier, O and Hedri, SE and Giampaolo, A and Gonin, M and Mueller, TA and Paganini, P and Quilain,
B and Ishizuka, T and Nakamura, T and Jang, JS and Learned, JG and Anthony,
LHV and Martin, D and Scott, M and Sztuc, AA and Uchida, Y and Cao, S and Berardi, V and Catanesi, MG and Radicioni, E and Calabria, NF and Machado, LN and De Rosa and G and Collazuol, G and Iacob, F and Lamoureux,
M and Mattiazzi, M and Ospina, N and Ludovici, L and Maekawa, Y and Nishimura, Y and Friend, M and Hasegawa, T and Ishida, T and Kobayashi,
T and Jakkapu, M and Matsubara, T},
Title = {First gadolinium loading to Super-Kamiokande},
Journal = {Nuclear Instruments and Methods in Physics Research, Section
A: Accelerators, Spectrometers, Detectors and Associated
Equipment},
Volume = {1027},
Pages = {166248-166248},
Publisher = {Elsevier BV},
Year = {2022},
Month = {March},
url = {http://dx.doi.org/10.1016/j.nima.2021.166248},
Abstract = {In order to improve Super-Kamiokande's neutron detection
efficiency and to thereby increase its sensitivity to the
diffuse supernova neutrino background flux, 13 tons of
Gd2(SO4)3⋅8H2O (gadolinium sulfate octahydrate) was
dissolved into the detector's otherwise ultrapure water from
July 14 to August 17, 2020, marking the start of the SK-Gd
phase of operations. During the loading, water was
continuously recirculated at a rate of 60 m3/h, extracting
water from the top of the detector and mixing it with
concentrated Gd2(SO4)3⋅8H2O solution to create a 0.02%
solution of the Gd compound before injecting it into the
bottom of the detector. A clear boundary between the
Gd-loaded and pure water was maintained through the loading,
enabling monitoring of the loading itself and the spatial
uniformity of the Gd concentration over the 35 days it took
to reach the top of the detector. During the subsequent
commissioning the recirculation rate was increased to 120
m3/h, resulting in a constant and uniform distribution of Gd
throughout the detector and water transparency equivalent to
that of previous pure-water operation periods. Using an
Am–Be neutron calibration source the mean neutron capture
time was measured to be 115±1 μs, which corresponds to a
Gd concentration of 111±2 ppm, as expected for this level
of Gd loading. This paper describes changes made to the
water circulation system for this detector upgrade, the Gd
loading procedure, detector commissioning, and the first
neutron calibration measurements in SK-Gd.},
Doi = {10.1016/j.nima.2021.166248},
Key = {fds361873}
}
@article{fds368890,
Author = {El Hedri and S and Ashida, Y and Giampaolo, A and Abe, K and Bronner, C and Hayato, Y and Hiraide, K and Ikeda, M and Kameda, J and Kanemura, Y and Kataoka, Y and Miki, S and Miura, M and Moriyama, S and Nagao, Y and Nakahata, M and Nakayama, S and Okamoto, K and Pronost, G and Sekiya, H and Shiozawa, M and Sonoda, Y and Suzuki, Y and Takeda, A and Takemoto, Y and Takenaka, A and Tanaka, H and Watanabe, S and Yano, T and Han, S and Kajita, T and Okumura, K and Tashiro, T and Xia, J and Megias, GD and Labarga, L and Marti, L and Zaldivar, B and Pointon, BW and Kearns, E and Raaf, JL and Wan, L and Wester, T and Bian, J and Griskevich, NJ and Kropp,
WR and Locke, S and Mine, S and Smy, MB and Sobel, HW and Takhistov, V and Hill, J and Kim, JY and Lim, IT and Park, RG and Bodur, B and Scholberg, K and Walter, CW and Bernard, L and Coffani, A and Drapier, O and Gimpaolo, A and Gonin, M and Mueller, TA and Paganini, P and Quilain, B and Ishizuka, T and Nakamura, T and Jang, JS and Learned, JG and Cao, S and Anthony, LHV and Martin, D and Scott, M and Sztuc, AA and Uchida, Y and Berardi, V and Catanesi, MG and Radicioni, E and Calabria, NF and Machado, LN and De
Rosa, G and Collazuol, G and Iacob, F and Lamoureux, M and Mattiazzi, M and Ospina, N and Ludovici, L and Maekawa, Y and Nishimura, Y and Friend, M and Hasegawa, T and Ishida, T and Kobayashi, T and Jakkapu, M and Matsubara,
T and Nakadaira, T and Nakamura, K and Oyama, Y},
Title = {Diffuse Supernova Neutrino Background Search at
Super-Kamiokande},
Journal = {Proceedings of Science},
Volume = {395},
Year = {2022},
Month = {March},
Abstract = {We present the results of a search for the Diffuse Supernova
Neutrino Background (DSNB) at Super-Kamiokande (SK) that
incorporates 22.5 × 2970 kton.days of data from its fourth
data-taking phase. Two analyses, with different energy
regimes covering the 9.3−81.3 MeV antineutrino energy
range, have been developed based on previous SK searches,
with substantially improved background modeling and data
reduction techniques. Moreover, a combined analysis of
nearly 20 years of SK data (1996-2018) has been performed,
with a 90% C.L. sensitivity to the DSNB flux comparable to
various DSNB predictions. No significant evidence for a DSNB
signal has been observed, and both analyses set
world-leading limits on the DSNB flux that can reach about
2.7νe.cm−2.s−1 for a wide range of models.},
Key = {fds368890}
}
@article{fds360747,
Author = {Pronost, G and Abe, K and Bronner, C and Hayato, Y and Hiraide, K and Ikeda, M and Kameda, J and Kanemura, Y and Kataoka, Y and Miki, S and Miura, M and Moriyama, S and Nagao, Y and Nakahata, M and Nakayama, S and Okamoto, K and Sekiya, H and Shiozawa, M and Sonoda, Y and Suzuki, Y and Takeda, A and Takemoto, Y and Takenaka, A and Tanaka, H and Watanabe, S and Yano, T and Han, S and Kajita, T and Okumura, K and Tashiro, T and Xia, J and Megias, GD and Labarga, L and Marti, L and Zaldivar, B and Pointon, BW and Kearns, E and Raaf, JL and Wan, L and Wester, T and Bian, J and Griskevich,
NJ and Kropp, WR and Locke, S and Mine, S and Smy, MB and Sobel, HW and Takhistov, V and Hill, J and Kim, JY and Lim, IT and Park, RG and Bodur, B and Scholberg, K and Walter, CW and Bernard, L and Coffani, A and Drapier,
O and El Hedri and S and Giampaolo, A and Gonin, M and Mueller, TA and Paganini, P and Quilain, B and Ishizuka, T and Nakamura, T and Jang, JS and Learned, JG and Cao, S and Anthony, LHV and Martin, D and Scott, M and Sztuc, AA and Uchida, Y and Berardi, V and Catanesi, MG and Radicioni,
E and Calabria, NF and Machado, LN and De Rosa and G and Collazuol, G and Iacob, F and Lamoureux, M and Mattiazzi, M and Ospina, N and Ludovici,
L and Maekawa, Y and Nishimura, Y and Friend, M and Hasegawa, T and Ishida,
T and Kobayashi, T and Jakkapu, M and Matsubara, T and Nakadaira, T and Nakamura, K and Oyama, Y and Sakashita, K and Sekiguchi,
T},
Title = {Low energy radioactivity BG model in Super-Kamiokande
detector from SK-IV data},
Journal = {Proceedings of Science},
Volume = {395},
Publisher = {Sissa Medialab},
Year = {2022},
Month = {March},
url = {http://dx.doi.org/10.22323/1.395.1046},
Abstract = {The radioactivity background are among the most dangerous
background for low energy neutrino analysis in
Super-Kamiokande (SK), like the solar neutrino analysis.
Among them, the main contribution is coming from 222Rn,
which is spread in the detector’s water due to the water
source and to the photo multiplier (PMT) emanations. Up to
now, its exact distribution in the detector was not known.
Using our knowledge of the radon concentration in the
detector water, and the SK-IV solar data, we developed a
model of the radon distribution in the detector. The
uncertainty on the Rn concentration associated with this
model was estimated to be ∼ 0.1 mBq/m3},
Doi = {10.22323/1.395.1046},
Key = {fds360747}
}
@article{fds360746,
Author = {Giampaolo, A and El Hedri and S and Abe, K and Bronner, C and Hayato, Y and Hiraide, K and Ikeda, M and Kameda, J and Kanemura, Y and Kataoka, Y and Miki, S and Miura, M and Moriyama, S and Nagao, Y and Nakahata, M and Nakayama, S and Okamoto, K and Pronost, G and Sekiya, H and Shiozawa, M and Sonoda, Y and Suzuki, Y and Takeda, A and Takemoto, Y and Takenaka, A and Tanaka, H and Watanabe, S and Yano, T and Han, S and Kajita, T and Okumura,
K and Tashiro, T and Xia, J and Megias, GD and Labarga, L and Marti, L and Zaldivar, B and Pointon, BW and Kearns, E and Raaf, JL and Wan, L and Wester, T and Bian, J and Griskevich, NJ and Kropp, WR and Locke, S and Mine, S and Smy, MB and Sobel, HW and Takhistov, V and Hill, J and Kim, JY and Lim, IT and Park, RG and Bodur, B and Scholberg, K and Walter, CW and Bernard, L and Coffani, A and Drapier, O and Giampolo, A and Gonin, M and Mueller, TA and Paganini, P and Quilain, B and Ishizuka, T and Nakamura,
T and Jang, JS and Learned, JG and Cao, S and Anthony, LHV and Martin, D and Scott, M and Sztuc, AA and Uchida, Y and Berardi, V and Catanesi, MG and Radicioni, E and Calabria, NF and Machado, LN and De Rosa and G and Collazuol, G and Iacob, F and Lamoureux, M and Mattiazzi, M and Ospina,
N and Ludovici, L and Maekawa, Y and Nishimura, Y and Friend, M and Hasegawa, T and Ishida, T and Kobayashi, T and Jakkapu, M and Matsubara,
T and Nakadaira, T and Nakamura, K and Oyama, Y and Sakashita,
K},
Title = {Diffuse Supernova Neutrino Background search at
Super-Kamiokande with neutron tagging},
Journal = {Proceedings of Science},
Volume = {395},
Publisher = {Sissa Medialab},
Year = {2022},
Month = {March},
url = {http://dx.doi.org/10.22323/1.395.1154},
Abstract = {Detecting the Diffuse Supernova Neutrino Background at
Super-Kamiokande requires designing state-of-the-art
background removal technique to reject radioactivity induced
by cosmic muon spallation, and identify atmospheric neutrino
interactions. Identifying the neutron produced by the
interaction of DSNB antineutrinos would allow to remove most
of these backgrounds, but is particularly challenging in
pure water. With the advent of the SK-Gd era, with
Gadolinium being dissolved in the SK water, the efficiency
of the neutron tagging procedure will increase dramatically,
and the SK experiment will make significant gains in its
sensitivity to the DSNB. I will present the role of neutron
tagging and the challenges it provides, as well as discuss
the impact of the SK-Gd project.},
Doi = {10.22323/1.395.1154},
Key = {fds360746}
}
@article{fds360748,
Author = {Abe, K and Bronner, C and Hayato, Y and Hiraide, K and Ikeda, M and Kameda,
J and Kanemura, Y and Kataoka, Y and Miki, S and Miura, M and Moriyama, S and Nagao, Y and Nakahata, M and Nakayama, S and Okamoto, K and Pronost, G and Sekiya, H and Shiozawa, M and Sonoda, Y and Suzuki, Y and Takeda, A and Takemoto, Y and Takenaka, A and Tanaka, H and Watanabe, S and Yano, T and Han, S and Kajita, T and Okumura, K and Tashiro, T and Xia, J and Megias,
GD and Labarga, L and Marti, L and Zaldivar, B and Pointon, BW and Kearns,
E and Raaf, JL and Wan, L and Wester, T and Bian, J and Griskevich, NJ and Kropp, WR and Locke, S and Mine, S and Smy, MB and Sobel, HW and Takhistov,
V and Hill, J and Kim, JY and Lim, IT and Park, RG and Bodur, B and Scholberg,
K and Walter, CW and Bernard, L and Coffani, A and Drapier, O and El Hedri,
S and Giampaolo, A and Gonin, M and Mueller, TA and Paganini, P and Quilain, B and Ishizuka, T and Nakamura, T and Jang, JS and Learned, JG and Cao, S and Anthony, LHV and Martin, D and Scott, M and Sztuc, AA and Uchida, Y and Berardi, V and Catanesi, MG and Radicioni, E and Calabria,
NF and Machado, LN and De Rosa and G and Collazuol, G and Iacob, F and Lamoureux, M and Mattiazzi, M and Ospina, N and Ludovici, L and Maekawa,
Y and Nishimura, Y and Friend, M and Hasegawa, T and Ishida, T and Kobayashi, T and Jakkapu, M and Matsubara, T and Nakadaira, T and Nakamura, K and Oyama, Y and Sakashita, K and Sekiguchi, T and Tsukamoto, T},
Title = {Follow-up of GWTC-2 gravitational wave events with neutrinos
from the Super-Kamiokande detector},
Journal = {Proceedings of Science},
Volume = {395},
Publisher = {Sissa Medialab},
Year = {2022},
Month = {March},
url = {http://dx.doi.org/10.22323/1.395.0947},
Abstract = {Super-Kamiokande (SK) is a 50-kt water Cherenkov detector,
instrumented with ∼ 13k photo-multipliers and running
since 1996. It is sensitive to neutrinos with energies
ranging from 4.5 MeV to several TeV. A new framework has
been developed for the follow-up of gravitational wave (GW)
alerts issued by the LIGO-Virgo collaboration (LVC).
Neutrinos are searched for, using a 1000-second time window
centered on the alert time and in both SK low-energy and
high-energy samples. Such observation can then be used to
constrain the neutrino emission from the GW source. The
significance of potential signals has been obtained by
comparing neutrino direction with the localization of the
GW. The computation of limits on incoming neutrino flux and
on the total energy emitted in neutrinos by the source has
been performed for the different neutrino flavors. The
results using the LVC GWTC-2 catalog (covering O3a period)
are presented, as well as the outlooks for the future
real-time public release of follow-ups for the O4 period (in
2022) and beyond.},
Doi = {10.22323/1.395.0947},
Key = {fds360748}
}
@article{fds368891,
Author = {Kitagawa, H and Nakano, Y and Koshio, Y and Abe, K and Bronner, C and Hayato, Y and Hiraide, K and Ikeda, M and Kameda, J and Kanemura, Y and Kataoka, Y and Miki, S and Miura, M and Moriyama, S and Nagao, Y and Nakahata, M and Nakayama, S and Okamoto, K and Pronost, G and Sekiya, H and Shiozawa, M and Sonoda, Y and Suzuki, Y and Takeda, A and Takemoto, Y and Takenaka, A and Tanaka, H and Watanabe, S and Yano, T and Han, S and Kajita, T and Okumura, K and Tashiro, T and Xia, J and Megias, GD and Labarga, L and Marti, L and Zaldivar, B and Pointon, BW and Kearns, E and Raaf, JL and Wan, L and Wester, T and Bian, J and Griskevich, NJ and Kropp,
WR and Locke, S and Mine, S and Smy, MB and Sobel, HW and Takhistov, V and Hill, J and Kim, JY and Lim, IT and Park, RG and Bodur, B and Scholberg, K and Walter, CW and Bernard, L and Coffani, A and Drapier, O and El Hedri and S and Giampaolo, A and Gonin, M and Mueller, TA and Paganini, P and Quilain,
B and Ishizuka, T and Nakamura, T and Jang, JS and Learned, JG and Cao, S and Anthony, LHV and Martin, D and Scott, M and Sztuc, AA and Uchida, Y and Berardi, V and Catanesi, MG and Radicioni, E and Calabria, NF and Machado, LN and De Rosa and G and Collazuol, G and Iacob, F and Lamoureux,
M and Mattiazzi, M and Ospina, N and Ludovici, L and Maekawa, Y and Nishimura, Y and Friend, M and Hasegawa, T and Ishida, T and Kobayashi,
T and Jakkapu, M and Matsubara, T and Nakadaira, T and Nakamura, K and Oyama, Y},
Title = {Measurements of the charge ratio and polarization of
cosmic-ray muons with the Super-Kamiokande
detector},
Journal = {Proceedings of Science},
Volume = {395},
Year = {2022},
Month = {March},
Abstract = {Cosmic-ray muons arise from the showers of secondary
particles produced via the interactions of primary cosmic
particles with air nuclei at the top of the atmosphere. The
interaction products, pions and kaons composing showers
mostly decay to muons reflect the details of the hadronic
interactions depending on their energy. Measurements of the
charge ratio and polarization of cosmic-ray muons can be
used to constrain high energy hadronic interaction models in
the atmosphere. In this presentation, we will report the
current status of the measurement of the charge ratio using
data collected by the Super-Kamiokande (SK) detector located
at a depth of 2700 m of water equivalent. Using the data
taken in the fourth phase of SK (SK-IV), the charge ratio is
measured to be 1.42 ± 0.02 (statistical uncertainty only),
at the energy of 1.3 TeV. This result for the charge ratio
is in good agreement with those previously obtained by deep
underground experiments.},
Key = {fds368891}
}
@article{fds362444,
Author = {Abe, K and Bronner, C and Hayato, Y and Ikeda, M and Imaizumi, S and Ito,
H and Kameda, J and Kataoka, Y and Miura, M and Moriyama, S and Nagao, Y and Nakahata, M and Nakajima, Y and Nakayama, S and Okada, T and Okamoto, K and Orii, A and Pronost, G and Sekiya, H and Shiozawa, M and Sonoda, Y and Suzuki, Y and Takeda, A and Takemoto, Y and Takenaka, A and Tanaka, H and Yano, T and Akutsu, R and Han, S and Kajita, T and Okumura, K and Tashiro,
T and Wang, R and Xia, J and Bravo-Berguño, D and Labarga, L and Marti, L and Zaldivar, B and Blaszczyk, FDM and Kearns, E and Raaf, JL and Stone, JL and Wan, L and Wester, T and Pointon, BW and Bian, J and Griskevich, NJ and Kropp, WR and Locke, S and Mine, S and Smy, MB and Sobel, HW and Takhistov,
V and Weatherly, P and Hill, J and Kim, JY and Lim, IT and Park, RG and Bodur,
B and Scholberg, K and Walter, CW and Bernard, L and Coffani, A and Drapier, O and Hedri, SE and Giampaolo, A and Gonin, M and Mueller, TA and Paganini, P and Quilain, B and Ishizuka, T and Nakamura, T and Jang, JS and Learned, JG and Anthony, LHV and Sztuc, AA and Uchida, Y and Berardi, V and Catanesi, MG and Radicioni, E and Calabria, NF and Machado, LN and De
Rosa, G and Collazuol, G and Iacob, F and Lamoureux, M and Ospina, N and Ludovici, L and Nishimura, Y and Cao, S and Friend, M and Hasegawa, T and Ishida, T and Jakkapu, M and Kobayashi, T and Matsubara, T and Nakadaira, T and Nakamura, K and Oyama, Y and Sakashita,
K},
Title = {Search for solar electron anti-neutrinos due to spin-flavor
precession in the Sun with Super-Kamiokande-IV},
Journal = {Astroparticle Physics},
Volume = {139},
Pages = {102702-102702},
Publisher = {Elsevier BV},
Year = {2022},
Month = {June},
url = {http://dx.doi.org/10.1016/j.astropartphys.2022.102702},
Abstract = {Due to a very low production rate of electron anti-neutrinos
(ν̄e) via nuclear fusion in the Sun, a flux of solar ν̄e
is unexpected. An appearance of ν̄e in solar neutrino flux
opens a new window for the new physics beyond the standard
model. In particular, a spin-flavor precession process is
expected to convert an electron neutrino into an electron
anti-neutrino (νe→ν̄e) when neutrino has a finite
magnetic moment. In this work, we have searched for solar
ν̄e in the Super-Kamiokande experiment, using neutron
tagging to identify their inverse beta decay signature. We
identified 78 ν̄e candidates for neutrino energies of 9.3
to 17.3 MeV in 2970.1 live days with a fiducial volume of
22.5 kiloton water (183.0 kton⋅year exposure). The energy
spectrum has been consistent with background predictions and
we thus derived a 90% confidence level upper limit of
4.7×10−4 on the νe→ν̄e conversion probability in the
Sun. We used this result to evaluate the sensitivity of
future experiments, notably the Super-Kamiokande Gadolinium
(SK-Gd) upgrade.},
Doi = {10.1016/j.astropartphys.2022.102702},
Key = {fds362444}
}
@article{fds365182,
Author = {Sánchez, BO and Kessler, R and Scolnic, D and Armstrong, R and Biswas,
R and Bogart, J and Chiang, J and Cohen-Tanugi, J and Fouchez, D and Gris,
P and Heitmann, K and Hložek, R and Jha, S and Kelly, H and Liu, S and Narayan, G and Racine, B and Rykoff, E and Sullivan, M and Walter, CW and Wood-Vasey, WM},
Title = {SNIa Cosmology Analysis Results from Simulated LSST Images:
From Difference Imaging to Constraints on Dark
Energy},
Journal = {Astrophysical Journal},
Volume = {934},
Number = {2},
Year = {2022},
Month = {August},
url = {http://dx.doi.org/10.3847/1538-4357/ac7a37},
Abstract = {The Vera Rubin Observatory Legacy Survey of Space and Time
(LSST) is expected to process ∼106 transient detections
per night. For precision measurements of cosmological
parameters and rates, it is critical to understand the
detection efficiency, magnitude limits, artifact
contamination levels, and biases in the selection and
photometry. Here we rigorously test the LSST Difference
Image Analysis (DIA) pipeline using simulated images from
the Rubin Observatory LSST Dark Energy Science Collaboration
Data Challenge (DC2) simulation for the Wide-Fast-Deep
survey area. DC2 is the first large-scale (300 deg2) image
simulation of a transient survey that includes realistic
cadence, variable observing conditions, and CCD image
artifacts. We analyze ∼15 deg2 of DC2 over a 5 yr time
span in which artificial point sources from Type Ia
supernova (SNIa) light curves have been overlaid onto the
images. The magnitude limits per filter are u = 23.66 mag, g
= 24.69 mag, r = 24.06 mag, i = 23.45 mag, z = 22.54 mag,
and y = 21.62 mag. The artifact contamination levels are
∼90% of all detections, corresponding to ∼1000 artifacts
deg-2 in g band, and falling to 300 deg-2 in y band. The
photometry has biases <1% for magnitudes 19.5 < m < 23. Our
DIA performance on simulated images is similar to that of
the Dark Energy Survey difference-imaging pipeline on real
images. We also characterize DC2 image properties to produce
catalog-level simulations needed for distance bias
corrections. We find good agreement between DC2 data and
simulations for distributions of signal-to-noise ratio,
redshift, and fitted light-curve properties. Applying a
realistic SNIa cosmology analysis for redshifts z < 1, we
recover the input cosmology parameters to within statistical
uncertainties.},
Doi = {10.3847/1538-4357/ac7a37},
Key = {fds365182}
}
@article{fds365627,
Author = {Machado, LN and Abe, K and Hayato, Y and Hiraide, K and Ieki, K and Ikeda,
M and Kameda, J and Kanemura, Y and Kaneshima, R and Kashiwagi, Y and Kataoka, Y and Miki, S and Mine, S and Miura, M and Moriyama, S and Nakano,
Y and Nakahata, M and Nakayama, S and Noguchi, Y and Okamoto, K and Sato,
K and Sekiya, H and Shiba, H and Shimizu, K and Shiozawa, M and Sonoda, Y and Suzuki, Y and Takeda, A and Takemoto, Y and Takenaka, A and Tanaka, H and Watanabe, S and Yano, T and De Perio and P and Martens, K and Vagins, MR and Bian, J and Griskevich, NJ and Kropp, WR and Locke, S and Smy, MB and Sobel, HW and Takhistov, V and Yankelevich, A and Han, S and Kajita, T and Okumura, K and Tashiro, T and Tomiya, T and Wang, X and Xia, J and Yoshida,
S and Megias, GD and Fernandez, P and Labarga, L and Ospina, N and Zaldivar, B and Pointon, BW and Akutsu, R and Gousy-Leblanc, V and Hartz, M and Konaka, A and Prouse, NW and Kearns, E and Raaf, JL and Wan,
L and Wester, T and Hill, J and Kim, JY and Lim, IT and Park, RG and Bodur, B and Scholberg, K and Walter, CW and Bernard, L and Coffani, A and Drapier,
O and El Hedri and S and Giampaolo, A and Mueller, TA and Santos, AD and Paganini, P and Quilain, B and Ishizuka, T and Nakamura, T and Jang, JS and Learned, JG and Cao, S and Choi, K and Anthony, LHV and Martin, D and Scott, M and Sztuc, AA and Uchida, Y and Berardi, V and Catanesi, MG and Radicioni, E and Calabria, NF and De Rosa and G and Collazuol,
G},
Title = {Pre-supernova Alert System for Super-Kamiokande},
Journal = {Astrophysical Journal},
Volume = {935},
Number = {1},
Pages = {40-40},
Publisher = {American Astronomical Society},
Year = {2022},
Month = {August},
url = {http://dx.doi.org/10.3847/1538-4357/ac7f9c},
Abstract = {In 2020, the Super-Kamiokande (SK) experiment moved to a new
stage (SK-Gd) in which gadolinium (Gd) sulfate octahydrate
was added to the water in the detector, enhancing the
efficiency to detect thermal neutrons and consequently
improving the sensitivity to low energy electron
anti-neutrinos from inverse beta decay (IBD) interactions.
SK-Gd has the potential to provide early alerts of incipient
core-collapse supernovae through detection of electron
anti-neutrinos from thermal and nuclear processes
responsible for the cooling of massive stars before the
gravitational collapse of their cores. These pre-supernova
neutrinos emitted during the silicon burning phase can
exceed the energy threshold for IBD reactions. We present
the sensitivity of SK-Gd to pre-supernova stars and the
techniques used for the development of a pre-supernova alarm
based on the detection of these neutrinos in SK, as well as
prospects for future SK-Gd phases with higher concentrations
of Gd. For the current SK-Gd phase, high-confidence alerts
for Betelgeuse could be issued up to 9 hr in advance of the
core collapse itself.},
Doi = {10.3847/1538-4357/ac7f9c},
Key = {fds365627}
}
@article{fds366923,
Author = {Workman, RL and Burkert, VD and Crede, V and Klempt, E and Thoma, U and Tiator, L and Agashe, K and Aielli, G and Allanach, BC and Amsler, C and Antonelli, M and Aschenauer, EC and Asner, DM and Baer, H and Banerjee,
SW and Barnett, RM and Baudis, L and Bauer, CW and Beatty, JJ and Belousov,
VI and Beringer, J and Bettini, A and Biebel, O and Black, KM and Blucher,
E and Bonventre, R and Bryzgalov, VV and Buchmuller, O and Bychkov, MA and Cahn, RN and Carena, M and Ceccucci, A and Cerri, A and Chivukula, RS and Cowan, G and Cranmer, K and Cremonesi, O and D'Ambrosio, G and Damour,
T and De Florian and D and De Gouvêa and A and DeGrand, T and De Jong and P and Demers, S and Dobrescu, BA and D'Onofrio, M and Doser, M and Dreiner,
HK and Eerola, P and Egede, U and Eidelman, S and El-Khadra, AX and Ellis,
J and Eno, SC and Erler, J and Ezhela, VV and Fetscher, W and Fields, BD and Freitas, A and Gallagher, H and Gershtein, Y and Gherghetta, T and Gonzalez-Garcia, MC and Goodman, M and Grab, C and Gritsan, AV and Grojean, C and Groom, DE and Grünewald, M and Gurtu, A and Gutsche, T and Haber, HE and Hamel, M and Hanhart, C and Hashimoto, S and Hayato, Y and Hebecker, A and Heinemeyer, S and Hernández-Rey, JJ and Hikasa, K and Hisano, J and Höcker, A and Holder, J and Hsu, L and Huston, J and Hyodo,
T and Ianni, A and Kado, M and Karliner, M and Katz, UF and Kenzie, M and Khoze, VA and Klein, SR and Krauss, F and Kreps, M and Križan, P and Krusche, B and Kwon, Y and Lahav, O and Laiho, J},
Title = {Review of Particle Physics},
Journal = {Progress of Theoretical and Experimental
Physics},
Volume = {2022},
Number = {8},
Publisher = {Oxford University Press (OUP)},
Year = {2022},
Month = {August},
url = {http://dx.doi.org/10.1093/ptep/ptac097},
Abstract = {The Review summarizes much of particle physics and
cosmology. Using data from previous editions, plus 2,143 new
measurements from 709 papers, we list, evaluate, and average
measured properties of gauge bosons and the recently
discovered Higgs boson, leptons, quarks, mesons, and
baryons. We summarize searches for hypothetical particles
such as supersymmetric particles, heavy bosons, axions, dark
photons, etc. Particle properties and search limits are
listed in Summary Tables. We give numerous tables, figures,
formulae, and reviews of topics such as Higgs Boson Physics,
Supersymmetry, Grand Unified Theories, Neutrino Mixing, Dark
Energy, Dark Matter, Cosmology, Particle Detectors,
Colliders, Probability and Statistics. Among the 120 reviews
are many that are new or heavily revised, including a new
review on Machine Learning, and one on Spectroscopy of Light
Meson Resonances. The Review is divided into two volumes.
Volume 1 includes the Summary Tables and 97 review articles.
Volume 2 consists of the Particle Listings and contains also
23 reviews that address specific aspects of the data
presented in the Listings. The complete Review (both
volumes) is published online on the website of the Particle
Data Group (pdg.lbl.gov) and in a journal. Volume 1 is
available in print as the PDG Book. A Particle Physics
Booklet with the Summary Tables and essential tables,
figures, and equations from selected review articles is
available in print, as a web version optimized for use on
phones, and as an Android app.},
Doi = {10.1093/ptep/ptac097},
Key = {fds366923}
}
@article{fds367497,
Author = {Mori, M and Abe, K and Hayato, Y and Hiraide, K and Ieki, K and Ikeda, M and Imaizumi, S and Kameda, J and Kanemura, Y and Kaneshima, R and Kashiwagi, Y and Kataoka, Y and Miki, S and Mine, S and Miura, M and Moriyama, S and Nagao, Y and Nakahata, M and Nakano, Y and Nakayama, S and Noguchi, Y and Okada, T and Okamoto, K and Orii, A and Sato, K and Sekiya,
H and Shiba, H and Shimizu, K and Shiozawa, M and Sonoda, Y and Suzuki, Y and Takeda, A and Takemoto, Y and Takenaka, A and Tanaka, H and Tomiya, T and Watanabe, S and Yano, T and Yoshida, S and Han, S and Kajita, T and Okumura, K and Tashiro, T and Wang, X and Xia, J and Megias, GD and Bravo-Berguño, D and Fernandez, P and Labarga, L and Ospina, N and Zaldivar, B and Zsoldos, S and Pointon, BW and Blaszczyk, FDM and Kearns, E and Raaf, JL and Stone, JL and Wan, L and Wester, T and Bian, J and Griskevich, NJ and Kropp, WR and Locke, S and Smy, MB and Sobel, HW and Takhistov, V and Yankelevich, A and Hill, J and Kim, JY and Lim, IT and Park, RG and Bodur, B and Scholberg, K and Walter, CW and Bernard, L and Coffani, A and Drapier, O and El Hedri and S and Giampaolo, A and Mueller,
TA and Paganini, P and Quilain, B and Santos, AD and Ishizuka, T and Nakamura, T and Jang, JS and Learned, JG and Anthony, LHV and Martin, D and Scott, M and Sztuc, AA and Uchida, Y and Berardi, V and Catanesi, MG and Radicioni, E and Calabria, NF and Machado, LN and De Rosa and G and Collazuol, G and Iacob, F},
Title = {Searching for Supernova Bursts in Super-Kamiokande
IV},
Journal = {Astrophysical Journal},
Volume = {938},
Number = {1},
Pages = {35-35},
Publisher = {American Astronomical Society},
Year = {2022},
Month = {October},
url = {http://dx.doi.org/10.3847/1538-4357/ac8f41},
Abstract = {Super-Kamiokande has been searching for neutrino bursts
characteristic of core-collapse supernovae continuously, in
real time, since the start of operations in 1996. The
present work focuses on detecting more distant supernovae
whose event rate may be too small to trigger in real time,
but may be identified using an offline approach. The
analysis of data collected from 2008 to 2018 found no
evidence of distant supernovae bursts. This establishes an
upper limit of 0.29 yr-1 on the rate of core-collapse
supernovae out to 100 kpc at 90% C.L. For supernovae that
fail to explode and collapse directly to black holes the
limit reaches to 300 kpc.},
Doi = {10.3847/1538-4357/ac8f41},
Key = {fds367497}
}
@article{fds367763,
Author = {Abe, K and Haga, Y and Hayato, Y and Hiraide, K and Ieki, K and Ikeda, M and Imaizumi, S and Iyogi, K and Kameda, J and Kanemura, Y and Kataoka, Y and Kato, Y and Kishimoto, Y and Miki, S and Mine, S and Miura, M and Mochizuki, T and Moriyama, S and Nagao, Y and Nakahata, M and Nakajima,
T and Nakano, Y and Nakayama, S and Okada, T and Okamoto, K and Orii, A and Sato, K and Sekiya, H and Shiozawa, M and Sonoda, Y and Suzuki, Y and Takeda, A and Takemoto, Y and Takenaka, A and Tanaka, H and Tasaka, S and Tomura, T and Ueno, K and Watanabe, S and Yano, T and Yokozawa, T and Han,
S and Irvine, T and Kajita, T and Kametani, I and Kaneyuki, K and Lee, KP and McLachlan, T and Okumura, K and Richard, E and Tashiro, T and Wang, R and Xia, J and Megias, GD and Bravo-Berguño, D and Labarga, L and Zaldivar,
B and Goldhaber, M and Blaszczyk, FDM and Gustafson, J and Kachulis, C and Kearns, E and Raaf, JL and Stone, JL and Sulak, LR and Sussman, S and Wan,
L and Wester, T and Pointon, BW and Bian, J and Carminati, G and Elnimr, M and Griskevich, NJ and Kropp, WR and Locke, S and Renshaw, A and Smy, MB and Sobel, HW and Takhistov, V and Weatherly, P and Ganezer, KS and Hartfiel, BL and Hill, J and Keig, WE and Hong, N and Kim, JY and Lim, IT and Park, RG and Akiri, T and Bodur, B and Himmel, A and Li, Z and O'Sullivan,
E and Scholberg, K and Walter, CW and Wongjirad, T and Bernard, L and Coffani, A and Drapier, O and El Hedri and S},
Title = {Neutron tagging following atmospheric neutrino events in a
water Cherenkov detector},
Journal = {Journal of Instrumentation},
Volume = {17},
Number = {10},
Year = {2022},
Month = {October},
url = {http://dx.doi.org/10.1088/1748-0221/17/10/P10029},
Abstract = {We present the development of neutron-tagging techniques in
Super-Kamiokande IV using a neural network analysis. The
detection efficiency of neutron capture on hydrogen is
estimated to be 26%, with a mis-tag rate of 0.016 per
neutrino event. The uncertainty of the tagging efficiency is
estimated to be 9.0%. Measurement of the tagging efficiency
with data from an Americium-Beryllium calibration agrees
with this value within 10%. The tagging procedure was
performed on 3,244.4 days of SK-IV atmospheric neutrino
data, identifying 18,091 neutrons in 26,473 neutrino events.
The fitted neutron capture lifetime was measured as 218±9
μs.},
Doi = {10.1088/1748-0221/17/10/P10029},
Key = {fds367763}
}
@article{fds367873,
Author = {Matsumoto, R and Abe, K and Hayato, Y and Hiraide, K and Ieki, K and Ikeda,
M and Kameda, J and Kanemura, Y and Kaneshima, R and Kashiwagi, Y and Kataoka, Y and Miki, S and Mine, S and Miura, M and Moriyama, S and Nakano,
Y and Nakahata, M and Nakayama, S and Noguchi, Y and Okamoto, K and Sato,
K and Sekiya, H and Shiba, H and Shimizu, K and Shiozawa, M and Sonoda, Y and Suzuki, Y and Takeda, A and Takemoto, Y and Takenaka, A and Tanaka, H and Watanabe, S and Yano, T and Han, S and Kajita, T and Okumura, K and Tashiro, T and Tomiya, T and Wang, X and Xia, J and Yoshida, S and Megias,
GD and Fernandez, P and Labarga, L and Ospina, N and Zaldivar, B and Pointon, BW and Kearns, E and Raaf, JL and Wan, L and Wester, T and Bian,
J and Griskevich, NJ and Kropp, WR and Locke, S and Smy, MB and Sobel, HW and Takhistov, V and Yankelevich, A and Hill, J and Kim, JY and Lim, IT and Park, RG and Bodur, B and Scholberg, K and Walter, CW and Bernard, L and Coffani, A and Drapier, O and El Hedri and S and Giampaolo, A and Mueller,
TA and Santos, AD and Paganini, P and Quilain, B and Ishizuka, T and Nakamura, T and Jang, JS and Learned, JG and Choi, K and Cao, S and Anthony, LHV and Martin, D and Scott, M and Sztuc, AA and Uchida, Y and Berardi, V and Catanesi, MG and Radicioni, E and Calabria, NF and Machado, LN and De Rosa and G and Collazuol, G and Iacob, F and Lamoureux,
M and Mattiazzi, M and Ludovici, L and Gonin, M and Pronost, G and Fujisawa, C},
Title = {Search for proton decay via p →μ+K0 in 0.37 megaton-years
exposure of Super-Kamiokande},
Journal = {Physical Review D},
Volume = {106},
Number = {7},
Year = {2022},
Month = {October},
url = {http://dx.doi.org/10.1103/PhysRevD.106.072003},
Abstract = {We searched for proton decay via p→μ+K0 in 0.37
Mton·years of data collected between 1996 and 2018 from the
Super-Kamiokande water Cherenkov experiment. The selection
criteria were defined separately for KS0 and KL0 channels.
No significant event excess has been observed. As a result
of this analysis, which extends the previous search by an
additional 0.2 Mton·years of exposure and uses an improved
event reconstruction, we set a lower limit of 3.6×1033
years on the proton lifetime.},
Doi = {10.1103/PhysRevD.106.072003},
Key = {fds367873}
}
@article{fds369064,
Author = {Abe, K and Hayato, Y and Hiraide, K and Ieki, K and Ikeda, M and Kameda, J and Kanemura, Y and Kaneshima, R and Kashiwagi, Y and Kataoka, Y and Miki,
S and Mine, S and Miura, M and Moriyama, S and Nakano, Y and Nakahata, M and Nakayama, S and Noguchi, Y and Okamoto, K and Sato, K and Sekiya, H and Shiba, H and Shimizu, K and Shiozawa, M and Sonoda, Y and Suzuki, Y and Takeda, A and Takemoto, Y and Takenaka, A and Tanaka, H and Watanabe, S and Yano, T and Han, S and Kajita, T and Okumura, K and Tashiro, T and Tomiya,
T and Wang, X and Xia, J and Yoshida, S and Megias, GD and Fernandez, P and Labarga, L and Ospina, N and Zaldivar, B and Pointon, BW and Kearns, E and Raaf, JL and Wan, L and Wester, T and Bian, J and Griskevich, NJ and Kropp,
WR and Locke, S and Smy, MB and Sobel, HW and Takhistov, V and Yankelevich,
A and Hill, J and Park, RG and Bodur, B and Scholberg, K and Walter, CW and Bernard, L and Coffani, A and Drapier, O and El Hedri and S and Giampaolo,
A and Mueller, TA and Santos, AD and Paganini, P and Quilain, B and Ishizuka, T and Nakamura, T and Jang, JS and Learned, JG and Choi, K and Cao, S and Anthony, LHV and Martin, D and Scott, M and Sztuc, AA and Uchida, Y and Berardi, V and Catanesi, MG and Radicioni, E and Calabria,
NF and Machado, LN and De Rosa and G and Collazuol, G and Iacob, F and Lamoureux, M and Mattiazzi, M and Ludovici, L and Gonin, M and Pronost,
G and Fujisawa, C and Maekawa, Y and Nishimura, Y and Friend, M and Hasegawa, T and Ishida, T and Kobayashi, T and Jakkapu, M and Matsubara,
T and Nakadaira, T and Nakamura, K and Oyama, Y and Sakashita, K and Sekiguchi, T and Tsukamoto, T and Boschi, T and Di Lodovico and F and Gao,
J and Goldsack, A and Katori, T and Migenda, J and Taani, M and Zsoldos, S and Kotsar, Y and Ozaki, H and Suzuki, AT and Takeuchi, Y and Bronner, C and Feng, J and Kikawa, T and Mori, M and Nakaya, T and Wendell, RA and Yasutome, K and Jenkins, SJ and McCauley, N and Mehta, P and Tsui, KM and Fukuda, Y and Itow, Y and Menjo, H and Ninomiya, K and Lagoda, J and Lakshmi, SM and Mandal, M and Mijakowski, P and Prabhu, YS and Zalipska,
J and Jia, M and Jiang, J and Jung, CK and Wilking, MJ and Yanagisawa, C and Harada, M and Ishino, H and Ito, S and Kitagawa, H and Koshio, Y and Nakanishi, F and Sakai, S and Barr, G and Barrow, D and Cook, L and Samani,
S and Wark, D and Nova, F and Yang, JY and Malek, M and McElwee, JM and Stone,
O and Thiesse, MD and Thompson, LF and Okazawa, H and Kim, SB and Seo, JW and Yu, I and Ichikawa, AK and Nakamura, KD and Tairafune, S and Nishijima,
K and Iwamoto, K and Nakagiri, K and Nakajima, Y and Taniuchi, N and Yokoyama, M and Martens, K and de Perio, P and Vagins, MR and Kuze, M and Izumiyama, S and Inomoto, M and Ishitsuka, M and Ito, H and Kinoshita,
T and Matsumoto, R and Ommura, Y and Shigeta, N and Shinoki, M and Suganuma, T and Yamauchi, K and Martin, JF and Tanaka, HA and Towstego,
T and Akutsu, R and Gousy-Leblanc, V and Hartz, M and Konaka, A and Prouse,
NW and Chen, S and Xu, BD and Zhang, B and Posiadala-Zezula, M and Hadley,
D and Nicholson, M and O'Flaherty, M and Richards, B and Ali, A and Jamieson, B and Marti, L and Minamino, A and Pintaudi, G and Sano, S and Suzuki, S and Wada, K and Super-Kamiokande Collaboration},
Title = {Search for Cosmic-Ray Boosted Sub-GeV Dark Matter Using
Recoil Protons at Super-Kamiokande.},
Journal = {Physical review letters},
Volume = {130},
Number = {3},
Pages = {031802},
Publisher = {American Physical Society (APS)},
Year = {2023},
Month = {January},
url = {http://dx.doi.org/10.1103/physrevlett.130.031802},
Abstract = {We report a search for cosmic-ray boosted dark matter with
protons using the 0.37 megaton×years data collected at
Super-Kamiokande experiment during the 1996-2018 period
(SKI-IV phase). We searched for an excess of proton recoils
above the atmospheric neutrino background from the vicinity
of the Galactic Center. No such excess is observed, and
limits are calculated for two reference models of dark
matter with either a constant interaction cross section or
through a scalar mediator. This is the first experimental
search for boosted dark matter with hadrons using
directional information. The results present the most
stringent limits on cosmic-ray boosted dark matter and
exclude the dark matter-nucleon elastic scattering cross
section between 10^{-33}cm^{2} and 10^{-27}cm^{2} for dark
matter mass from 1 MeV/c^{2} to 300 MeV/c^{2}.},
Doi = {10.1103/physrevlett.130.031802},
Key = {fds369064}
}
@article{fds370037,
Author = {Guo, Z and Walter, CW and Lage, C and Lupton, RH},
Title = {Fringing Analysis and Simulation for the Vera C. Rubin
Observatory’s Legacy Survey of Space and
Time},
Journal = {Publications of the Astronomical Society of the
Pacific},
Volume = {135},
Number = {1045},
Pages = {034503-034503},
Publisher = {IOP Publishing},
Year = {2023},
Month = {March},
url = {http://dx.doi.org/10.1088/1538-3873/acbe67},
Abstract = {The presence of fringing in astronomical Charge-Coupled
Device (CCD) images will have an impact on photometric
quality and measurements. Yet its impact on the Vera C.
Rubin Observatory’s Legacy Survey of Space and Time (LSST)
has not been fully studied. We present a detailed study on
fringing for CCDs already implemented on the Rubin
Observatory LSST Camera’s focal plane. After making
physical measurements and knowing the compositions, we
developed a model for the e2v CCDs. We present a method to
fit for the internal height variation of the epoxy layer
within the sensors based on fringing measurements in a
laboratory setting. This method is generic enough that it
can be easily modified to work for other CCDs. Using the
derived fringing model, we successfully reproduce comparable
fringing amplitudes that match the observed levels in images
taken by existing telescopes with different optical designs.
This model is then used to forecast the expected level of
fringing in a single LSST y-band sky background exposure
with Rubin telescope optics in the presence of a realistic
time-varying sky spectrum. The predicted fringing amplitude
in LSST images ranges from 0.04% to 0.2% depending on the
location of a CCD on the focal plane. We find that the
predicted variation in surface brightness caused by fringing
in LSST y-band sky background images is about 0.6 μ Jy
arcsec − 2 , which is 40 times larger than the current
measurement error. We conclude that it is necessary to
include fringing correction in the Rubin’s LSST image
processing pipeline.},
Doi = {10.1088/1538-3873/acbe67},
Key = {fds370037}
}
@article{fds369344,
Author = {Longley, EP and Chang, C and Walter, CW and Zuntz, J and Ishak, M and Mandelbaum, R and Miyatake, H and Nicola, A and Pedersen, EM and Pereira, MES and Prat, J and Sánchez, J and Secco, LF and Tröster, T and Troxel, M and Wright, AH},
Title = {A unified catalogue-level reanalysis of stage-III cosmic
shear surveys},
Journal = {Monthly Notices of the Royal Astronomical
Society},
Volume = {520},
Number = {4},
Pages = {5016-5041},
Publisher = {Oxford University Press (OUP)},
Year = {2023},
Month = {April},
url = {http://dx.doi.org/10.1093/mnras/stad246},
Abstract = {Cosmological parameter constraints from recent galaxy
imaging surveys are reaching percent-level accuracy on the
effective amplitude of the lensing signal, S8. The upcoming
Legacy Survey of Space and Time (LSST) of the Vera C. Rubin
Observatory will produce subpercent level measurements of
cosmological parameters, providing a milestone test of the
CDM model. To supply guidance to the upcoming LSST analysis,
it is important to understand thoroughly the results from
different recent galaxy imaging surveys and assess their
consistencies. In this work, we perform a unified
catalogue-level reanalysis of three cosmic shear data sets:
the first year data from the Dark Energy Survey (DES-Y1),
the 1000 deg2 data set from the Kilo-Degree Survey
(KiDS-1000), and the first year data from the Hyper
Suprime-Cam Subaru Strategic Program (HSC-Y1). We utilize a
pipeline developed and rigorously tested by the LSST Dark
Energy Science Collaboration to perform the reanalysis and
assess the robustness of the results to analysis choices. We
find the S8 constraint to be robust to two different
small-scale modelling approaches, and varying choices of
cosmological priors. Our unified analysis allows the
consistency of the surveys to be rigorously tested, and we
find the three surveys to be statistically consistent. Due
to the partially overlapping footprint, we model the
cross-covariance between KiDS-1000 and HSC-Y1 approximately
when combining all three data sets, resulting in a 1.6–1.9
per cent constraint on S8 given different assumptions on the
cross-covariance.},
Doi = {10.1093/mnras/stad246},
Key = {fds369344}
}
@article{fds371709,
Author = {Shinoki, M and Abe, K and Hayato, Y and Hiraide, K and Hosokawa, K and Ieki, K and Ikeda, M and Kameda, J and Kanemura, Y and Kaneshima, R and Kashiwagi, Y and Kataoka, Y and Miki, S and Mine, S and Miura, M and Moriyama, S and Nakano, Y and Nakahata, M and Nakayama, S and Noguchi,
Y and Okamoto, K and Sato, K and Sekiya, H and Shiba, H and Shimizu, K and Shiozawa, M and Sonoda, Y and Suzuki, Y and Takeda, A and Takemoto, Y and Takenaka, A and Tanaka, H and Watanabe, S and Yano, T and Han, S and Kajita, T and Okumura, K and Tashiro, T and Tomiya, T and Wang, X and Yoshida, S and Megias, GD and Fernandez, P and Labarga, L and Ospina, N and Zaldivar, B and Pointon, BW and Kearns, E and Raaf, JL and Wan, L and Wester, T and Bian, J and Griskevich, NJ and Kropp, WR and Locke, S and Smy, MB and Sobel, HW and Takhistov, V and Yankelevich, A and Hill, J and Lee, SH and Moon, DH and Park, RG and Bodur, B and Scholberg, K and Walter,
CW and Beauchêne, A and Bernard, L and Coffani, A and Drapier, O and El
Hedri, S and Giampaolo, A and Mueller, TA and Santos, AD and Paganini,
P and Quilain, B and Ishizuka, T and Nakamura, T and Jang, JS and Learned,
JG and Choi, K and Cao, S and Anthony, LHV and Martin, D and Scott, M and Sztuc, AA and Uchida, Y and Berardi, V and Catanesi, MG and Radicioni,
E and Calabria, NF and Langella, A and Machado, LN and De Rosa and G and Collazuol, G and Iacob, F and Lamoureux, M and Mattiazzi, M and Ludovici, L and Gonin, M},
Title = {Measurement of the cosmogenic neutron yield in
Super-Kamiokande with gadolinium loaded water},
Journal = {Physical Review D},
Volume = {107},
Number = {9},
Year = {2023},
Month = {May},
url = {http://dx.doi.org/10.1103/PhysRevD.107.092009},
Abstract = {Cosmic-ray muons that enter the Super-Kamiokande detector
cause hadronic showers due to spallation in water, producing
neutrons and radioactive isotopes. These are a major
background source for studies of MeV-scale neutrinos and
searches for rare events. In 2020, gadolinium was introduced
into the ultra-pure water in the Super-Kamiokande detector
to improve the detection efficiency of neutrons. In this
study, the cosmogenic neutron yield was measured using data
acquired during the period after the gadolinium loading. The
yield was found to be (2.76±0.02(stat)±0.19(syst))×10-4
μ-1 g-1 cm2 at an average muon energy 259 GeV at the
Super-Kamiokande detector.},
Doi = {10.1103/PhysRevD.107.092009},
Key = {fds371709}
}
@article{fds370036,
Author = {Troxel, MA and Lin, C and Park, A and Hirata, C and Mandelbaum, R and Jarvis, M and Choi, A and Givans, J and Higgins, M and Sanchez, B and Yamamoto, M and Awan, H and Chiang, J and Doré, O and Walter, CW and Zhang, T and Cohen-Tanugi, J and Gawiser, E and Hearin, A and Heitmann,
K and Ishak, M and Kovacs, E and Mao, YY and Wood-Vasey,
M},
Title = {A joint Roman Space Telescope and Rubin Observatory
synthetic wide-field imaging survey},
Journal = {Monthly Notices of the Royal Astronomical
Society},
Volume = {522},
Number = {2},
Pages = {2801-2820},
Publisher = {Oxford University Press (OUP)},
Year = {2023},
Month = {June},
url = {http://dx.doi.org/10.1093/mnras/stad664},
Abstract = {We present and validate 20 deg2 of overlapping synthetic
imaging surveys representing the full depth of the Nancy
Grace Roman Space Telescope High-Latitude Imaging Survey
(HLIS) and 5 yr of observations of the Vera C. Rubin
Observatory Legacy Survey of Space and Time (LSST). The two
synthetic surveys are summarized, with reference to the
existing 300 deg2 of LSST simulated imaging produced as part
of Dark Energy Science Collaboration (DESC) Data Challenge 2
(DC2). Both synthetic surveys observe the same simulated
DESC DC2 universe. For the synthetic Roman survey, we
simulate for the first time fully chromatic images along
with the detailed physics of the Sensor Chip Assemblies
derived from lab measurements using the flight detectors.
The simulated imaging and resulting pixel-level measurements
of photometric properties of objects span a wavelength range
of ∼0.3–2.0 μm. We also describe updates to the Roman
simulation pipeline, changes in how astrophysical objects
are simulated relative to the original DC2 simulations, and
the resulting simulated Roman data products. We use these
simulations to explore the relative fraction of unrecognized
blends in LSST images, finding that 20–30 per cent of
objects identified in LSST images with i-band magnitudes
brighter than 25 can be identified as multiple objects in
Roman images. These simulations provide a unique testing
ground for the development and validation of joint
pixel-level analysis techniques of ground- and space-based
imaging data sets in the second half of the 2020s – in
particular the case of joint Roman–LSST
analyses.},
Doi = {10.1093/mnras/stad664},
Key = {fds370036}
}
@article{fds371635,
Author = {Harada, M and Abe, K and Bronner, C and Hayato, Y and Hiraide, K and Hosokawa, K and Ieki, K and Ikeda, M and Kameda, J and Kanemura, Y and Kaneshima, R and Kashiwagi, Y and Kataoka, Y and Miki, S and Mine, S and Miura, M and Moriyama, S and Nakano, Y and Nakahata, M and Nakayama, S and Noguchi, Y and Okamoto, K and Sato, K and Sekiya, H and Shiba, H and Shimizu, K and Shiozawa, M and Sonoda, Y and Suzuki, Y and Takeda, A and Takemoto, Y and Takenaka, A and Tanaka, H and Watanabe, S and Yano, T and Han, S and Kajita, T and Okumura, K and Tashiro, T and Tomiya, T and Wang,
X and Yoshida, S and Megias, GD and Fernandez, P and Labarga, L and Ospina,
N and Zaldivar, B and Pointon, BW and Kearns, E and Raaf, JL and Wan, L and Wester, T and Bian, J and Griskevich, NJ and Locke, S and Smy, MB and Sobel, HW and Takhistov, V and Yankelevich, A and Hill, J and Lee, SH and Moon, DH and Park, RG and Bodur, B and Scholberg, K and Walter, CW and Beauchêne, A and Drapier, O and Giampaolo, A and Mueller, TA and Santos, AD and Paganini, P and Quilain, B and Ishizuka, T and Nakamura,
T and Jang, JS and Learned, JG and Choi, K and Iovine, N and Cao, S and Anthony, LHV and Martin, D and Scott, M and Sztuc, AA and Uchida, Y and Berardi, V and Catanesi, MG and Radicioni, E and Calabria, NF and Langella, A and Machado, LN and De Rosa and G and Collazuol, G and Iacob,
F and Lamoureux, M and Mattiazzi, M and Ludovici, L and Gonin, M and Pronost, G and Fujisawa, C},
Title = {Search for Astrophysical Electron Antineutrinos in
Super-Kamiokande with 0.01% Gadolinium-loaded
Water},
Journal = {Astrophysical Journal Letters},
Volume = {951},
Number = {2},
Pages = {L27-L27},
Publisher = {American Astronomical Society},
Year = {2023},
Month = {July},
url = {http://dx.doi.org/10.3847/2041-8213/acdc9e},
Abstract = {We report the first search result for the flux of
astrophysical electron antineutrinos for energies(10)MeV in
the gadolinium-loaded Super-Kamiokande (SK) detector. In
2020 June, gadolinium was introduced to the ultrapure water
of the SK detector in order to detect neutrons more
efficiently. In this new experimental phase, SK-Gd, we can
search for electron antineutrinos via inverse beta decay
with efficient background rejection thanks to the high
efficiency of the neutron tagging technique. In this paper,
we report the result for the initial stage of SK-Gd, during
2020 August 26, and 2022 June 1 with a 22.5 × 552 kton ·
day exposure at 0.01% Gd mass concentration. No significant
excess over the expected background in the observed events
is found for the neutrino energies below 31.3 MeV. Thus, the
flux upper limits are placed at the 90% confidence level.
The limits and sensitivities are already comparable with the
previous SK result with pure water (22.5 × 2970 kton ·
day) owing to the enhanced neutron tagging. Operation with
Gd increased to 0.03% started in 2022 June.},
Doi = {10.3847/2041-8213/acdc9e},
Key = {fds371635}
}
@article{fds375135,
Author = {Abe, K and Hayato, Y and Hiraide, K and Ieki, K and Ikeda, M and Kameda, J and Kanemura, Y and Kaneshima, R and Kashiwagi, Y and Kataoka, Y and Miki,
S and Mine, S and Miura, M and Moriyama, S and Nakano, Y and Nakahata, M and Nakayama, S and Noguchi, Y and Okamoto, K and Sato, K and Sekiya, H and Shiba, H and Shimizu, K and Shiozawa, M and Sonoda, Y and Suzuki, Y and Takeda, A and Takemoto, Y and Takenaka, A and Tanaka, H and Watanabe, S and Yano, T and Han, S and Kajita, T and Okumura, K and Tashiro, T and Tomiya,
T and Wang, X and Xia, J and Yoshida, S and Megias, GD and Fernandez, P and Labarga, L and Ospina, N and Zaldivar, B and Pointon, BW and Kearns, E and Raaf, JL and Wan, L and Wester, T and Bian, J and Griskevich, NJ and Kropp,
WR and Locke, S and Smy, MB and Sobel, HW and Takhistov, V and Yankelevich,
A and Hill, J and Park, RG and Bodur, B and Scholberg, K and Walter, CW and Bernard, L and Coffani, A and Drapier, O and El Hedri and S and Giampaolo,
A and Mueller, TA and Santos, AD and Paganini, P and Quilain, B and Ishizuka, T and Nakamura, T and Jang, JS and Learned, JG and Choi, K and Cao, S and Anthony, LHV and Martin, D and Scott, M and Sztuc, AA and Uchida, Y and Berardi, V and Catanesi, MG and Radicioni, E and Calabria,
NF and Machado, LN and De Rosa and G and Collazuol, G and Iacob, F and Lamoureux, M and Mattiazzi, M and Ludovici, L and Gonin, M and Pronost,
G and Fujisawa, C and Maekawa, Y and Nishimura, Y and Friend, M and Hasegawa, T and Ishida, T and Kobayashi, T and Jakkapu, M and Matsubara,
T and Nakadaira, T and Nakamura, K and Oyama, Y and Sakashita, K and Sekiguchi, T and Tsukamoto, T and Boschi, T and Di Lodovico and F and Gao,
J and Goldsack, A and Katori, T and Migenda, J and Taani, M and Zsoldos, S and Kotsar, Y and Ozaki, H and Suzuki, AT and Takeuchi, Y and Bronner, C and Feng, J and Kikawa, T and Mori, M and Nakaya, T and Wendell, RA and Yasutome, K and Jenkins, SJ and McCauley, N and Mehta, P and Tsui, KM and Fukuda, Y and Itow, Y and Menjo, H and Ninomiya, K and Lagoda, J and Lakshmi, SM and Mandal, M and Mijakowski, P and Prabhu, YS and Zalipska,
J and Jia, M and Jiang, J and Jung, CK and Wilking, MJ and Yanagisawa, C and Harada, M and Ishino, H and Ito, S and Kitagawa, H and Koshio, Y and Nakanishi, F and Sakai, S and Barr, G and Barrow, D and Cook, L and Samani,
S and Wark, D and Nova, F and Yang, JY and Malek, M and McElwee, JM and Stone,
O and Thiesse, MD and Thompson, LF and Okazawa, H and Kim, SB and Seo, JW and Yu, I and Ichikawa, AK and Nakamura, KD and Tairafune, S and Nishijima,
K and Iwamoto, K and Nakagiri, K and Nakajima, Y and Taniuchi, N and Yokoyama, M and Martens, K and de Perio, P and Vagins, MR and Kuze, M and Izumiyama, S and Inomoto, M and Ishitsuka, M and Ito, H and Kinoshita,
T and Matsumoto, R and Ommura, Y and Shigeta, N and Shinoki, M and Suganuma, T and Yamauchi, K and Martin, JF and Tanaka, HA and Towstego,
T and Akutsu, R and Gousy-Leblanc, V and Hartz, M and Konaka, A and Prouse,
NW and Chen, S and Xu, BD and Zhang, B and Posiadala-Zezula, M and Hadley,
D and Nicholson, M and O'Flaherty, M and Richards, B and Ali, A and Jamieson, B and Marti, L and Minamino, A and Pintaudi, G and Sano, S and Suzuki, S and Wada, K and Super-Kamiokande Collaboration},
Title = {Erratum: Search for Cosmic-Ray Boosted Sub-GeV Dark Matter
Using Recoil Protons at Super-Kamiokande [Phys. Rev. Lett.
130, 031802 (2023)].},
Journal = {Physical review letters},
Volume = {131},
Number = {15},
Pages = {159903},
Year = {2023},
Month = {October},
url = {http://dx.doi.org/10.1103/physrevlett.131.159903},
Abstract = {This corrects the article DOI: 10.1103/PhysRevLett.130.031802.},
Doi = {10.1103/physrevlett.131.159903},
Key = {fds375135}
}
@article{fds375284,
Author = {Sakai, S and Abe, K and Bronner, C and Hayato, Y and Hiraide, K and Hosokawa, K and Ieki, K and Ikeda, M and Kameda, J and Kanemura, Y and Kaneshima, R and Kashiwagi, Y and Kataoka, Y and Miki, S and Mine, S and Miura, M and Moriyama, S and Nakano, Y and Nakahata, M and Nakayama, S and Noguchi, Y and Sato, K and Sekiya, H and Shiba, H and Shimizu, K and Shiozawa, M and Sonoda, Y and Suzuki, Y and Takeda, A and Takemoto, Y and Tanaka, H and Yano, T and Han, S and Kajita, T and Okumura, K and Tashiro,
T and Tomiya, T and Wang, X and Yoshida, S and Fernandez, P and Labarga, L and Ospina, N and Zaldivar, B and Pointon, BW and Kearns, E and Raaf, JL and Wan, L and Wester, T and Bian, J and Griskevich, NJ and Locke, S and Smy,
MB and Sobel, HW and Takhistov, V and Yankelevich, A and Hill, J and Jang,
MC and Lee, SH and Moon, DH and Park, RG and Bodur, B and Scholberg, K and Walter, CW and Beauchêne, A and Drapier, O and Giampaolo, A and Mueller, TA and Santos, AD and Paganini, P and Quilain, B and Nakamura,
T and Jang, JS and Machado, LN and Learned, JG and Choi, K and Iovine, N and Cao, S and Anthony, LHV and Martin, D and Prouse, NW and Scott, M and Sztuc, AA and Uchida, Y and Berardi, V and Calabria, NF and Catanesi,
MG and Radicioni, E and Langella, A and De Rosa and G and Collazuol, G and Iacob, F and Mattiazzi, M and Ludovici, L and Gonin, M and Pronost, G and Fujisawa, C and Maekawa, Y and Nishimura, Y and Okazaki, R and Akutsu,
R},
Title = {Measurement of the neutrino-oxygen neutral-current
quasielastic cross section using atmospheric neutrinos in
the SK-Gd experiment},
Journal = {Physical Review D},
Volume = {109},
Number = {1},
Publisher = {American Physical Society (APS)},
Year = {2024},
Month = {January},
url = {http://dx.doi.org/10.1103/PhysRevD.109.L011101},
Abstract = {We report the first measurement of the atmospheric
neutrino-oxygen neutral-current quasielastic (NCQE) cross
section in the gadolinium-loaded Super-Kamiokande (SK) water
Cherenkov detector. In June 2020, SK began a new
experimental phase, named SK-Gd, by loading 0.011% by mass
of gadolinium into the ultrapure water of the SK detector.
The introduction of gadolinium to ultrapure water has the
effect of improving the neutron-tagging efficiency. Using a
552.2 day dataset from August 2020 to June 2022, we measure
the NCQE cross section to be 0.74±0.22(stat)-0.15+0.85(syst)×10-38
cm2/oxygen in the energy range from 160 MeV to 10 GeV, which
is consistent with the atmospheric neutrino-flux-averaged
theoretical NCQE cross section and the measurement in the SK
pure-water phase within the uncertainties. Furthermore, we
compare the models of the nucleon-nucleus interactions in
water and find that the binary cascade model and the Liège
intranuclear cascade model provide a somewhat better fit to
the observed data than the Bertini cascade model. Since the
atmospheric neutrino-oxygen NCQE reactions are one of the
main backgrounds in the search for diffuse supernova
neutrino background (DSNB), these new results will
contribute to future studies - and the potential discovery -
of the DSNB in SK.},
Doi = {10.1103/PhysRevD.109.L011101},
Key = {fds375284}
}
@article{fds375968,
Author = {Nicola, A and Hadzhiyska, B and Findlay, N and García-García, C and Alonso, D and Slosar, A and Guo, Z and Kokron, N and Angulo, R and Aviles,
A and Blazek, J and Dunkley, J and Jain, B and Pellejero, M and Sullivan,
J and Walter, CW and Zennaro, M},
Title = {Galaxy bias in the era of LSST: perturbative bias
expansions},
Journal = {Journal of Cosmology and Astroparticle Physics},
Volume = {2024},
Number = {2},
Pages = {015-015},
Publisher = {IOP Publishing},
Year = {2024},
Month = {February},
url = {http://dx.doi.org/10.1088/1475-7516/2024/02/015},
Abstract = {Upcoming imaging surveys will allow for high signal-to-noise
measurements of galaxy clustering at small scales. In this
work, we present the results of the Rubin Observatory Legacy
Survey of Space and Time (LSST) bias challenge, the goal of
which is to compare the performance of different nonlinear
galaxy bias models in the context of LSST Year 10 (Y10)
data. Specifically, we compare two perturbative approaches,
Lagrangian perturbation theory (LPT) and Eulerian
perturbation theory (EPT) to two variants of Hybrid
Effective Field Theory (HEFT), with our fiducial
implementation of these models including terms up to second
order in the bias expansion as well as nonlocal bias and
deviations from Poissonian stochasticity. We consider a
variety of different simulated galaxy samples and test the
performance of the bias models in a tomographic joint
analysis of LSST-Y10-like galaxy clustering,
galaxy-galaxy-lensing and cosmic shear. We find both HEFT
methods as well as LPT and EPT combined with
non-perturbative predictions for the matter power spectrum
to yield unbiased constraints on cosmological parameters up
to at least a maximal scale of k max = 0.4 Mpc-1 for all
samples considered, even in the presence of assembly bias.
While we find that we can reduce the complexity of the bias
model for HEFT without compromising fit accuracy, this is
not generally the case for the perturbative models. We find
significant detections of non-Poissonian stochasticity in
all cases considered, and our analysis shows evidence that
small-scale galaxy clustering predominantly improves
constraints on galaxy bias rather than cosmological
parameters. These results therefore suggest that the
systematic uncertainties associated with current nonlinear
bias models are likely to be subdominant compared to other
sources of error for tomographic analyses of upcoming
photometric surveys, which bodes well for future galaxy
clustering analyses using these high signal-to-noise
data.},
Doi = {10.1088/1475-7516/2024/02/015},
Key = {fds375968}
}
@article{fds376106,
Author = {Hirata, CM and Yamamoto, M and Laliotis, K and Macbeth, E and Troxel,
MA and Zhang, T and Cao, K and Choi, A and Givans, J and Heitmann, K and Ishak, M and Jarvis, M and Kovacs, E and Long, H and Mandelbaum, R and Park, A and Porredon, A and Walter, CW and Wood-Vasey,
WM},
Title = {Simulating image coaddition with the Nancy Grace Roman Space
Telescope – I. Simulation methodology and general
results},
Journal = {Monthly Notices of the Royal Astronomical
Society},
Volume = {528},
Number = {2},
Pages = {2533-2561},
Year = {2024},
Month = {February},
url = {http://dx.doi.org/10.1093/mnras/stae182},
Abstract = {The upcoming Nancy Grace Roman Space Telescope will carry
out a wide-area survey in the near-infrared. A key science
objective is the measurement of cosmic structure via weak
gravitational lensing. Roman data will be undersampled,
which introduces new challenges in the measurement of source
galaxy shapes; a potential solution is to use linear
algebra-based coaddition techniques such as IMCOM that
combine multiple undersampled images to produce a single
oversampled output mosaic with a desired ‘target’ point
spread function (PSF). We present here an initial
application of IMCOM to 0.64 square degrees of simulated
Roman data, based on the Roman branch of the Legacy Survey
of Space and Time (LSST) Dark Energy Science Collaboration
(DESC) Data Challenge 2 (DC2) simulation. We show that IMCOM
runs successfully on simulated data that includes features
such as plate scale distortions, chip gaps, detector
defects, and cosmic ray masks. We simultaneously propagate
grids of injected sources and simulated noise fields as well
as the full simulation. We quantify the residual deviations
of the PSF from the target (the ‘leakage’), as well as
noise properties of the output images; we discuss how the
overall tiling pattern as well as Moiré patterns appear in
the final leakage and noise maps. We include appendices on
interpolation algorithms and the interaction of
undersampling with image processing operations that may be
of broader applicability. The companion paper (‘Paper
II’) explores the implications for weak lensing
analyses.},
Doi = {10.1093/mnras/stae182},
Key = {fds376106}
}
%% Papers Accepted
@techreport{2km-loi,
Author = {The T2K Collaboration},
Title = {A letter of intent to extend T2K with a detector 2~km away
from the JPARC neutrino source},
Editor = {Chris Walter},
Year = {2007},
Key = {2km-loi}
}
%% Preprints
@article{Super-Kamiokande:2021the,
Author = {Abe, K and Bronner, C and Hayato, Y and Hiraide, K and Ikeda, M and Imaizumi, S and Kameda, J and Kanemura, Y and Kataoka, Y and Miki, S and Miura, M and Moriyama, S and Nagao, Y and Nakahata, M and Nakayama, S and Okada, T and Okamoto, K and Orii, A and Pronost, G and Sekiya, H and Shiozawa, M and Sonoda, Y and Suzuki, Y and Takeda, A and Takemoto, Y and Takenaka, A and Tanaka, H and Watanabe, S and Yano, T and Han, S and Kajita, T and Okumura, K and Tashiro, T and Xia, J and Megias, GD and Bravo-Berguno, D and Labarga, L and Marti, L and Zaldivar, B and Pointon, BW and Blaszczyk, FDM and Kearns, E and Raaf, JL and Stone, JL and Wan, L and Wester, T and Bian, J and Griskevich, NJ and Kropp, WR and Locke, S and Mine, S and Smy, MB and Sobel, HW and Takhistov, V and Hill,
J and Kim, JY and Lim, IT and Park, RG and Bodur, B and Scholberg, K and Walter, CW and Bernard, L and Coffani, A and Drapier, O and Hedri, SE and Giampaolo, A and Gonin, M and Mueller, TA and Paganini, P and Quilain,
B and Ishizuka, T and Nakamura, T and Jang, JS and Learned, JG and Anthony,
LHV and Martin, D and Scott, M and Sztuc, AA and Uchida, Y and Cao, S and Berardi, V and Catanesi, MG and Radicioni, E and Calabria, NF and Machado, LN and Rosa, GD and Collazuol, G and Iacob, F and Lamoureux, M and Mattiazzi, M and Ospina, N and Ludovici, L and Maekawa, Y and Nishimura,
Y and Friend, M and Hasegawa, T and Ishida, T and Kobayashi, T and Jakkapu,
M and Matsubara, T and Nakadaira, T and Nakamura, K and Oyama, Y and Sakashita, K and Sekiguchi, T and Tsukamoto, T and Boschi, T and Gao, J and Lodovico, FD and Migenda, J and Taani, M and Zsoldos, S and Kotsar, Y and Nakano, Y and Ozaki, H and Shiozawa, T and Suzuki, AT and Takeuchi, Y and Yamamoto, S and Ali, A and Ashida, Y and Feng, J and Hirota, S and Kikawa,
T and Mori, M and Nakaya, T and Wendell, RA and Yasutome, K and Fernandez,
P and McCauley, N and Mehta, P and Tsui, KM and Fukuda, Y and Itow, Y and Menjo, H and Niwa, T and Sato, K and Tsukada, M and Lagoda, J and Lakshmi,
SM and Mijakowski, P and Zalipska, J and Jiang, J and Jung, CK and Vilela,
C and Wilking, MJ and Yanagisawa, C and Hagiwara, K and Harada, M and Horai, T and Ishino, H and Ito, S and Kitagawa, F and Koshio, Y and Ma, W and Piplani, N and Sakai, S and Barr, G and Barrow, D and Cook, L and Goldsack,
A and Samani, S and Wark, D and Nova, F and Yang, JY and Jenkins, SJ and Malek, M and McElwee, JM and Stone, O and Thiesse, MD and Thompson, LF and Okazawa, H and Kim, SB and Seo, JW and Yu, I and Ichikawa, AK and Nishijima, K and Koshiba, M and Iwamoto, K and Nakajima, Y and Ogawa, N and Yokoyama, M and Martens, K and Vagins, MR and Kuze, M and Izumiyama, S and Yoshida, T and Inomoto, M and Ishitsuka, M and Ito, H and Kinoshita, T and Matsumoto, R and Ohta, K and Shinoki, M and Suganuma, T and Martin, JF and Tanaka, HA and Towstego, T and Akutsu, R and Hartz, M and Konaka, A and Perio, PD and Prouse, NW and Chen, S and Xu, BD and Posiadala-Zezula, M and Hadley, D and O'Flaherty, M and Richards, B and Jamieson, B and Walker,
J and Minamino, A and Pintaudi, G and Sano, S and Sasaki,
R},
Title = {First Gadolinium Loading to Super-Kamiokande},
Year = {2021},
Month = {September},
url = {http://arxiv.org/pdf/2109.00360},
Abstract = {http://arxiv.org/abs/2109.00360},
Key = {Super-Kamiokande:2021the}
}
@article{fds365853,
Author = {Collaboration, S-K and Weatherly, P and Abe, K and Bronner, C and Hayato, Y and Hiraide, K and Ikeda, M and Iyogi, K and Kameda, J and Kanemura, Y and Kataoka, Y and Kato, Y and Kishimoto, Y and Miki, S and Miura, M and Moriyama, S and Mochizuki, T and Nakahata, M and Nakano, Y and Nakayama, S and Okada, T and Okamoto, K and Orii, A and Pronost, G and Sato, K and Sekiya, H and Shiozawa, M and Sonoda, Y and Suzuki, Y and Takeda, A and Takemoto, Y and Takenaka, A and Tanaka, H and Tasaka, S and Wang, X and Watanabe, S and Yano, T and Han, S and Kajita, T and Kaneyuki,
K and Okumura, K and Tashiro, T and Wang, R and Xia, J and Megias, GD and Labarga, L and Zaldivar, B and Pointon, BW and Blaszczyk, FDM and Kachulis, C and Kearns, E and Raaf, JL and Stone, JL and Sulak, LR and Sussman, S and Wan, L and Wester, T and Berkman, S and Tobayama, S and Bian, J and Elnimr, M and Griskevich, NJ and Kropp, WR and Locke, S and Mine, S and Smy, MB and Sobel, HW and Takhistov, V and Yankelevich, A and Ganezer, KS and Hill, J and Kim, JY and Lim, IT and Park, RG and Bodur, B and Li, Z and Scholberg, K and Walter, CW and Bernard, L and Coffani, A and Drapier, O and Giampaolo, A and Hedri, SE and Imber, J and Mueller, TA and Paganini, P and Quilain, B and Santos, AD and Ishizuka, T and Nakamura,
T and Jang, JS and Learned, JG and Matsuno, S and Cao, S and Amey, J and Anthony, LHV and Litchfield, RP and Ma, WY and Martin, D and Scott, M and Sztuc, AA and Uchida, Y and Wascko, MO and Berardi, V and Catanesi, MG and Intonti, RA and Radicioni, E and Calabria, NF and Machado, LN and Rosa,
GD and Collazuol, G and Iacob, F and Lamoureux, M and Mattiazzi, M and Ospina, N and Ludovici, L and Gonin, M and Maekawa, Y and Nishimura, Y and Friend, M and Hasegawa, T and Ishida, T and Jakkapu, M and Kobayashi, T and Matsubara, T and Nakadaira, T and Nakamura, K and Oyama, Y and Sakashita, K and Sekiguchi, T and Tsukamoto, T and Boschi, T and Lodovico, FD and Gao, J and Katori, T and Migenda, J and Taani, M and Zsoldos, S and Abe, KE and Hasegawa, M and Isobe, Y and Kotsar, Y and Miyabe, H and Ozaki, H and Sugimoto, T and Suzuki, AT and Takeuchi, Y and Yamamoto, S and Ashida, Y and Feng, J and Hayashino, T and Hirota, S and Jiang, M and Kikawa, T and Mori, M and Nakaya, T and Wendell, RA and Yasutome, K and Fernandez, P and McCauley, N and Mehta, P and Pritchard,
A and Tsui, KM and Fukuda, Y and Itow, Y and Menjo, H and Murase, M and Frankiewicz, K and Lagoda, J and Lakshmi, SM and Mandal, M and Mijakowski, P and Prabhu, YS and Zalipska, J and Jia, M and Jiang, J and Jung, CK and Li, X and Palomino, JL and Santucci, G and Vilela, C and Wilking, MJ and Yanagisawa, C and Fukuda, D and Hagiwara, K and Harada,
M and Ishino, H and Ito, S and Kitagawa, H and Koshio, Y and Ma, W and Sakai,
S and Sakuda, M and Takahira, Y and Xu, C and Kuno, Y and Barr, G and Barrow,
D and Cook, L and Goldsack, A and Samani, S and Simpson, C and Wark, D and Sedgwick, SM and Tacik, R and Nova, F and Yang, JY and Jenkins, SJ and Malek, M and McElwee, JM and Stone, O and Thiesse, MD and Thompson, LF and Okazawa, H and Choi, Y and Kim, SB and Seo, JW and Yu, I and Ichikawa, A and Nakamura, KD and Nishijima, K and Koshiba, M and Iwamoto, K and Nakagiri, K and Nakajima, Y and Suda, Y and Taniuchi, N and Yokoyama, M and Martens, K and Murdoch, M and Vagins, MR and Hamabe, D and Izumiyama, S and Kuze, M and Okajima, Y and Yoshida, T and Inomoto, M and Ishitsuka, M and Ito, H and Kinoshita, T and Matsumoto, R and Shinoki, M and Suganuma, T and Yonenaga, M and Martin, JF and Nantais, CM and Tanaka, HA and Towstego,
T and Akutsu, R and Perio, PD and Gousy-Leblanc, V and Hartz, M and Konaka,
A and Prouse, NW and Chen, S and Xu, BD and Zhang, B and Posiadala-Zezula,
M and Hadley, D and Nicholson, M and O'Flaherty, M and Richards, B and Ali,
A and Jamieson, B and Giorgio, P and Marti, L and Minamino, A and Pintaudi,
G and Sano, S and Sasaki, R and Wada, K},
Title = {Testing Non-Standard Interactions Between Solar Neutrinos
and Quarks with Super-Kamiokande},
Year = {2022},
Month = {March},
Key = {fds365853}
}
@article{fds365508,
Author = {Collaboration, S-K and Machado, LN and Abe, K and Hayato, Y and Hiraide,
K and Ieki, K and Ikeda, M and Kameda, J and Kanemura, Y and Kaneshima, R and Kashiwagi, Y and Kataoka, Y and Miki, S and Mine, S and Miura, M and Moriyama, S and Nakano, Y and Nakahata, M and Nakayama, S and Noguchi,
Y and Okamoto, K and Sato, K and Sekiya, H and Shiba, H and Shimizu, K and Shiozawa, M and Sonoda, Y and Suzuki, Y and Takeda, A and Takemoto, Y and Takenaka, A and Tanaka, H and Watanabe, S and Yano, T and Perio, PD and Martens, K and Vagins, MR and Bian, J and Griskevich, NJ and Kropp, WR and Locke, S and Smy, MB and Sobel, HW and Takhistov, V and Yankelevich, A and Han, S and Kajita, T and Okumura, K and Tashiro, T and Tomiya, T and Wang,
X and Xia, J and Yoshida, S and Megias, GD and Fernandez, P and Labarga, L and Ospina, N and Zaldivar, B and Pointon, BW and Akutsu, R and Gousy-Leblanc, V and Hartz, M and Konaka, A and Prouse, NW and Kearns,
E and Raaf, JL and Wan, L and Wester, T and Hill, J and Kim, JY and Lim, IT and Park, RG and Bodur, B and Scholberg, K and Walter, CW and Bernard, L and Coffani, A and Drapier, O and Hedri, SE and Giampaolo, A and Mueller,
TA and Santos, AD and Paganini, P and Quilain, B and Ishizuka, T and Nakamura, T and Jang, JS and Learned, JG and Cao, S and Choi, K and Anthony, LHV and Martin, D and Scott, M and Sztuc, AA and Uchida, Y and Berardi, V and Catanesi, MG and Radicioni, E and Calabria, NF and Rosa,
GD and Collazuol, G and Iacob, F and Lamoureux, M and Mattiazzi, M and Ludovici, L and Gonin, M and Pronost, G and Fujisawa, C and Maekawa, Y and Nishimura, Y and Sasaki, R and Friend, M and Hasegawa, T and Ishida, T and Jakkapu, M and Kobayashi, T and Matsubara, T and Nakadaira, T and Nakamura, K and Oyama, Y and Sakashita, K and Sekiguchi, T and Tsukamoto, T and Boschi, T and Lodovico, FD and Gao, J and Goldsack, A and Katori, T and Migenda, J and Taani, M and Zsoldos, S and Kotsar, Y and Ozaki, H and Suzuki, AT and Takeuchi, Y and Yaamoto, S and Bronner, C and Feng, J and Kikawa, T and Mori, M and Nakaya, T and Wendell, RA and Yasutome, K and Jenkins, SJ and McCauley, N and Mehta, P and Tsui, KM and Fukuda, Y and Itow, Y and Menjo, H and Ninomiya, K and Lagoda, J and Lakshmi, SM and Mandal, M and Mijakowski, P and Prabhu, YS and Zalipska,
J and Jia, M and Jiang, J and Jung, CK and Wilking, MJ and Yanagisawa, C and Harada, M and Ishino, H and Ito, S and Kitagawa, H and Koshio, Y and Ma, W and Nakanishi, F and Sakai, S and Barr, G and Barrow, D and Cook, L and Samani,
S and Wark, D and Nova, F and Yang, JY and Malek, M and McElwee, JM and Stone,
O and Thiesse, MD and Thompson, LF and Okazawa, H and Kim, SB and Seo, JW and Yu, I and Ichikawa, AK and Nakamura, KD and Tairafune, S and Nishijima,
K and Iwamoto, K and Nakagiri, K and Nakajima, Y and Taniuchi, N and Yokoyama, M and Izumiyama, S and Kuze, M and Inomoto, M and Ishitsuka,
M and Ito, H and Kinoshita, T and Matsumoto, R and Ommura, Y and Shigeta,
N and Shinoki, M and Suganuma, T and Yonenaga, M and Martin, JF and Tanaka,
HA and Towstego, T and Chen, S and Xu, BD and Zhang, B and Posiadala-Zezula, M and Hadley, D and Nicholson, M and O'Flaherty, M and Richards, B and Ali, A and Jamieson, B and Marti, L and Minamino, A and Pintaudi, G and Sano, S and Suzuki, S and Wada, K},
Title = {Pre-Supernova Alert System for Super-Kamiokande},
Year = {2022},
Month = {May},
Key = {fds365508}
}
@article{fds363991,
Author = {collaboration, TS-K and Mori, M and Abe, K and Hayato, Y and Hiraide, K and Ieki, K and Ikeda, M and Imaizumi, S and Kameda, J and Kanemura, Y and Kaneshima, R and Kashiwagi, Y and Kataoka, Y and Miki, S and Mine, S and Miura, M and Moriyama, S and Nagao, Y and Nakahata, M and Nakano, Y and Nakayama, S and Noguchi, Y and Okada, T and Okamoto, K and Orii, A and Sato, K and Sekiya, H and Shiba, H and Shimizu, K and Shiozawa, M and Sonoda, Y and Suzuki, Y and Takeda, A and Takemoto, Y and Takenaka, A and Tanaka, H and Tomiya, T and Watanabe, S and Yano, T and Yoshida, S and Han,
S and Kajita, T and Okumura, K and Tashiro, T and Wang, X and Xia, J and Megias, GD and Bravo-Berguno, D and Fernandez, P and Labarga, L and Ospina, N and Zaldivar, B and Zsoldos, S and Pointon, BW and Blaszczyk,
FDM and Kearns, E and Raaf, JL and Stone, JL and Wan, L and Wester, T and Bian, J and Griskevich, NJ and Kropp, WR and Locke, S and Smy, MB and Sobel, HW and Takhistov, V and Yankelevich, and Hill, J and Kim, JY and Lim, IT and Park, RG and Bodur, B and Scholberg, K and Walter, CW and Bernard, L and Coffani, A and Drapier, O and Hedri, SE and Giampaolo, A and Mueller, TA and Paganini, P and Quilain, B and Santos, AD and Ishizuka,
T and Nakamura, T and Jang, JS and Learned, JG and Anthony, LHV and Martin,
D and Scott, M and Sztuc, AA and Uchida, Y and Berardi, V and Catanesi, MG and Radicioni, E and Calabria, NF and Machado, LN and Rosa, GD and Collazuol, G and Iacob, F and Lamoureux, M and Mattiazzi, M and Ludovici, L and Gonin, M and Pronost, G and Maekawa, Y and Nishimura, Y and Fujisawa, C and Friend, M and Hasegawa, T and Ishida, T and Kobayashi,
T and Jakkapu, M and Matsubara, T and Nakadaira, T and Nakamura, K and Oyama, Y and Sakashita, K and Sekiguchi, T and Tsukamoto, T and Ozaki,
H and Shiozawa, T and Suzuki, AT and Takeuchi, Y and Yamamoto, S and Kotsar, Y and Ashida, Y and Bronner, C and Feng, J and Hirota, S and Kikawa, T and Nakaya, T and Wendell, RA and Yasutome, K and McCauley, N and Mehta, P and Tsui, KM and Fukuda, Y and Itow, Y and Menjo, H and Ninomiya,
K and Niwa, T and Tsukada, M and Lagoda, J and Lakshmi, SM and Mijakowski,
P and Zalipska, J and Mandal, M and Prabhu, YS and Jiang, J and Jung, CK and Vilela, C and Wilking, MJ and Yanagisawa, C and Jia, M and Hagiwara, K and Harada, M and Horai, T and Ishino, H and Ito, S and Kitagawa, H and Koshio,
Y and Ma, W and Nakanishi, F and Piplani, N and Sakai, S and Barr, G and Barrow, D and Cook, L and Samani, S and Wark, D and Nova, F and Boschi, T and Gao, J and Goldsack, A and Katori, T and Lodovico, FD and Migenda, J and Taani, M and Yang, JY and Jenkins, SJ and Malek, M and McElwee, JM and Stone, O and Thiesse, MD and Thompson, LF and Okazawa, H and Kim, SB and Seo, JW and Yu, I and Nishijima, K and Koshiba, M and Nakagiri, K and Nakajima, Y and Iwamoto, K and Taniuchi, N and Yokoyama, M and Martens,
K and Perio, PD and Vagins, MR and Kuze, M and Izumiyama, S and Yoshida, T and Inomoto, M and Ishitsuka, M and Ito, H and Kinoshita, T and Matsumoto,
R and Ohta, K and Ommura, Y and Shigeta, N and Shinoki, M and Suganuma, T and Yamauchi, K and Martin, JF and Tanaka, HA and Towstego, T and Akutsu, R and Gousy-Leblanc, V and Hartz, M and Konaka, A and Prouse, NW and Chen, S and Xu, BD and Zhang, B and Posiadala-Zezula, M and Hadley, D and Nicholson,
M and Flaherty, MO and Richards, B and Ali, A and Jamieson, B and Walker,
J and Marti, L and Minamino, A and Pintaudi, G and Sasaki, R and Sano, S and Suzuki, S and Wada, K and Cao, S and Ichikawa, A and Nakamura, KD and Tairafun, S},
Title = {Search for supernova bursts in Super-Kamiokande
IV},
Year = {2022},
Month = {June},
Key = {fds363991}
}
@article{fds365852,
Author = {Longley, EP and Chang, C and Walter, CW and Zuntz, J and Ishak, M and Mandelbaum, R and Miyatake, H and Nicola, A and Pedersen, EM and Pereira, MES and Prat, J and Sánchez, J and Tröster, T and Troxel, M and Wright, A and Collaboration, TLSSTDES},
Title = {A Unified Catalog-level Reanalysis of Stage-III Cosmic Shear
Surveys},
Year = {2022},
Month = {August},
Key = {fds365852}
}
@article{fds375015,
Author = {Collaboration, S-K and Matsumoto, R and Abe, K and Hayato, Y and Hiraide, K and Ieki, K and Ikeda, M and Kameda, J and Kanemura, Y and Kaneshima, R and Kashiwagi, Y and Kataoka, Y and Miki, S and Mine, S and Miura, M and Moriyama, S and Nakano, Y and Nakahata, M and Nakayama, S and Noguchi, Y and Okamoto, K and Sato, K and Sekiya, H and Shiba, H and Shimizu, K and Shiozawa, M and Sonoda, Y and Suzuki, Y and Takeda, A and Takemoto, Y and Takenaka, A and Tanaka, H and Watanabe, S and Yano, T and Han, S and Kajita, T and Okumura, K and Tashiro, T and Tomiya, T and Wang,
X and Xia, J and Yoshida, S and Megias, GD and Fernandez, P and Labarga, L and Ospina, N and Zaldivar, B and Pointon, BW and Kearns, E and Raaf, JL and Wan, L and Wester, T and Bian, J and Griskevich, NJ and Kropp, WR and Locke, S and Smy, MB and Sobel, HW and Takhistov, V and Yankelevich, A and Hill, J and Kim, JY and Lim, IT and Park, RG and Bodur, B and Scholberg, K and Walter, CW and Bernard, L and Coffani, A and Drapier, O and Hedri, SE and Giampaolo, A and Mueller, TA and Santos, AD and Paganini, P and Quilain,
B and Ishizuka, T and Nakamura, T and Jang, JS and Learned, JG and Choi, K and Cao, S and Anthony, LHV and Martin, D and Scott, M and Sztuc, AA and Uchida, Y and Berardi, V and Catanesi, MG and Radicioni, E and Calabria,
NF and Machado, LN and Rosa, GD and Collazuol, G and Iacob, F and Lamoureux, M and Mattiazzi, M and Ludovici, L and Gonin, M and Pronost,
G and Fujisawa, C and Maekawa, Y and Nishimura, Y and Friend, M and Hasegawa, T and Ishida, T and Kobayashi, T and Jakkapu, M and Matsubara,
T and Nakadaira, T and Nakamura, K and Oyama, Y and Sakashita, K and Sekiguchi, T and Tsukamoto, T and Boschi, T and Lodovico, FD and Gao, J and Goldsack, A and Katori, T and Migenda, J and Taani, M and Xie, Z and Zsoldos, S and Kotsar, Y and Ozaki, H and Suzuki, AT and Takeuchi, Y and Yamamoto, S and Bronner, C and Feng, J and Kikawa, T and Mori, M and Nakaya, T and Wendell, RA and Yasutome, K and Jenkins, SJ and McCauley,
N and Mehta, P and Tsui, KM and Tarrant, A and Fukuda, Y and Itow, Y and Menjo, H and Ninomiya, K and Lagoda, J and Lakshmi, SM and Mandal, M and Mijakowski, P and Prabhu, YS and Zalipska, J and Jiang, MJJ and Jung,
CK and Wilking, MJ and Yanagisawa, C and Harada, M and Ishino, H and Ito,
S and Kitagawa, H and Koshio, Y and Ma, W and Nakanishi, F and Sakai, S and Barr, G and Barrow, D and Cook, L and Samani, S and Wark, D and Holin, A and Nova, F and Yang, JY and Malek, M and McElwee, JM and Stone, O and Thiesse,
MD and Thompson, LF and Okazawa, H and Kim, SB and Kwon, E and Seo, JW and Yu,
I and Ichikawa, AK and Nakamura, KD and Tairafune, S and Nishijima, K and Koshiba, M and Iwamoto, K and Nakagiri, K and Nakajima, Y and Shima, S and Taniuchi, N and Yokoyama, M and Martens, K and Perio, PD and Vagins, MR and Kuze, M and Izumiyama, S and Inomoto, M and Ishitsuka, M and Ito, H and Kinoshita, T and Ommura, Y and Shigeta, N and Shinoki, M and Suganuma,
T and Yamauchi, K and Martin, JF and Tanaka, HA and Towstego, T and Akutsu,
R and Gousy-Leblanc, V and Hartz, M and Konaka, A and Li, X and Prouse, NW and Chen, S and Xu, BD and Zhang, B and Posiadala-Zezula, M and Boyd, SB and Hadley, D and Nicholson, M and O'Flaherty, M and Richards, B and Ali, A and Jamieson, B and Marti, L and Minamino, A and Pintaudi, G and Sano, S and Suzuki, S and Wada, K},
Title = {Search for proton decay via $p\rightarrow μ^+K^0$ in 0.37
megaton-years exposure of Super-Kamiokande},
Year = {2022},
Month = {August},
Key = {fds375015}
}
@article{fds368064,
Author = {Troxel, MA and Lin, C and Park, A and Hirata, C and Mandelbaum, R and Jarvis, M and Choi, A and Givans, J and Higgins, M and Sanchez, B and Yamamoto, M and Awan, H and Chiang, J and Dore, O and Walter, CW and Zhang,
T and Cohen-Tanugi, J and Gawiser, E and Hearin, A and Heitmann, K and Ishak, M and Kovacs, E and Mao, Y-Y and Wood-Vasey, M and Collaboration,
TLSSTDES},
Title = {A Joint Roman Space Telescope and Rubin Observatory
Synthetic Wide-Field Imaging Survey},
Year = {2022},
Month = {September},
Key = {fds368064}
}
@article{fds375014,
Author = {Abe, K and Haga, Y and Hayato, Y and Hiraide, K and Ieki, K and Ikeda, M and Imaizumi, S and Iyogi, K and Kameda, J and Kanemura, Y and Kataoka, Y and Kato, Y and Kishimoto, Y and Miki, S and Mine, S and Miura, M and Mochizuki, T and Moriyama, S and Nagao, Y and Nakahata, M and Nakajima,
T and Nakano, Y and Nakayama, S and Okada, T and Okamoto, K and Orii, A and Sato, K and Sekiya, H and Shiozawa, M and Sonoda, Y and Suzuki, Y and Takeda, A and Takemoto, Y and Takenaka, A and Tanaka, H and Tasaka, S and Tomura, T and Ueno, K and Watanabe, S and Yano, T and Yokozawa, T and Han,
S and Irvine, T and Kajita, T and Kametani, I and Kaneyuki, K and Lee, KP and McLachlan, T and Okumura, K and Richard, E and Tashiro, T and Wang, R and Xia, J and Megias, GD and Bravo-Berguño, D and Labarga, L and Zaldivar,
B and Goldhaber, M and Blaszczyk, FDM and Gustafson, J and Kachulis, C and Kearns, E and Raaf, JL and Stone, JL and Sulak, LR and Sussman, S and Wan,
L and Wester, T and Pointon, BW and Bian, J and Carminati, G and Elnimr, M and Griskevich, NJ and Kropp, WR and Locke, S and Renshaw, A and Smy, MB and Sobel, HW and Takhistov, V and Weatherly, P and Ganezer, KS and Hartfiel, BL and Hill, J and Keig, WE and Hong, N and Kim, JY and Lim, IT and Park, RG and Akiri, T and Bodur, B and Himmel, A and Li, Z and O'Sullivan,
E and Scholberg, K and Walter, CW and Wongjirad, T and Bernard, L and Coffani, A and Drapier, O and Hedri, SE and Giampaolo, A and Imber, J and Mueller, TA and Paganini, P and Quilain, B and Ishizuka, T and Nakamura,
T and Jang, JS and Choi, K and Learned, JG and Matsuno, S and Smith, SN and Amey, J and Anthony, LHV and Litchfield, RP and Ma, WY and Marin, D and Sztuc, AA and Uchida, Y and Wascko, MO and Berardi, V and Catanesi, MG and Intonti, RA and Radicioni, E and Calabria, NF and Rosa, GD and Machado,
LN and Collazuol, G and Iacob, F and Lamoureux, M and Ospina, N and Ludovici, L and Gonin, M and Pronost, G and Maekawa, Y and Nishimura, Y and Cao, S and Friend, M and Hasegawa, T and Ishida, T and Ishii, T and Jakkapu, M and Kobayashi, T and Matsubara, T and Nakadaira, T and Nakamura, K and Oyama, Y and Sakashita, K and Sekiguchi, T and Tsukamoto, T and Boschi, T and Lodovico, FD and Migenda, J and Sedgwick,
SM and Taani, M and Zsoldos, S and Abe, KE and Hasegawa, M and Isobe, Y and Kotsar, Y and Miyabe, H and Ozaki, H and Shiozawa, T and Sugimoto, T and Suzuki, AT and Takeuchi, Y and Yamamoto, S and Ali, A and Ashida, Y and Bronner, C and Feng, J and Hayashino, T and Hiraki, T and Hirota, S and Huang, K and Jiang, M and Kikawa, T and Mori, M and Murakami, A and Nakamura, KE and Nakaya, T and Patel, ND and Suzuki, K and Takahashi, S and Tateishi, K and Wendell, RA and Yasutome, K and Fernandez, P and McCauley, N and Mehta, P and Pritchard, A and Tsui, KM and Fukuda, Y and Itow, Y and Menjo, H and Mitsuka, G and Murase, M and Muto, F and Niwa, T and Tsukada, TSM and Frankiewicz, K and Mijakowski, P and Hignight, J and Jiang, J and Jung, CK and Li, X and Palomino, JL and Santucci, G and Vilela, C and Wilking, MJ and Yanagisawa, C and Fukuda, D and Hagiwara,
K and Harada, M and Horai, T and Ishino, H and Ito, S and Kayano, T and Kibayashi, A and Kitagawa, H and Koshio, Y and Ma, W and Mori, T and Nagata, H and Piplani, N and Sakai, S and Sakuda, M and Takahira, Y and Xu,
C and Yamaguchi, R and Kuno, Y and Barr, G and Barrow, D and Cook, L and Goldsack, A and Samani, S and Simpson, C and Wark, D and Nova, F and Tacik,
R and Yang, JY and Cole, A and Jenkins, SJ and Malek, M and McElwee, JM and Stone, O and Thiesse, MD and Thompson, LF and Okazawa, H and Choi, Y and Kim, SB and Yu, I and Ichikawa, AK and Ito, K and Nishijima, K and Calland,
RG and Perio, PD and Martens, K and Murdoch, M and Vagins, MR and Koshiba,
M and Totsuka, Y and Iwamoto, K and Nakajima, Y and Ogawa, N and Suda, Y and Yokoyama, M and Hamabe, D and Izumiyama, S and Kuze, M and Okajima, Y and Tanaka, M and Yoshida, T and Inomoto, M and Ishitsuka, M and Ito, H and Matsumoto, R and Ohta, K and Shinoki, M and Martin, JF and Nantais, CM and Tanaka, HA and Towstego, T and Akutsu, R and Hartz, M and Konaka, A and Prouse, NW and Chen, S and Xu, BD and Zhang, Y and Berkman, S and Tobayama,
S and Connolly, K and Wilkes, RJ and Posiadala-Zezula, M and Hadley, D and Richards, B and Jamieson, B and Walker, J and Marti, L and Minamino, A and Pintaudi, G and Sano, S and Sasaki, R},
Title = {Neutron Tagging following Atmospheric Neutrino Events in a
Water Cherenkov Detector},
Year = {2022},
Month = {September},
Key = {fds375014}
}
@article{fds368063,
Author = {Collaboration, TS-K and Abe, K and Hayato, Y and Hiraide, K and Ieki, K and Ikeda, M and Kameda, J and Kanemura, Y and Kaneshima, R and Kashiwagi,
Y and Kataoka, Y and Miki, S and Mine, S and Miura, M and Moriyama, S and Nakano, Y and Nakahata, M and Nakayama, S and Noguchi, Y and Okamoto, K and Sato, K and Sekiya, H and Shiba, H and Shimizu, K and Shiozawa, M and Sonoda, Y and Suzuki, Y and Takeda, A and Takemoto, Y and Takenaka, A and Tanaka, H and Watanabe, S and Yano, T and Han, S and Kajita, T and Okumura,
K and Tashiro, T and Tomiya, T and Wang, X and Xia, J and Yoshida, S and Megias, GD and Fernandez, P and Labarga, L and Ospina, N and Zaldivar,
B and Pointon, BW and Kearns, E and Raaf, JL and Wan, L and Wester, T and Bian, J and Griskevich, NJ and Kropp, WR and Locke, S and Smy, MB and Sobel, HW and Takhistov, V and Yankelevich, A and Hill, J and Park, RG and Bodur, B and Scholberg, K and Walter, CW and Bernard, L and Coffani, A and Drapier, O and Hedri, SE and Giampaolo, A and Mueller, TA and Santos,
AD and Paganini, P and Quilain, B and Ishizuka, T and Nakamura, T and Jang,
JS and Learned, JG and Choi, K and Cao, S and Anthony, LHV and Martin, D and Scott, M and Sztuc, AA and Uchida, Y and Berardi, V and Catanesi, MG and Radicioni, E and Calabria, NF and Machado, LN and Rosa, GD and Collazuol, G and Iacob, F and Lamoureux, M and Mattiazzi, M and Ludovici, L and Gonin, M and Pronost, G and Fujisawa, C and Maekawa, Y and Nishimura, Y and Friend, M and Hasegawa, T and Ishida, T and Kobayashi,
T and Jakkapu, M and Matsubara, T and Nakadaira, T and Nakamura, K and Oyama, Y and Sakashita, K and Sekiguchi, T and Tsukamoto, T and Boschi,
T and Lodovico, FD and Gao, J and Goldsack, A and Katori, T and Migenda, J and Taani, M and Zsoldos, S and Kotsar, Y and Ozaki, H and Suzuki, AT and Takeuchi, Y and Bronner, C and Feng, J and Kikawa, T and Mori, M and Nakaya, T and Wendell, RA and Yasutome, K and Jenkins, SJ and McCauley,
N and Mehta, P and Tsui, KM and Fukuda, Y and Itow, Y and Menjo, H and Ninomiya, K and Lagoda, J and Lakshmi, SM and Mandal, M and Mijakowski,
P and Prabhu, YS and Zalipska, J and Jia, M and Jiang, J and Jung, CK and Wilking, MJ and Yanagisawa, C and Harada, M and Ishino, H and Ito, S and Kitagawa, H and Koshio, Y and Nakanishi, F and Sakai, S and Barr, G and Barrow, D and Cook, L and Samani, S and Wark, D and Nova, F and Yang, JY and Malek, M and McElwee, JM and Stone, O and Thiesse, MD and Thompson, LF and Okazawa, H and Kim, SB and Seo, JW and Yu, I and Ichikawa, AK and Nakamura,
KD and Tairafune, S and Nishijima, K and Iwamoto, K and Nakagiri, K and Nakajima, Y and Taniuchi, N and Yokoyama, M and Martens, K and Perio,
PD and Vagins, MR and Kuze, M and Izumiyama, S and Inomoto, M and Ishitsuka, M and Ito, H and Kinoshita, T and Matsumoto, R and Ommura, Y and Shigeta, N and Shinoki, M and Suganuma, T and Yamauchi, K and Martin,
JF and Tanaka, HA and Towstego, T and Akutsu, R and Gousy-Leblanc, V and Hartz, M and Konaka, A and Prouse, NW and Chen, S and Xu, BD and Zhang, B and Posiadala-Zezula, M and Hadley, D and Nicholson, M and O'Flaherty, M and Richards, B and Ali, A and Jamieson, B and Marti, L and Minamino, A and Pintaudi, G and Sano, S and Suzuki, S and Wada, K},
Title = {Search for Cosmic-ray Boosted Sub-GeV Dark Matter using
Recoil Protons at Super-Kamiokande},
Year = {2022},
Month = {September},
Key = {fds368063}
}
@article{fds375013,
Author = {Okamoto, K and Abe, K and Hayato, Y and Hiraide, K and Hosokawa, K and Ieki, K and Ikeda, M and Kameda, J and Kanemura, Y and Kaneshima, Y and Kataoka, Y and Kashiwagi, Y and Miki, S and Mine, S and Miura, M and Moriyama, S and Nagao, Y and Nakahata, M and Nakano, Y and Nakayama, S and Noguchi, Y and Sato, K and Sekiya, H and Shimizu, K and Shiozawa, M and Shiba, H and Sonoda, Y and Suzuki, Y and Takeda, A and Takemoto, Y and Takenaka, A and Tanaka, H and Watanabe, S and Yano, T and Han, S and Kajita, T and Okumura, K and Tashiro, T and Tomiya, T and Wang, X and Xia,
J and Yoshida, S and Megias, GD and Fernandez, P and Labarga, L and Ospina,
N and Zaldivar, B and Pointon, BW and Kearns, E and Raaf, JL and Wan, L and Wester, T and Bian, J and Griskevich, NJ and Kropp, WR and Locke, S and Smy, MB and Sobel, HW and Takhistov, V and Yankelevich, A and Hill, J and Kim, JY and Lee, SH and Lim, IT and Moon, DH and Park, RG and Bodur, B and Scholberg, K and Walter, CW and Beauchene, A and Bernard, L and Coffani,
A and Drapier, O and Hedri, SE and Giampaolo, A and Mueller, TA and Santos,
AD and Paganini, P and Quilain, B and Ishizuka, T and Nakamura, T and Jang,
JS and Learned, JG and Choi, K and Cao, S and Anthony, LHV and Martin, D and Scott, M and Sztuc, AA and Uchida, Y and Berardi, V and Catanesi, MG and Radicioni, E and Calabria, NF and Machado, LN and Rosa, GD and Collazuol, G and Iacob, F and Lamoureux, M and Mattiazzi, M and Ludovici, L and Gonin, M and Pronost, G and Fujisawa, C and Maekawa, Y and Nishimura, Y and Friend, M and Hasegawa, T and Ishida, T and Kobayashi,
T and Jakkapu, M and Matsubara, T and Nakadaira, T and Nakamura, K and Oyama, Y and Sakashita, K and Sekiguchi, T and Tsukamoto, T and Bhuiyan,
N and Boschi, T and Burton, GT and Lodovico, FD and Gao, J and Goldsack, A and Katori, T and Migenda, J and Taani, M and Xie, Z and Zsoldos, S and Kotsar,
Y and Ozaki, H and Suzuki, AT and Takeuchi, Y and Yamamoto, S and Bronner,
C and Feng, J and Kikawa, T and Mori, M and Nakaya, T and Wendell, RA and Yasutome, K and Jenkins, SJ and McCauley, N and Mehta, P and Tarrant, A and Tsui, KM and Fukuda, Y and Itow, Y and Menjo, H and Ninomiya, K and Lagoda,
J and Lakshmi, SM and Mandal, M and Mijakowski, P and Prabhu, YS and Zalipska, J and Jia, M and Jiang, J and Jung, CK and Vilela, C and Wilking,
MJ and Yanagisawa, C and Harada, M and Ishino, H and Ito, S and Kitagawa,
H and Koshio, Y and Ma, W and Nakanishi, F and Piplani, N and Sakai, S and Barr, G and Barrow, D and Cook, L and Samani, S and Wark, D and Holin, A and Nova, F and Yang, JY and Fannon, JEP and Malek, M and McElwee, JM and Stone, O and Thiesse, MD and Thompson, LF and Okazawa, H and Kim, SB and Kwon, E and Seo, JW and Yu, I and Ichikawa, AK and Nakamura, KD and Tairafune, S and Nishijima, K and Koshiba, M and Iwamoto, K and Nakagiri, K and Nakajima, Y and Shima, S and Taniuchi, N and Yokoyama,
M and Martens, K and Perio, PD and Vagins, MR and Kuze, M and Izumiyama, S and Inomoto, M and Ishitsuka, M and Ito, H and Kinoshita, T and Matsumoto,
R and Ommura, Y and Shigeta, N and Shinoki, M and Suganuma, T and Yamauchi,
K and Martin, JF and Tanaka, HA and Towstego, T and Akutsu, R and Gaur, R and Gousy-Leblanc, V and Hartz, M and Konaka, A and Li, X and Prouse, NW and Chen, S and Xu, BD and Zhang, B and Posiadala-Zezula, M and Boyd, SB and Hadley, D and Nicholson, M and O'Flaherty, M and Richards, B and Ali, A and Jamieson, B and Walker, J and Marti, L and Minamino, A and Pintaudi, G and Sano, S and Sasaki, R and Suzuki, S and Wada, K},
Title = {Searching for neutrinos from solar flares across solar
cycles 23 and 24 with the Super-Kamiokande
detector},
Year = {2022},
Month = {October},
Key = {fds375013}
}
@article{fds368062,
Author = {Guo, Z and Walter, CW and Lage, C and Lupton, RH and Collaboration,
TLSSTDES},
Title = {Fringing Analysis and Simulation for the Vera C. Rubin
Observatory's Legacy Survey of Space and
Time},
Year = {2022},
Month = {November},
Key = {fds368062}
}
@article{fds375012,
Author = {Collaboration, S-K and Shinoki, M and Abe, K and Hayato, Y and Hiraide,
K and Hosokawa, K and Ieki, K and Ikeda, M and Kameda, J and Kanemura, Y and Kaneshima, R and Kashiwagi, Y and Kataoka, Y and Miki, S and Mine, S and Miura, M and Moriyama, S and Nakano, Y and Nakahata, M and Nakayama, S and Noguchi, Y and Okamoto, K and Sato, K and Sekiya, H and Shiba, H and Shimizu, K and Shiozawa, M and Sonoda, Y and Suzuki, Y and Takeda, A and Takemoto, Y and Takenaka, A and Tanaka, H and Watanabe, S and Yano, T and Han, S and Kajita, T and Okumura, K and Tashiro, T and Tomiya, T and Wang,
X and Yoshida, S and Megias, GD and Fernandez, P and Labarga, L and Ospina,
N and Zaldivar, B and Pointon, BW and Kearns, E and Raaf, JL and Wan, L and Wester, T and Bian, J and Griskevich, NJ and Kropp, WR and Locke, S and Smy, MB and Sobel, HW and Takhistov, V and Yankelevich, A and Hill, J and Lee, SH and Moon, DH and Park, RG and Bodur, B and Scholberg, K and Walter,
CW and Beauchêne, A and Bernard, L and Coffani, A and Drapier, O and Hedri, SE and Giampaolo, A and Mueller, TA and Santos, AD and Paganini,
P and Quilain, B and Ishizuka, T and Nakamura, T and Jang, JS and Learned,
JG and Choi, K and Cao, S and Anthony, LHV and Martin, D and Scott, M and Sztuc, AA and Uchida, Y and Berardi, V and Catanesi, MG and Radicioni,
E and Calabria, NF and Langella, A and Machado, LN and Rosa, GD and Collazuol, G and Iacob, F and Lamoureux, M and Mattiazzi, M and Ludovici, L and Gonin, M and Pronost, G and Fujisawa, C and Maekawa, Y and Nishimura, Y and Akutsu, R and Friend, M and Hasegawa, T and Ishida, T and Kobayashi, T and Jakkapu, M and Matsubara, T and Nakadaira, T and Nakamura, K and Oyama, Y and Sakashita, K and Sekiguchi, T and Tsukamoto, T and Bhuiyan, N and Boschi, T and Burton, GT and Lodovico,
FD and Gao, J and Goldsack, A and Katori, T and Migenda, J and Taani, M and Xie, Z and Zsoldos, S and Kotsar, Y and Ozaki, H and Suzuki, AT and Takeuchi, Y and Bronner, C and Feng, J and Kikawa, T and Mori, M and Nakaya, T and Wendell, RA and Yasutome, K and Jenkins, SJ and McCauley,
N and Mehta, P and Tarrant, A and Tsui, KM and Fukuda, Y and Itow, Y and Menjo, H and Ninomiya, K and Lagoda, J and Lakshmi, SM and Mandal, M and Mijakowski, P and Prabhu, YS and Zalipska, J and Jia, M and Jiang, J and Jung, CK and Wilking, MJ and Yanagisawa, C and Harada, M and Ishino, H and Ito, S and Kitagawa, H and Koshio, Y and Nakanishi, F and Sakai, S and Barr, G and Barrow, D and Cook, L and Samani, S and Wark, D and Holin, A and Nova, F and Yang, JY and Yang, BS and Yoo, J and Fannon, JEP and Kneale, L and Malek, M and McElwee, JM and Stone, O and Thiesse, MD and Thompson, LF and Okazawa, H and Kim, SB and Kwon, E and Seo, JW and Yu, I and Ichikawa, AK and Nakamura, KD and Tairafune, S and Nishijima, K and Koshiba, M and Iwamoto, K and Nakagiri, K and Nakajima, Y and Shima, S and Taniuchi, N and Yokoyama, M and Martens, K and Perio, PD and Vagins, MR and Xia, J and Kuze, M and Izumiyama, S and Inomoto, M and Ishitsuka, M and Ito, H and Kinoshita, T and Matsumoto, R and Ommura, Y and Shigeta, N and Suganuma,
T and Yamauchi, K and Martin, JF and Tanaka, HA and Towstego, T and Gaur,
R and Gousy-Leblanc, V and Hartz, M and Konaka, A and Li, X and Prouse, NW and Chen, S and Xu, BD and Zhang, B and Posiadala-Zezula, M and Boyd, SB and Hadley, D and Nicholson, M and O'Flaherty, M and Richards, B and Ali, A and Jamieson, B and Marti, L and Minamino, A and Pintaudi, G and Sano, S and Suzuki, S and Wada, K},
Title = {Measurement of the cosmogenic neutron yield in
Super-Kamiokande with gadolinium loaded water},
Year = {2022},
Month = {December},
Key = {fds375012}
}
@article{fds375010,
Author = {Hirata, CM and Yamamoto, M and Laliotis, K and Macbeth, E and Troxel,
MA and Zhang, T and Cao, K and Choi, A and Givans, J and Heitmann, K and Ishak, M and Jarvis, M and Kovacs, E and Long, H and Mandelbaum, R and Park, A and Porredon, A and Walter, CW and Wood-Vasey,
WM},
Title = {Simulating image coaddition with the Nancy Grace Roman Space
Telescope: I. Simulation methodology and general
results},
Year = {2023},
Month = {March},
Key = {fds375010}
}
@article{fds375011,
Author = {Yamamoto, M and Laliotis, K and Macbeth, E and Zhang, T and Hirata, CM and Troxel, MA and Cao, K and Choi, A and Givans, J and Heitmann, K and Ishak,
M and Jarvis, M and Kovacs, E and Long, H and Mandelbaum, R and Park, A and Porredon, A and Walter, CW and Wood-Vasey, WM},
Title = {Simulating image coaddition with the Nancy Grace Roman Space
Telescope: II. Analysis of the simulated images and
implications for weak lensing},
Volume = {528},
Number = {4},
Pages = {6680-6705},
Year = {2023},
Month = {March},
url = {http://dx.doi.org/10.1093/mnras/stae177},
Abstract = {One challenge for applying current weak lensing analysis
tools to the Nancy Grace Roman Space Telescope is that
individual images will be undersampled. Our companion paper
presented an initial application of IMCOM - an algorithm
that builds an optimal mapping from input to output pixels
to reconstruct a fully sampled combined image - on the Roman
image simulations. In this paper, we measure the output
noise power spectra, identify the sources of the major
features in the power spectra, and show that simple analytic
models that ignore sampling effects underestimate the power
spectra of the coadded noise images. We compute the moments
of both idealized injected stars and fully simulated stars
in the coadded images, and their one- and two-point
statistics. We show that the idealized injected stars have
root-mean-square ellipticity errors (1-6) × 10−4 per
component depending on the band; the correlation functions
are ≥2 orders of magnitude below requirements, indicating
that the image combination step itself is using a small
fraction of the overall Roman second moment error budget,
although the fourth moments are larger and warrant further
investigation. The stars in the simulated sky images, which
include blending and chromaticity effects, have correlation
functions near the requirement level (and below the
requirement level in a wide-band image constructed by
stacking all four filters). We evaluate the noise-induced
biases in the ellipticities of injected stars, and explain
the resulting trends with an analytical model. We conclude
by enumerating the next steps in developing an image
coaddition pipeline for Roman.},
Doi = {10.1093/mnras/stae177},
Key = {fds375011}
}
@article{fds375136,
Author = {Harada, M and Abe, K and Bronner, C and Hayato, Y and Hiraide, K and Hosokawa, K and Ieki, K and Ikeda, M and Kameda, J and Kanemura, Y and Kaneshima, R and Kashiwagi, Y and Kataoka, Y and Miki, S and Mine, S and Miura, M and Moriyama, S and Nakano, Y and Nakahata, M and Nakayama, S and Noguchi, Y and Okamoto, K and Sato, K and Sekiya, H and Shiba, H and Shimizu, K and Shiozawa, M and Sonoda, Y and Suzuki, Y and Takeda, A and Takemoto, Y and Takenaka, A and Tanaka, H and Watanabe, S and Yano, T and Han, S and Kajita, T and Okumura, K and Tashiro, T and Tomiya, T and Wang,
X and Yoshida, S and Megias, GD and Fernandez, P and Labarga, L and Ospina,
N and Zaldivar, B and Pointon, BW and Kearns, E and Raaf, JL and Wan, L and Wester, T and Bian, J and Griskevich, NJ and Locke, S and Smy, MB and Sobel, HW and Takhistov, V and Yankelevich, A and Hill, J and Lee, SH and Moon, DH and Park, RG and Bodur, B and Scholberg, K and Walter, CW and Beauchene, A and Drapier, O and Giampaolo, A and Mueller, TA and Santos,
AD and Paganini, P and Quilain, B and Ishizuka, T and Nakamura, T and Jang,
JS and Learned, JG and Choi, K and Iovine, N and Cao, S and Anthony, LHV and Martin, D and Scott, M and Sztuc, AA and Uchida, Y and Berardi, V and Catanesi, MG and Radicioni, E and Calabria, NF and Langella, A and Machado, LN and Rosa, GD and Collazuol, G and Iacob, F and Lamoureux, M and Mattiazzi, M and Ludovici, L and Gonin, M and Pronost, G and Fujisawa,
C and Maekawa, Y and Nishimura, Y and Okazaki, R and Akutsu, R and Friend,
M and Hasegawa, T and Ishida, T and Kobayashi, T and Jakkapu, M and Matsubara, T and Nakadaira, T and Nakamura, K and Oyama, Y and Sakashita, K and Sekiguchi, T and Tsukamoto, T and Bhuiyan, N and Burton, GT and Lodovico, FD and Gao, J and Goldsack, A and Katori, T and Migenda, J and Xie, Z and Zsoldos, S and Kotsar, Y and Ozaki, H and Suzuki,
AT and Takagi, Y and Takeuchi, Y and Feng, J and Feng, L and Hu, JR and Hu, Z and Kikawa, T and Mori, M and Nakaya, T and Wendell, RA and Yasutome, K and Jenkins, SJ and McCauley, N and Mehta, P and Tarrant, A and Fukuda, Y and Itow, Y and Menjo, H and Ninomiya, K and Lagoda, J and Lakshmi, SM and Mandal, M and Mijakowski, P and Prabhu, YS and Zalipska, J and Jia, M and Jiang, J and Jung, CK and Wilking, MJ and Yanagisawa, C and Hino, Y and Ishino, H and Kitagawa, H and Koshio, Y and Nakanishi, F and Sakai, S and Tada, T and Tano, T and Barr, G and Barrow, D and Cook, L and Samani, S and Wark, D and Holin, A and Nova, F and Yang, BS and Yang, JY and Yoo, J and Fannon, JEP and Kneale, L and Malek, M and McElwee, JM and Thiesse, MD and Thompson, LF and Wilson, ST and Okazawa, H and Kim, SB and Kwon, E and Seo,
JW and Yu, I and Ichikawa, AK and Nakamura, KD and Tairafune, S and Nishijima, K and Nakagiri, K and Nakajima, Y and Shima, S and Taniuchi,
N and Watanabe, E and Yokoyama, M and Perio, PD and Martens, K and Tsui,
KM and Vagins, MR and Xia, J and Kuze, M and Izumiyama, S and Matsumoto, R and Ishitsuka, M and Ito, H and Kinoshita, T and Ommura, Y and Shigeta, N and Shinoki, M and Suganuma, T and Yamauchi, K and Martin, JF and Tanaka,
HA and Towstego, T and Gaur, R and Gousy-Leblanc, V and Hartz, M and Konaka, A and Li, X and Prouse, NW and Chen, S and Xu, BD and Zhang, B and Posiadala-Zezula, M and Boyd, SB and Edwards, R and Hadley, D and Nicholson, M and Flaherty, MO and Richards, B and Ali, A and Jamieson,
B and Marti, L and Minamino, A and Pintaudi, G and Sano, S and Suzuki, S and Wada, K},
Title = {Search for astrophysical electron antineutrinos in
Super-Kamiokande with 0.01wt% gadolinium-loaded
water},
Year = {2023},
Month = {May},
Key = {fds375136}
}
@article{fds375009,
Author = {Nicola, A and Hadzhiyska, B and Findlay, N and García-García, C and Alonso, D and Slosar, A and Guo, Z and Kokron, N and Angulo, R and Aviles,
A and Blazek, J and Dunkley, J and Jain, B and Pellejero, M and Sullivan,
J and Walter, CW and Zennaro, M},
Title = {Galaxy bias in the era of LSST: perturbative bias
expansions},
Year = {2023},
Month = {July},
Key = {fds375009}
}
@article{fds375008,
Author = {Abe, K and Bronner, C and Hayato, Y and Hiraide, K and Hosokawa, K and Ieki, K and Ikeda, M and Kameda, J and Kanemura, Y and Kaneshima, R and Kashiwagi, Y and Kataoka, Y and Miki, S and Mine, S and Miura, M and Moriyama, S and Nakano, Y and Nakahata, M and Nakayama, S and Noguchi,
Y and Sato, K and Sekiya, H and Shiba, H and Shimizu, K and Shiozawa, M and Sonoda, Y and Suzuki, Y and Takeda, A and Takemoto, Y and Tanaka, H and Yano, T and Han, S and Kajita, T and Okumura, K and Tashiro, T and Tomiya,
T and Wang, X and Yoshida, S and Fernandez, P and Labarga, L and Ospina, N and Zaldivar, B and Pointon, BW and Kearns, E and Raaf, JL and Wan, L and Wester, T and Bian, J and Griskevich, NJ and Locke, S and Smy, MB and Sobel, HW and Takhistov, V and Yankelevich, A and Hill, J and Lee, SH and Moon, DH and Park, RG and Jang, MC and Bodur, B and Scholberg, K and Walter, CW and Beauchene, A and Drapier, O and Giampaolo, A and Mueller,
TA and Santos, AD and Paganini, P and Quilain, B and Nakamura, T and Jang,
JS and Machado, LN and Learned, JG and Choi, K and Iovine, N and Cao, S and Anthony, LHV and Martin, D and Prouse, NW and Scott, M and Sztuc, AA and Uchida, Y and Berardi, V and Catanesi, MG and Radicioni, E and Calabria,
NF and Langella, A and Rosa, GD and Collazuol, G and Iacob, F and Mattiazzi, M and Ludovici, L and Gonin, M and Pronost, G and Fujisawa,
C and Maekawa, Y and Nishimura, Y and Okazaki, R and Akutsu, R and Friend,
M and Hasegawa, T and Ishida, T and Kobayashi, T and Jakkapu, M and Matsubara, T and Nakadaira, T and Nakamura, K and Oyama, Y and Sakashita, K and Sekiguchi, T and Tsukamoto, T and Bhuiyan, N and Burton, GT and Lodovico, FD and Gao, J and Goldsack, A and Katori, T and Migenda, J and Xie, Z and Ramsden, RM and Zsoldos, S and Suzuki, AT and Takagi, Y and Zhong, H and Takeuchi, Y and Feng, J and Feng, L and Hu, JR and Hu, Z and Kikawa, T and Mori, M and Kawaue, M and Nakaya, T and Wendell,
RA and Yasutome, K and Jenkins, SJ and McCauley, N and Mehta, P and Tarant,
A and Fukuda, Y and Itow, Y and Menjo, H and Ninomiya, K and Yoshioka, Y and Lagoda, J and Lakshmi, SM and Mandal, M and Mijakowski, P and Prabhu,
YS and Zalipska, J and Jia, M and Jiang, J and Jung, CK and Wilking, MJ and Yanagisawa, C and Shi, W and Harada, M and Hino, Y and Ishino, H and Koshio, Y and Nakanishi, F and Sakai, S and Tada, T and Tano, T and Ishizuka, T and Barr, G and Barrow, D and Cook, L and Samani, S and Wark,
D and Holin, A and Nova, F and Yang, BS and Yang, JY and Yoo, J and Jung, S and Fannon, JEP and Kneale, L and Malek, M and McElwee, JM and Thiesse, MD and Thompson, LF and Wilson, ST and Okazawa, H and Kim, SB and Kwon, E and Seo,
JW and Yu, I and Ichikawa, AK and Nakamura, KD and Tairafune, S and Nishijima, K and Eguchi, A and Nakagiri, K and Nakajima, Y and Shima, S and Taniuchi, N and Watanabe, E and Yokoyama, M and Perio, PD and Fujita, S and Martens, K and Tsui, KM and Vagins, MR and Xia, J and Izumiyama, S and Kuze, M and Matsumoto, R and Ishitsuka, M and Ito, H and Ommura, Y and Shigeta, N and Shinoki, M and Yamauchi, K and Yoshida, T and Gaur, R and Gousy-Leblanc, V and Hartz, M and Konaka, A and Li, X and Chen, S and Xu,
BD and Zhang, B and Posiadala-Zezula, M and Boyd, SB and Edwards, R and Hadley, D and Nicholson, M and Flaherty, MO and Richards, B and Ali, A and Jamieson, B and Amanai, S and Marti, L and Minamino, A and Suzuki,
S},
Title = {Search for Periodic Time Variations of the Solar $^8$B
Neutrino Flux Between 1996 and 2018 in Super-Kamiokande},
Year = {2023},
Month = {November},
Key = {fds375008}
}
@article{fds375007,
Author = {Sakai, S and Abe, K and Bronner, C and Hayato, Y and Hiraide, K and Hosokawa, K and Ieki, K and Ikeda, M and Kameda, J and Kanemura, Y and Kaneshima, R and Kashiwagi, Y and Kataoka, Y and Miki, S and Mine, S and Miura, M and Moriyama, S and Nakano, Y and Nakahata, M and Nakayama, S and Noguchi, Y and Sato, K and Sekiya, H and Shiba, H and Shimizu, K and Shiozawa, M and Sonoda, Y and Suzuki, Y and Takeda, A and Takemoto, Y and Tanaka, H and Yano, T and Han, S and Kajita, T and Okumura, K and Tashiro,
T and Tomiya, T and Wang, X and Yoshida, S and Fernandez, P and Labarga, L and Ospina, N and Zaldivar, B and Pointon, BW and Kearns, E and Raaf, JL and Wan, L and Wester, T and Bian, J and Griskevich, NJ and Locke, S and Smy,
MB and Sobel, HW and Takhistov, V and Yankelevich, A and Hill, J and Jang,
MC and Lee, SH and Moon, DH and Park, RG and Bodur, B and Scholberg, K and Walter, CW and Beauchene, A and Drapier, O and Giampaolo, A and Mueller,
TA and Santos, AD and Paganini, P and Quilain, B and Nakamura, T and Jang,
JS and Machado, LN and Learned, JG and Choi, K and Iovine, N and Cao, S and Anthony, LHV and Martin, D and Prouse, NW and Scott, M and Sztuc, AA and Uchida, Y and Berardi, V and Calabria, NF and Catanesi, MG and Radicioni, E and Langella, A and Rosa, GD and Collazuol, G and Iacob, F and Mattiazzi, M and Ludovici, L and Gonin, M and Pronost, G and Fujisawa,
C and Maekawa, Y and Nishimura, Y and Okazaki, R and Akutsu, R and Friend,
M and Hasegawa, T and Ishida, T and Kobayashi, T and Jakkapu, M and Matsubara, T and Nakadaira, T and Nakamura, K and Oyama, Y and Sakashita, K and Sekiguchi, T and Tsukamoto, T and Bhuiyan, N and Burton, GT and Lodovico, FD and Gao, J and Goldsack, A and Katori, T and Migenda, J and Ramsden, RM and Xie, Z and Zsoldos, S and Suzuki, AT and Takagi, Y and Zhong, H and Takeuchi, Y and Feng, J and Feng, L and Hu, JR and Hu, Z and Kawaue, M and Kikawa, T and Mori, M and Nakaya, T and Wendell,
RA and Yasutome, K and Jenkins, SJ and McCauley, N and Mehta, P and Tarant,
A and Fukuda, Y and Itow, Y and Menjo, H and Ninomiya, K and Yoshioka, Y and Lagoda, J and Lakshmi, SM and Mandal, M and Mijakowski, P and Prabhu,
YS and Zalipska, J and Jia, M and Jiang, J and Jung, CK and Shi, W and Wilking, MJ and Yanagisawa, C and Harada, M and Hino, Y and Ishino, H and Koshio, Y and Nakanishi, F and Tada, T and Tano, T and Ishizuka, T and Barr, G and Barrow, D and Cook, L and Samani, S and Wark, D and Holin, A and Nova, F and Jung, S and Yang, BS and Yang, JY and Yoo, J and Fannon, JEP and Kneale, L and Malek, M and McElwee, JM and Thiesse, MD and Thompson, LF and Wilson, ST and Okazawa, H and Kim, SB and Kwon, E and Seo, JW and Yu, I and Ichikawa, AK and Nakamura, KD and Tairafune, S and Nishijima, K and Eguchi, A and Nakagiri, K and Nakajima, Y and Shima, S and Taniuchi, N and Watanabe, E and Yokoyama, M and Perio, PD and Fujita, S and Martens, K and Tsui, KM and Vagins, MR and Xia, J and Izumiyama, S and Kuze, M and Matsumoto, R and Ishitsuka, M and Ito, H and Ommura, Y and Shigeta, N and Shinoki, M and Yamauchi, K and Yoshida, T and Gaur, R and Gousy-Leblanc,
V and Hartz, M and Konaka, A and Li, X and Chen, S and Xu, BD and Zhang, B and Posiadala-Zezula, M and Boyd, SB and Edwards, R and Hadley, D and Nicholson, M and O'Flaherty, M and Richards, B and Ali, A and Jamieson,
B and Amanai, S and Marti, L and Minamino, A and Suzuki,
S},
Title = {Measurement of the neutrino-oxygen neutral-current
quasielastic cross section using atmospheric neutrinos in
the SK-Gd experiment},
Year = {2023},
Month = {November},
Key = {fds375007}
}
@article{fds375006,
Author = {Collaboration, S-K and Wester, T and Abe, K and Bronner, C and Hayato,
Y and Hiraide, K and Hosokawa, K and Ieki, K and Ikeda, M and Kameda, J and Kanemura, Y and Kaneshima, R and Kashiwagi, Y and Kataoka, Y and Miki,
S and Mine, S and Miura, M and Moriyama, S and Nakano, Y and Nakahata, M and Nakayama, S and Noguchi, Y and Sato, K and Sekiya, H and Shiba, H and Shimizu, K and Shiozawa, M and Sonoda, Y and Suzuki, Y and Takeda, A and Takemoto, Y and Tanaka, H and Yano, T and Han, S and Kajita, T and Okumura,
K and Tashiro, T and Tomiya, T and Wang, X and Yoshida, S and Fernandez, P and Labarga, L and Ospina, N and Zaldivar, B and Pointon, BW and Kearns, E and Raaf, JL and Wan, L and Bian, J and Griskevich, NJ and Locke, S and Smy,
MB and Sobel, HW and Takhistov, V and Yankelevich, A and Hill, J and Lee,
SH and Moon, DH and Park, RG and Bodur, B and Scholberg, K and Walter, CW and Beauchene, A and Drapier, O and Giampaolo, A and Mueller, TA and Santos,
AD and Paganini, P and Quilain, B and Nakamura, T and Jang, JS and Machado,
LN and Learned, JG and Choi, K and Iovine, N and Cao, S and Anthony, LHV and Martin, D and Prouse, NW and Scott, M and Sztuc, AA and Uchida, Y and Berardi, V and Catanesi, MG and Radicioni, E and Calabria, NF and Langella, A and Rosa, GD and Collazuol, G and Iacob, F and Mattiazzi, M and Ludovici, L and Gonin, M and Pronost, G and Fujisawa, C and Maekawa, Y and Nishimura, Y and Okazaki, R and Akutsu, R and Friend, M and Hasegawa, T and Ishida, T and Kobayashi, T and Jakkapu, M and Matsubara, T and Nakadaira, T and Nakamura, K and Oyama, Y and Sakashita, K and Sekiguchi, T and Tsukamoto, T and Bhuiyan, N and Burton, GT and Lodovico, FD and Gao, J and Goldsack, A and Katori, T and Migenda, J and Ramsden, R and Xie, Z and Zsoldos, S and Suzuki, AT and Takagi, Y and Takeuchi, Y and Zhong, H and Feng, J and Feng, L and Hu, JR and Hu, Z and Kawaue, M and Kikawa, T and Mori, M and Nakaya, T and Wendell, RA and Yasutome, K and Jenkins, SJ and McCauley, N and Mehta, P and Tarrant, A and Fukuda, Y and Itow, Y and Menjo, H and Ninomiya, K and Lagoda, J and Lakshmi, SM and Mandal, M and Mijakowski, P and Prabhu, YS and Zalipska,
J and Jia, M and Jiang, J and Jung, CK and Shi, W and Wilking, MJ and Yanagisawa, C and Harada, M and Hino, Y and Ishino, H and Koshio, Y and Nakanishi, F and Sakai, S and Tada, T and Tano, T and Ishizuka, T and Barr,
G and Barrow, D and Cook, L and Holin, A and Nova, F and Samani, S and Wark,
D and Jung, S and Yang, BS and Yang, JY and Yoo, J and Fannon, JEP and Kneale,
L and Malek, M and McElwee, JM and Thiesse, MD and Thompson, LF and Wilson,
ST and Okazawa, H and Kim, SB and Kwon, E and Seo, JW and Yu, I and Ichikawa,
AK and Nakamura, KD and Tairafune, S and Nishijima, K and Koshiba, M and Eguchi, A and Nakagiri, K and Nakajima, Y and Shima, S and Taniuchi, N and Watanabe, E and Yokoyama, M and Perio, PD and Fujita, S and Martens, K and Tsui, KM and Vagins, MR and Xia, J and Izumiyama, S and Kuze, M and Matsumoto, R and Ishitsuka, M and Ito, H and Ommura, Y and Shigeta, N and Shinoki, M and Yamauchi, K and Yoshida, T and Gaur, R and Gousy-Leblanc,
V and Hartz, M and Konaka, A and Li, X and Chen, S and Xu, BD and Zhang, B and Posiadala-Zezula, M and Boyd, SB and Edwards, R and Hadley, D and Nicholson, M and O'Flaherty, M and Richards, B and Ali, A and Jamieson,
B and Amanai, S and Marti, L and Minamino, A and Suzuki,
S},
Title = {Atmospheric neutrino oscillation analysis with neutron
tagging and an expanded fiducial volume in Super-Kamiokande
I-V},
Year = {2023},
Month = {November},
Key = {fds375006}
}
@article{fds375005,
Author = {Collaboration, S-K and Abe, K and Bronner, C and Hayato, Y and Hiraide,
K and Hosokawa, K and Ieki, K and Ikeda, M and Imaizumi, S and Iyogi, K and Kameda, J and Kanemura, Y and Kaneshima, R and Kashiwagi, Y and Kataoka,
Y and Kato, Y and Kishimoto, Y and Miki, S and Mine, S and Miura, M and Mochizuki, T and Moriyama, S and Nagao, Y and Nakahata, M and Nakano, Y and Nakayama, S and Noguchi, Y and Okada, T and Okamoto, K and Orii, A and Sato, K and Sekiya, H and Shiba, H and Shimizu, K and Shiozawa, M and Sonoda, Y and Suzuki, Y and Takeda, A and Takemoto, Y and Takenaka, A and Tanaka, H and Watanabe, S and Yano, T and Han, S and Kajita, T and Okumura,
K and Tashiro, T and Tomiya, T and Wang, R and Wang, X and Yoshida, S and Bravo-Berguno, D and Fernandez, P and Labarga, L and Ospina, N and Zaldivar, B and Pointon, BW and Blaszczyk, FDM and Kachulis, C and Kearns, E and Raaf, JL and Stone, JL and Wan, L and Wester, T and Bian, J and Griskevich, NJ and Kropp, WR and Locke, S and Smy, MB and Sobel, HW and Takhistov, V and Weatherly, P and Yankelevich, A and Ganezer, KS and Hill, J and Jang, MC and Kim, JY and Lee, S and Lim, IT and Moon, DH and Park,
RG and Bodur, B and Scholberg, K and Walter, CW and Beauchene, A and Bernard, L and Coffani, A and Drapier, O and Hedri, SE and Giampaolo, A and Imber, J and Mueller, TA and Paganini, P and Rogly, R and Quilain, B and Santos, A and Nakamura, T and Jang, JS and Machado, LN and Learned, JG and Matsuno, S and Iovine, N and Choi, K and Cao, S and Anthony, LHV and Litchfield, RP and Prouse, N and Marin, D and Scott, M and Sztuc, AA and Uchida, Y and Berardi, V and Catanesi, MG and Intonti, RA and Radicioni,
E and Calabria, NF and Rosa, GD and Langella, A and Collazuol, G and Iacob,
F and Lamoureux, M and Mattiazzi, M and Ludovici, L and Gonin, M and Perisse, L and Pronost, G and Fujisawa, C and Maekawa, Y and Nishimura,
Y and Okazaki, R and Friend, M and Hasegawa, T and Ishida, T and Jakkapu,
M and Kobayashi, T and Matsubara, T and Nakadaira, T and Nakamura, K and Oyama, Y and Sakashita, K and Sekiguchi, T and Tsukamoto, T and Boschi,
T and Bhuiyan, N and Burton, GT and Gao, J and Goldsack, A and Katori, T and Lodovico, FD and Migenda, J and Sedgwick, SM and Ramsden, RM and Taani,
M and Xie, Z and Zsoldos, S and Abe, KE and Hasegawa, M and Isobe, Y and Kotsar, Y and Miyabe, H and Ozaki, H and Shiozawa, T and Sugimoto, T and Suzuki, AT and Takagi, Y and Takeuchi, Y and Yamamoto, S and Zhong, H and Ashida, Y and Feng, J and Feng, L and Hayashino, T and Hirota, S and Hu,
JR and Hu, Z and Jiang, M and Kawaue, M and Kikawa, T and Mori, M and Nakamura, KE and Nakaya, T and Wendell, RA and Yasutome, K and Jenkins,
SJ and McCauley, N and Mehta, P and Pritchard, A and Tarrant, A and Wilking, MJ and Fukuda, Y and Itow, Y and Menjo, H and Murase, M and Ninomiya, K and Niwa, T and Tsukada, M and Yoshioka, Y and Frankiewicz,
K and Lagoda, J and Mandal, M and Mijakowski, P and Prabhu, YS and Zalipska, J and Jiang, J and Jia, M and Jung, CK and Palomino, JL and Santucci, G and Shi, W and Vilela, C and Yanagisawa, C and Fukuda, D and Hagiwara, K and Harada, M and Hino, Y and Horai, T and Ishino, H and Ito,
S and Kitagawa, H and Koshio, Y and Ma, W and Nakanishi, F and Piplani, N and Sakai, S and Sakuda, M and Tada, T and Tano, T and Xu, C and Yamaguchi, R and Ishizuka, T and Kuno, Y and Barr, G and Barrow, D and Cook, L and Samani,
S and Simpson, C and Wark, D and Holin, AM and Nova, F and Jung, S and Yang,
B and Yang, JY and Yoo, J and Fannon, JEP and Kneale, L and Malek, M and McElwee, JM and Stone, O and Thiesse, MD and Thompson, LF and Wilson,
ST and Okazawa, H and Lakshmi, SM and Choi, Y and Kim, SB and Kwon, E and Seo,
JW and Yu, I and Ichikawa, AK and Tairahune, S and Nishijima, K and Eguchi,
A and Iwamoto, K and Nakagiri, K and Nakajima, Y and Ogawa, N and Shima, S and Watanabe, E and Yokoyama, M and Calland, RG and Fujita, S and Jesus-Valls, C and Junjie, X and Ming, TK and Perio, PD and Martens, K and Murdoch, M and Vagins, MR and Izumiyama, S and Kuze, M and Matsumoto, R and Okajima, Y and Tanaka, M and Yoshida, T and Inomoto, M and Ishitsuka, M and Ito, H and Kinoshita, T and Ohta, K and Ommura, Y and Shinoki, M and Shigeta, N and Suganuma, T and Yamaguchi, K and Martin, JF and Nantais,
CM and Tanaka, HA and Towstego, T and Gaur, R and Gousy-Leblanc, V and Hartz, M and Konaka, A and Li, X and Chen, S and Xu, BD and Zhang, B and Berkman, S and Posiadala-Zezula, M and Boyd, SB and Edwards, R and Hadley, D and Nicholson, M and O'Flaherty, M and Richards, B and Ali, A and Jamieson, B and Walker, J and Amanai, S and Marti, L and Minamino, A and Pintaudi, G and Sano, S and Sasaki, R and Suzuki, S and Wada,
K},
Title = {Solar neutrino measurements using the full data period of
Super-Kamiokande-IV},
Year = {2023},
Month = {December},
Key = {fds375005}
}
%% Other
@misc{fds140077,
Author = {The 2KM Collaboration},
Title = {A Proposal for a Detector 2 km Away From the T2K Neutrino
Source},
Year = {2005},
Month = {June},
Key = {fds140077}
}