NASA Technical Reports Server (NTRS) 20120009190: IceCube Sensitivity for Low-Energy Neutrinos from Nearby Supernovae

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by  NASA Technical Reports Server (NTRS)

IceCube Sensitivity for Low-Energy Neutrinos
from Nearby Supernovae
IceCube Collaboration: R. Abbasi I , Y. Abdou2, T. Abu-Zayyad3, M. Ackermann 10, J. Adams4, J. A. Aguilar I ,M. Ahlers5,
M. M. Allen 26 ,D. A It mann 18 ,K. An d een l.44 ,J. Au ff en b erg6, X. Bal· 7.45 ,M. B a k erI, S . W. B arwl.c k 8 , V. B aum3 3 ,R. B ay9,
J. L. Bazo A Ib a 10 ,K. BeattI. e 11 ,J. J . B eatty 12.13 ,S. B ech et 14 , J . K. B eck er 15 , K .-H . B eck er6, M . L . B enab de rrah mane 10 ,
S. BenZvil, J. BerdermannlO, P. Berghaus1, D. Berley16, E. Bernardini 10, D. Bertrandl4, D. Z. Bessonl7, D. Bindig6,
M. Bissokl8, E. Blaufussl6, J. Blumenthal18, D. J. Boersma I 8 ,C. Bohml9, D. Bose20, S. Boser21, O. Botner22,
A. M. Brown4, S. Buitink11, K. S. Caballero-Mora26, M. Carson2, D. Chirkin 1, B. Christyl6, F. Clevermann23, S. Cohen24,
C. Colnard25, D. F. Cowen26.27, A. H. Cruz Silva 10, M. V. D'Agostin09, M. Danninger19, J. Daughhetee28, J. C. Davisl2,
C. De Clercq20, T. Degne;l, L. Demirors24, F. Descamps2, P. Desiati 1, G. de Vries-Uiterweerd2, T. DeYoung26,
J. C. Diaz-Velez1, M. Dierckxsens14, J. Dreyer I 5, J. P. Dumm1, M. Dunkman26, J. Eisch1, R. W. Ellsworthl6, O. Engdegard22,
S. Euler I 8, P. A. Evenson 7, O. Fadiran29, A. R. Fazely30, A. Fedynitchl5, J. Feintzeig1, T. Feusels2, K. Filimonov9,
C. Finley19, T. Fischer-Wasels6, B. D. Fox26, A. Franckowiak21, R. Frankel 0, T. K. Gaisser7, J. Gallagher31, L. Gerhardt 1 1.9,
L. Gladstone I , T. Gliisenkampl8, A. Goldschmidtll, J. A. Goodmanl6, D. G6ralO, D. Grant32, T. Griesel33, A. GroB4.25,
S . Gru II on I ,M. G urtner6 ,C. Ha2 6 , A. Hal. I smal.1 2 ,A. HaI I gren 22 , F. HaI z en I ,K. H an4, K . H anson 14.1 ,D. He·m en 18 ,
K. Helbing6, R. Hellauerl6, S. Hickford4, G. C. Hill I ,K. D. Hoffmanl6, B. Hoffmannl8, A. Homeier21, K. Hoshina I,
W. HuelsnitzI6.46, J.-P. HiilBI8, P. O. Hulth 19, K. Hultqvistl9, S. Hussain 7, A. Ishihara35, E. Jakobi 10, J. Jacobsenl,
G. S . Japan· dz e 29 ,H. Jo h ansson 19 , K .-H. Kamper6t, A . Kappes 36 ,T. K arg6, A . K arI e I , P. K enny 17 , J. K·I ry IU kl1,9 , F. K·I S Ia t 10 ,
23 34 36 33 6 26 21
S. R. Klein I 1.9, H. KOhne , G. Kohnen , H. Kolanoski , L. Kopke , S. Kopper , D. J. Koskinen , M. Kowalski ,
T. Kowarik33, M. Krasbergl, G. Kro1l33, N. Kurahashi 1, T. Kuwabara 7, M. Labare20, K. Laiheml8, H. Landsman 1,
M. J. Larson 26 , R. Lauer 1,0J. ·L·un emann 33 ,J. Madsen3 , A. Marotta 14 , R. MaruyamaI , K . Mase3 5 , H. S. MatI.S II ,
K. Meagher I 6, M. Merck], P. Meszaros27.26, T. Meuresl8, S. Miarecki 11,9, E. MiddelllO, N. Milke23 , J. Mille;2,
T. M ontaru1 I· 1.37 ,R. Morse I, S. MM. o V·lt2 7 , R . Nah n h auer 10 , J . W. N am8, U.N a umann6, D. R . N ygren II ,S.O dr ows k·I2 5 ,
A. Olivasl6, M. Oliv022.15, A. 0' Murchadha1, S. Panknin21, L. Pau118, C. Perez de los Heros22, J. Petrovic 14, A. Piegsa33,
D. Pieloth23, R. Porrata9, J. Posselt6, P. B. Price9, G. T. Przybylski 11 , K. Rawlins38, P. Red116, E. Resconi25.42, W. Rhode23,
M. Ribordy24, A. S. Richard30, M. Richmanl6, J. P. Rodrigues I ,F. Rothmaier33, C. Rottl2, T. Ruhe23, D. Rutledge26,
B. Ruzybayev7, D. Ryckbosch2, H.-G. Sander33, M. Santander I ,S. Sarkar5, K. Schatt033, T. SChmidtl6, A. SchonwaldlO,
A. Schukraftl8, L. Schulte33, A. Schultes6, O. Schulz25.43, M. SChunckl8, D. Seckel7, B. Semburg6, S. H. Seol9,
39 8 20 26 3 2
Y. Sestay025, S. Seunarine , A. Silvestri , K. Singh , A. Slipak , G. M. Spiczak , C. SpieringlO, M. StamatikosI .40,
T. Stanev 7, T. Stezelberger11, R. G. Stokstad 11, A. StOBiI 0, E. A. Strahler20, R. Strom22, M. Stiie; I , G. W. Sullivan 16,
Q. S WI· 11 ens 14 ,H. Taavo Ia 22 , I. Ta b oad a 28 , A. Ta m b urro 3 ,A. Te pe2 8 , S . Ter-Antonyan 30, S . TI· 1 av 7 ,P. A . Toa Ie 26 , S . Toscano I ,
D. Tosi 10, N. van Eijndhoven20, J. Vandenbroucke9, A. Van Overloop2, J. van Santenl, M. Vehringl8, M. Voge25, C. Walck I 9 ,
T. Waldenmaier36, M. Wallraffl8, M. Walter 10 , Ch. Weaver I ,c. Wendt 1 , S. Westerhoff I , N. Whitehorn I , K. Wiebe33,
C. H. Wiebusch 18, D. R. Williams41, R. WischnewskilO, H. Wissingl6, M. WOlf25, T. R. Wood32, K. Woschnagg9, C. Xu7,
D. L. Xu41, X. W. Xu30, J. P. YanezlO, G. Yodh8, S. Yoshida35, P. Zarzhitsky41, and M. Zo1119
(Affiliations can be found ajier the references)
Received / Accepted
ABSTRACT
This paper describes the response of the lceCube neutrino telescope located at the geographic South Pole to outbursts of MeV neutrinos from the
core collapse of nearby massive stars. IceCube was completed in December 2010 forming a lattice of 5160 photomultiplier tubes that monitor a
volume of - I km3 in the deep Antarctic ice for particle induced photons. The telescope was designed to detect neutrinos with energies greater
than 100 GeY. Owing to subfreezing ice temperatures, the photomultiplier dark noise rates are particularly low. Hence IceCube can also detect
large numbers of MeV neutrinos by observing a collective rise in all photomultiplier rates on top of the dark noise. With 2 ms timing resolution,
JceCube can detcct subtle features in the temporal development of the supernova neutrino burst. For a supemova at the galactic center, its sensitivity
matches that of a background-free megaton-scale supernova search experiment. The sensitivity decreases to 20 standard deviations at the galactic
edge (30 kpc) and 6 standard deviations at the Large Magellanic Cloud (50 kpc). lceCube is sending triggers from potential supernovae to the
Supernova Early Warning System. The to neutrino properties such as the neutrino hierarchy is discussed, as well as the possibility to
detect the neutronization burst, a short outbreak's released by electron capture on protons soon after collapse. Tantalizing signatures, such as
the formation of a quark star or a black hole as well as the characteristics of shock waves, are investigated to illustrate IceCube's capability for
supernova detection.
Key words. neutrinos supernovae: general - telescope