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IceCube sensitivity for low-energy neutrinos from nearby supernovae

R Abbasi, Yasser Abdou UGent, T Abu-Zayyad, M Ackermann, J Adams, JA Aguilar, M Ahlers, MM Allen, D Altmann and K Andeen, et al. (2011) ASTRONOMY & ASTROPHYSICS. 535.
abstract
This paper describes the response of the IceCube 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 similar to 1 km(3) in the deep Antarctic ice for particle induced photons. The telescope was designed to detect neutrinos with energies greater than 100 GeV. 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, IceCube can detect subtle features in the temporal development of the supernova neutrino burst. For a supernova 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). IceCube is sending triggers from potential supernovae to the Supernova Early Warning System. The sensitivity to neutrino properties such as the neutrino hierarchy is discussed, as well as the possibility to detect the neutronization burst, a short outbreak of nu(e)'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.
Please use this url to cite or link to this publication:
author
organization
year
type
journalArticle (original)
publication status
published
subject
keyword
GRAVITATIONAL-WAVE, NEUTRON-STAR, EXPLOSION MECHANISM, EQUATION-OF-STATE, CORE-COLLAPSE SUPERNOVAE, instrumention: detectors, supernovae: general, neutrinos, DETECTOR, BURST, SN1987A, SIGNAL, WATER
journal title
ASTRONOMY & ASTROPHYSICS
Astron. Astrophys.
volume
535
article_number
A109
pages
18 pages
Web of Science type
Article
Web of Science id
000297841200121
JCR category
ASTRONOMY & ASTROPHYSICS
JCR impact factor
4.587 (2011)
JCR rank
10/56 (2011)
JCR quartile
1 (2011)
ISSN
0004-6361
DOI
10.1051/0004-6361/201117810
language
English
UGent publication?
yes
classification
A1
additional info
correction published in Astron. Astrophys. (2014) 563, C1 ; DOI 10.1051/0004-6361/201117810e
copyright statement
I have transferred the copyright for this publication to the publisher
id
2145786
handle
http://hdl.handle.net/1854/LU-2145786
date created
2012-06-13 14:16:33
date last changed
2015-06-22 15:10:05
@article{2145786,
  abstract     = {This paper describes the response of the IceCube 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 similar to 1 km(3) in the deep Antarctic ice for particle induced photons. The telescope was designed to detect neutrinos with energies greater than 100 GeV. 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, IceCube can detect subtle features in the temporal development of the supernova neutrino burst. For a supernova 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). IceCube is sending triggers from potential supernovae to the Supernova Early Warning System. The sensitivity to neutrino properties such as the neutrino hierarchy is discussed, as well as the possibility to detect the neutronization burst, a short outbreak of nu(e)'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.},
  articleno    = {A109},
  author       = {Abbasi, R and Abdou, Yasser and Abu-Zayyad, T and Ackermann, M and Adams, J and Aguilar, JA and Ahlers, M and Allen, MM and Altmann, D and Andeen, K and Auffenberg, J and Bai, X and Baker, M and Barwick, SW and Baum, V and Bay, R and Alba, JLB and Beattie, K and Beatty, JJ and Bechet, S and Becker, JK and Becker, KH and Benabderrahmane, ML and BenZvi, S and Berdermann, J and Berghaus, P and Berley, D and Bernardini, E and Bertrand, D and Besson, DZ and Bindig, D and Bissok, M and Blaufuss, E and Blumenthal, J and Boersma, DJ and Bohm, C and Bose, D and Boser, S and Botner, O and Brown, AM and Buitink, S and Caballero-Mora, KS and Carson, Michael and Chirkin, D and Christy, B and Clevermann, F and Cohen, S and Colnard, C and Cowen, DF and Silva, AHC and D'Agostino, MV and Danninger, M and Daughhetee, J and Davis, JC and De Clercq, C and Degner, T and Demirors, L and Descamps, Freija and Desiati, P and De Vries-Uiterweerd, Garmt and DeYoung, T and Diaz-Velez, JC and Dierckxsens, M and Dreyer, J and Dumm, JP and Dunkman, M and Eisch, J and Ellsworth, RW and Engdegard, O and Euler, S and Evenson, PA and Fadiran, O and Fazely, AR and Fedynitch, A and Feintzeig, J and Feusels, Tom and Filimonov, K and Finley, C and Fischer-Wasels, T and Fox, BD and Franckowiak, A and Franke, R and Gaisser, TK and Gallagher, J and Gerhardt, L and Gladstone, L and Glusenkamp, T and Goldschmidt, A and Goodman, JA and Gora, D and Grant, D and Griesel, T and Gross, A and Grullon, S and Gurtner, M and Ha, C and Haj Ismail, Abd Al Karim and Hallgren, A and Halzen, F and Han, K and Hanson, K and Heinen, D and Helbing, K and Hellauer, R and Hickford, S and Hill, GC and Hoffman, KD and Hoffmann, B and Homeier, A and Hoshina, K and Huelsnitz, W and Hulss, JP and Hulth, PO and Hultqvist, K and Hussain, S and Ishihara, A and Jakobi, E and Jacobsen, J and Japaridze, GS and Johansson, H and Kampert, KH and Kappes, A and Karg, T and Karle, A and Kenny, P and Kiryluk, J and Kislat, F and Klein, SR and Kohne, H and Kohnen, G and Kolanoski, H and Kopke, L and Kopper, S and Koskinen, DJ and Kowalski, M and Kowarik, T and Krasberg, M and Kroll, G and Kurahashi, N and Kuwabara, T and Labare, Mathieu and Laihem, K and Landsman, H and Larson, MJ and Lauer, R and Lunemann, J and Madsen, J and Marotta, A and Maruyama, R and Mase, K and Matis, HS and Meagher, K and Merck, M and Meszaros, P and Meures, T and Miarecki, S and Middell, E and Milke, N and Miller, J and Montaruli, T and Morse, R and Movit, SM and Nahnhauer, R and Nam, JW and Naumann, U and Nygren, DR and Odrowski, S and Olivas, A and Olivo, M and O'Murchadha, A and Panknin, S and Paul, L and de los Heros, CP and Petrovic, J and Piegsa, A and Pieloth, D and Porrata, R and Posselt, J and Price, PB and Przybylski, GT and Rawlins, K and Redl, P and Resconi, E and Rhode, W and Ribordy, M and Richard, AS and Richman, M and Rodrigues, JP and Rothmaier, F and Rott, C and Ruhe, T and Rutledge, D and Ruzybayev, B and Ryckbosch, Dirk and Sander, HG and Santander, M and Sarkar, S and Schatto, K and Schmidt, T and Schonwald, A and Schukraft, A and Schulte, L and Schultes, A and Schulz, O and Schunck, M and Seckel, D and Semburg, B and Seo, SH and Sestayo, Y and Seunarine, S and Silvestri, A and Singh, K and Slipak, A and Spiczak, GM and Spiering, C and Stamatikos, M and Stanev, T and Stezelberger, T and Stokstad, RG and Stossl, A and Strahler, EA and Strom, R and Stuer, M and Sullivan, GW and Swillens, Q and Taavola, H and Taboada, I and Tamburro, A and Tepe, A and Ter-Antonyan, S and Tilav, S and Toale, PA and Toscano, S and Tosi, D and van Eijndhoven, N and Vandenbroucke, J and Van Overloop, Arne and van Santen, J and Vehring, M and Voge, M and Walck, C and Waldenmaier, T and Wallraff, M and Walter, M and Weaver, C and Wendt, C and Westerhoff, S and Whitehorn, N and Wiebe, K and Wiebusch, CH and Williams, DR and Wischnewski, R and Wissing, H and Wolf, M and Wood, TR and Woschnagg, K and Xu, C and Xu, DL and Xu, XW and Yanez, JP and Yodh, G and Yoshida, S and Zarzhitsky, P and Zoll, M},
  issn         = {0004-6361},
  journal      = {ASTRONOMY \& ASTROPHYSICS},
  keyword      = {GRAVITATIONAL-WAVE,NEUTRON-STAR,EXPLOSION MECHANISM,EQUATION-OF-STATE,CORE-COLLAPSE SUPERNOVAE,instrumention: detectors,supernovae: general,neutrinos,DETECTOR,BURST,SN1987A,SIGNAL,WATER},
  language     = {eng},
  pages        = {18},
  title        = {IceCube sensitivity for low-energy neutrinos from nearby supernovae},
  url          = {http://dx.doi.org/10.1051/0004-6361/201117810},
  volume       = {535},
  year         = {2011},
}

Chicago
Abbasi, R, Yasser Abdou, T Abu-Zayyad, M Ackermann, J Adams, JA Aguilar, M Ahlers, et al. 2011. “IceCube Sensitivity for Low-energy Neutrinos from Nearby Supernovae.” Astronomy & Astrophysics 535.
APA
Abbasi, R., Abdou, Y., Abu-Zayyad, T., Ackermann, M., Adams, J., Aguilar, J., Ahlers, M., et al. (2011). IceCube sensitivity for low-energy neutrinos from nearby supernovae. ASTRONOMY & ASTROPHYSICS, 535.
Vancouver
1.
Abbasi R, Abdou Y, Abu-Zayyad T, Ackermann M, Adams J, Aguilar J, et al. IceCube sensitivity for low-energy neutrinos from nearby supernovae. ASTRONOMY & ASTROPHYSICS. 2011;535.
MLA
Abbasi, R, Yasser Abdou, T Abu-Zayyad, et al. “IceCube Sensitivity for Low-energy Neutrinos from Nearby Supernovae.” ASTRONOMY & ASTROPHYSICS 535 (2011): n. pag. Print.