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Sensitivity of the IceCube neutrino detector to dark matter annihilating in dwarf galaxies

Sandick, Pearl and Spolyar, Douglas and Buckley, Matthew and Freese, Katherine and Hooper, Dan (2010) Sensitivity of the IceCube neutrino detector to dark matter annihilating in dwarf galaxies. Physical Review D, 81 (8). Art. No. 083506 . ISSN 2470-0010. doi:10.1103/PhysRevD.81.083506.

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In this paper, we compare the relative sensitivities of gamma-ray and neutrino observations to the dark matter annihilation cross section in leptophilic models such as have been designed to explain PAMELA data. We investigate whether the high energy neutrino telescope IceCube will be competitive with current and upcoming searches by gamma-ray telescopes, such as the Atmospheric Çerenkov Telescopes (H.E.S.S., VERITAS, and MAGIC), or the Fermi Gamma-Ray Space Telescope, in detecting or constraining dark matter particles annihilating in dwarf spheroidal galaxies. We find that after 10 years of observation of the most promising nearby dwarfs, IceCube will have sensitivity comparable to the current sensitivity of gamma-ray telescopes only for very heavy (m_X ≳ 7  TeV) or relatively light (m_X ≲ 200  GeV) dark matter particles which annihilate primarily to μ^+μ^-. If dark matter particles annihilate primarily to τ^+τ^-, IceCube will have superior sensitivity only for dark matter particle masses below the 200 GeV threshold of current Atmospheric Çerenkov Telescopes. If dark matter annihilations proceed directly to neutrino-antineutrino pairs a substantial fraction of the time, IceCube will be competitive with gamma-ray telescopes for a much wider range of dark matter masses.

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Additional Information:© 2010 The American Physical Society. Received 15 December 2009; revised 26 February 2010; published 5 April 2010; publisher error corrected 12 April 2010. K. F. is supported by the US Department of Energy and MCTP via the University of Michigan and the National Science Foundation under Grant No. PHY-0455649; D. S. and D. H. are supported by the U.S. Department of Energy, including Grant No. DE-FG02-95ER40896; D.H. is also supported by NASA Grant No. NAG5-10842; P. S. is supported by the National Science Foundation under Grant No. PHY-0455649. M.B. is supported by the US Department of Energy, under Grant No. DE-FG03-92- ER40701. K. F. would like to thank the Aspen Center for Physics and the Texas Cosmology Center, and P. S. would like to thank MCTP.
Group:Caltech Theory
Funding AgencyGrant Number
US Department of EnergyDE-FG02-95ER40896
US Department of EnergyDE-FG03-92ER40701
MCTP via the University of MichiganUNSPECIFIED
Issue or Number:8
Classification Code:PACS: 95.35.+d, 95.30.Cq, 95.55.Ka, 98.52.Wz.
Record Number:CaltechAUTHORS:20100527-095649460
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Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:18476
Deposited By: Tony Diaz
Deposited On:01 Jun 2010 03:17
Last Modified:08 Nov 2021 23:44

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