Estimate for GLAST LAT Milky Way Dark Matter WIMP Line Sensitivity

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The LAT Dark Matter and New Physics Working group has been developing approaches for the indirect astrophysical detection of annihilation of dark matter. Our work has assumed that a significant component of dark matter is a new type of Weakly Interacting Massive Particle (WIMP). The annihilation of two WIMPs usually results in the production of many high energy gamma rays (>1 GeV) that can be well measured in the GLAST LAT if present. There is also the possibility to observe {gamma} lines from annihilation into {gamma}{gamma} and or {gamma}Z final states. In popular SUSY theories these line decays occur at ... continued below

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2 pages

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Edmonds, Y.; Baltz, E.; Bloom, E.; Cohen-Tanugi, J.; Godfrey, G.; Wai, L. et al. November 2, 2007.

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The LAT Dark Matter and New Physics Working group has been developing approaches for the indirect astrophysical detection of annihilation of dark matter. Our work has assumed that a significant component of dark matter is a new type of Weakly Interacting Massive Particle (WIMP). The annihilation of two WIMPs usually results in the production of many high energy gamma rays (>1 GeV) that can be well measured in the GLAST LAT if present. There is also the possibility to observe {gamma} lines from annihilation into {gamma}{gamma} and or {gamma}Z final states. In popular SUSY theories these line decays occur at the 10{sup -4} to 10{sup -2} branching fraction level. Estimates of LAT sensitivity (at 5{sigma} above background) and upper limits (upper limit at the 95% confidence level) to these WIMP lines will be presented. These sensitivities are given in photons/cm2/sec/sr and so do not depend on the WIMP models. However, they do depend on the diffuse background model. The latter is derived from GALPROP[1] based on EGRET and other data in the EGRET energy range. We use extrapolations, provided by the GALPROP team to the higher energy range of 150 GeV explored in the preliminary line sensitivity study presented here. Comparison with theory depends upon the WIMP model (e.g., line energy and 1 or 2 lines), the DM halo model, and other astrophysics backgrounds. Thus estimates of the ability of the LAT to actually observe WIMP lines can vary over orders of magnitude depending upon which models are chosen.

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2 pages

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  • Journal Name: AIP Conf.Proc.921:514-515,2007; Conference: Prepared for 1st GLAST Symposium, Stanford, Palo Alto, 5-8 Feb 2007

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  • Report No.: SLAC-PUB-12941
  • Grant Number: AC02-76SF00515
  • Office of Scientific & Technical Information Report Number: 918975
  • Archival Resource Key: ark:/67531/metadc882125

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  • November 2, 2007

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  • Sept. 22, 2016, 2:13 a.m.

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  • Dec. 5, 2016, 3:16 p.m.

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Edmonds, Y.; Baltz, E.; Bloom, E.; Cohen-Tanugi, J.; Godfrey, G.; Wai, L. et al. Estimate for GLAST LAT Milky Way Dark Matter WIMP Line Sensitivity, article, November 2, 2007; [Menlo Park, California]. (digital.library.unt.edu/ark:/67531/metadc882125/: accessed September 24, 2017), University of North Texas Libraries, Digital Library, digital.library.unt.edu; crediting UNT Libraries Government Documents Department.