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Title: The Dark Matter Annihilation Signal from Galactic Substructure: Predictions for GLAST

Abstract

In this article, we present quantitative predictions for the detectability of individual Galactic dark matter subhalos in gamma rays from dark matter pair annihilations in their centers. Our method is based on a hybrid approach, employing the highest resolution numerical simulations available (including the recently completed 1 billion particle Via Lactea II simulation), as well as analytical models, for extrapolating beyond the simulations' resolution limit. We include a self-consistent treatment of subhalo boost factors, motivated by our numerical results, and a realistic treatment of the expected backgrounds that individual subhalos must outshine. We show that for reasonable values of the dark matter particle physics parameters (Mχ ~ 50-500 GeV and $$\langle$$ σv $$\rangle$$ ~ 10-26-10-25 cm3 s-1) GLAST may very well discover a few, even up to several dozen, such subhalos at 5 σ significance, and some at more than 20 σ. We predict that the majority of luminous sources would be resolved with GLAST's expected angular resolution. For most observer locations, the angular distribution of detectable subhalos is consistent with a uniform distribution across the sky. The brightest subhalos tend to be massive (median Vmax of 24 km s-1) and therefore likely hosts of dwarf galaxies, but many subhalos with Vmax-1 are also visible. Typically detectable subhalos are 20-40 kpc from the observer, and only a small fraction are closer than 10 kpc. The total number of observable subhalos has not yet converged in our simulations, and we estimate that we may be missing up to 3/4 of all detectable subhalos.

Authors:
 [1];  [2];  [2]
  1. Inst. for Advanced Study, Princeton, NJ (United States)
  2. Univ. of California, Santa Cruz, CA (United States)
Publication Date:
Research Org.:
Oak Ridge National Lab. (ORNL), Oak Ridge, TN (United States). Oak Ridge Leadership Computing Facility (OLCF)
Sponsoring Org.:
USDOE Office of Science (SC)
OSTI Identifier:
1564656
Resource Type:
Accepted Manuscript
Journal Name:
Astrophysical Journal
Additional Journal Information:
Journal Volume: 686; Journal Issue: 1; Journal ID: ISSN 0004-637X
Publisher:
Institute of Physics (IOP)
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; astronomy & astrophysics; dark matter; galaxies; halos; structure; gamma rays; n-body simulations

Citation Formats

Kuhlen, Michael, Diemand, Jürg, and Madau, Piero. The Dark Matter Annihilation Signal from Galactic Substructure: Predictions for GLAST. United States: N. p., 2008. Web. https://doi.org/10.1086/590337.
Kuhlen, Michael, Diemand, Jürg, & Madau, Piero. The Dark Matter Annihilation Signal from Galactic Substructure: Predictions for GLAST. United States. https://doi.org/10.1086/590337
Kuhlen, Michael, Diemand, Jürg, and Madau, Piero. Fri . "The Dark Matter Annihilation Signal from Galactic Substructure: Predictions for GLAST". United States. https://doi.org/10.1086/590337. https://www.osti.gov/servlets/purl/1564656.
@article{osti_1564656,
title = {The Dark Matter Annihilation Signal from Galactic Substructure: Predictions for GLAST},
author = {Kuhlen, Michael and Diemand, Jürg and Madau, Piero},
abstractNote = {In this article, we present quantitative predictions for the detectability of individual Galactic dark matter subhalos in gamma rays from dark matter pair annihilations in their centers. Our method is based on a hybrid approach, employing the highest resolution numerical simulations available (including the recently completed 1 billion particle Via Lactea II simulation), as well as analytical models, for extrapolating beyond the simulations' resolution limit. We include a self-consistent treatment of subhalo boost factors, motivated by our numerical results, and a realistic treatment of the expected backgrounds that individual subhalos must outshine. We show that for reasonable values of the dark matter particle physics parameters (Mχ ~ 50-500 GeV and $\langle$ σv $\rangle$ ~ 10-26-10-25 cm3 s-1) GLAST may very well discover a few, even up to several dozen, such subhalos at 5 σ significance, and some at more than 20 σ. We predict that the majority of luminous sources would be resolved with GLAST's expected angular resolution. For most observer locations, the angular distribution of detectable subhalos is consistent with a uniform distribution across the sky. The brightest subhalos tend to be massive (median Vmax of 24 km s-1) and therefore likely hosts of dwarf galaxies, but many subhalos with Vmax-1 are also visible. Typically detectable subhalos are 20-40 kpc from the observer, and only a small fraction are closer than 10 kpc. The total number of observable subhalos has not yet converged in our simulations, and we estimate that we may be missing up to 3/4 of all detectable subhalos.},
doi = {10.1086/590337},
journal = {Astrophysical Journal},
number = 1,
volume = 686,
place = {United States},
year = {2008},
month = {10}
}

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