Galactic substructure and dark-matter annihilation in the Milky Way halo
Abstract
We study the effects of substructure on the rate of dark-matter annihilation in the Galactic halo. We use an analytic model for substructure that can extend numerical simulation results to scales too small to be resolved by the simulations. We first calibrate the analytic model to numerical simulations, and then determine the annihilation boost factor, for standard weakly interacting massive particle (WIMP) models as well as those with Sommerfeld (or other) enhancements, as a function of galactocentric radius in the Milky Way. We provide an estimate of the dependence of the gamma-ray intensity of WIMP annihilation as a function of angular distance from the Galactic center. This methodology, coupled with future numerical simulation results can be a powerful tool that can be used to constrain WIMP properties using Fermi all-sky data.
Additional Information
© 2010 The American Physical Society. Received 19 January 2010; published 22 February 2010. This work was initiated during a workshop, attended by all three authors, hosted by the Caltech/JPL Keck Institute for Space Studies. M. Kuhlen thanks the Theoretical Astrophysics Center at UC Berkeley for support and acknowledges the hospitality of KITP at UC Santa Barbara, where part of this work was completed. This work was supported at Caltech by DoE DE-FG03-92-ER40701 and the Gordon and Betty Moore Foundation, and in part by the National Science Foundation under Grant No. PHY05-51164.Attached Files
Published - Kamionkowski2010p7443Phys_Rev_D.pdf
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Additional details
- Eprint ID
- 17969
- Resolver ID
- CaltechAUTHORS:20100414-091218940
- Department of Energy (DOE)
- DE-FG03-92-ER40701
- Gordon and Betty Moore Foundation
- NSF
- PHY05-51164
- Created
-
2010-04-30Created from EPrint's datestamp field
- Updated
-
2021-11-08Created from EPrint's last_modified field
- Caltech groups
- TAPIR, Keck Institute for Space Studies, Moore Center for Theoretical Cosmology and Physics