Realistic estimation for the detectability of dark matter subhalos using Fermi-LAT catalogs

Francesca Calore, Valentina De Romeri, Mattia Di Mauro, Fiorenza Donato, and Federico Marinacci
Phys. Rev. D 96, 063009 – Published 15 September 2017

Abstract

Numerical simulations of structure formation have made remarkable progress in recent years, in particular due to the inclusion of baryonic physics evolving with the dark matter component. We generate Monte Carlo realizations of the dark matter subhalo population based on the results of the recent hydrodynamical simulation suite of Milky Way–sized galaxies [F. Marinacci, R. Pakmor, and V. Springel, Mon. Not. R. Astron. Soc. 437, 1750 (2014).]. We then simulate the gamma-ray sky for both the setup of the 3FGL and 2FHL Fermi Large Area Telescope (LAT) catalogs, including the contribution from the annihilation of dark matter in the subhalos. We find that the flux sensitivity threshold strongly depends on the particle dark matter mass and, more mildly, also on its annihilation channel and the observation latitude. The results differ for the 3FGL and 2FHL catalogs, given their different energy thresholds. We also predict that the number of dark matter subhalos among the unassociated sources is very small. A null number of detectable subhalos in the Fermi-LAT 3FGL catalog would imply upper limits on the dark matter annihilation cross section into bb¯ of 2×1026(5×1025)cm3/s with MDM=50(1000)GeV. We find less than one extended subhalo in the Fermi-LAT 3FGL catalog. As a matter of fact, the differences in the spatial and mass distribution of subhalos between hydrodynamic and dark matter–only runs do not have significant impact on the detectability of dark subhalos in gamma rays.

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  • Received 4 May 2017

DOI:https://doi.org/10.1103/PhysRevD.96.063009

© 2017 American Physical Society

Physics Subject Headings (PhySH)

Gravitation, Cosmology & AstrophysicsParticles & Fields

Authors & Affiliations

Francesca Calore1,*, Valentina De Romeri2,†, Mattia Di Mauro3,‡, Fiorenza Donato4,§, and Federico Marinacci5,∥

  • 1LAPTh, CNRS, and Université Savoie Mont Blanc, 9 Chemin de Bellevue, B.P. 110 Annecy-le-Vieux F-74941, France
  • 2Departamento de Física Teórica and Instituto de Física Teórica, IFT-UAM/CSIC, Universidad Autónoma de Madrid, Cantoblanco, 28049 Madrid, Spain
  • 3W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University, Stanford, California 94305, USA
  • 4Dipartimento di Fisica, Università di Torino and Istituto Nazionale di Fisica Nucleare, Sezione di Torino, via P. Giuria 1, I-10125 Torino, Italy
  • 5Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, Massachusetts 02139, USA

  • *francesca.calore@lapth.cnrs.fr
  • valentina.deromeri@uam.es
  • mdimauro@slac.stanford.edu
  • §donato@to.infn.it
  • fmarinac@mit.edu

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Issue

Vol. 96, Iss. 6 — 15 September 2017

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