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Search for gamma-ray emission from dark matter annihilation in the large magellanic cloud with the fermi large area telescope

Matthew R. Buckley1, Eric Charles2, Jennifer M. Gaskins3,4, Alyson M. Brooks1, Alex Drlica-Wagner5, Pierrick Martin6, and Geng Zhao2

  • 1Department of Physics and Astronomy, Rutgers University, Piscataway, New Jersey 08854, USA
  • 2W. 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
  • 3California Institute of Technology, Pasadena, California 91125, USA
  • 4GRAPPA, University of Amsterdam, 1098 XH Amsterdam, Netherlands
  • 5Center for Particle Astrophysics, Fermi National Accelerator Laboratory, Batavia, Illinois 60510, USA
  • 6Institut de Recherche en Astrophysique et Planétologie, UPS/CNRS, UMR5277, 31028 Toulouse cedex 4, France

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Phys. Rev. D 91, 102001 – Published 5 May, 2015

DOI: https://doi.org/10.1103/PhysRevD.91.102001

Abstract

At a distance of 50 kpc and with a dark matter mass of ∼1010  M⊙, the large magellanic cloud (LMC) is a natural target for indirect dark matter searches. We use five years of data from the Fermi Large Area Telescope (LAT) and updated models of the gamma-ray emission from standard astrophysical components to search for a dark matter annihilation signal from the LMC. We perform a rotation curve analysis to determine the dark matter distribution, setting a robust minimum on the amount of dark matter in the LMC, which we use to set conservative bounds on the annihilation cross section. The LMC emission is generally very well described by the standard astrophysical sources, with at most a 1–2σ excess identified near the kinematic center of the LMC once systematic uncertainties are taken into account. We place competitive bounds on the dark matter annihilation cross section as a function of dark matter particle mass and annihilation channel.

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Phys. Rev. D 91, 102001– Published 5 May, 2015
  • Received 2 February 2015
Article part of CHORUS

© 2015 American Physical Society

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