arXiv:1712.03188·v1·Cosmology and Nongalactic Astrophysics
-factors for self-interacting dark matter in 20 dwarf spheroidal galaxies
Sebastian Bergström🇸🇪 · Riccardo Catena🇸🇪 · Andrea Chiappo🇸🇪 · Jan Conrad🇸🇪 · Björn Eurenius🇸🇪 · Magdalena Eriksson🇸🇪 · Michael Högberg🇸🇪 · Susanna Larsson🇸🇪 · Emelie Olsson🇸🇪 · Andreas Unger🇸🇪 · Rikard Wadman🇸🇪
Abstract
Dwarf spheroidal galaxies are among the most promising targets for indirect dark matter (DM) searches in -rays. The -ray flux from DM annihilation in a dwarf spheroidal galaxy is proportional to the -factor of the source. The -factor of a dwarf spheroidal galaxy is the line-of-sight integral of the DM mass density squared times , where is the DM annihilation cross-section times relative velocity , angle brackets denote average over , and is the -independent part of . If is constant in , -factors only depend on the DM space distribution in the source. However, if varies with , as in the presence of DM self-interactions, -factors also depend on the DM velocity distribution, and on the strength and range of the DM self-interaction. Models for self-interacting DM are increasingly important in the study of the small scale clustering of DM, and are compatible with current cosmological observations. Here we derive the -factor of 20 dwarf spheroidal galaxies from stellar kinematic data under the assumption of Yukawa DM self-interactions. -factors are derived through a profile Likelihood approach, assuming either NFW or cored DM profiles. We also compare our results with -factors derived assuming the same velocity for all DM particles in the target galaxy. We find that this common approximation overestimates the -factors by up to one order of magnitude. -factors for a sample of DM particle masses, self-interaction coupling constants and density profiles are provided electronically, ready to be used in other projects.
Comments: 10 pages, 3 figures and 2 tables