DWARF GALAXY ANNIHILATION AND DECAY EMISSION PROFILES FOR DARK MATTER EXPERIMENTS

被引：192

作者：

Geringer-Sameth, Alex ^{[1
,2
]}

Koushiappas, Savvas M. ^{[1
]}

Walker, Matthew ^{[2
]}

机构：

[1] Brown Univ, Dept Phys, Providence, RI 02912 USA

[2] Carnegie Mellon Univ, McWilliams Ctr Cosmol, Dept Phys, Pittsburgh, PA 15213 USA

来源：

ASTROPHYSICAL JOURNAL | 2015年 / 801卷 / 02期

基金：

美国国家科学基金会;

关键词：

dark matter; galaxies: dwarf; galaxies: fundamental parameters; galaxies: kinematics and dynamics; MILKY-WAY SATELLITE; COMPLETE SPECTROSCOPIC SURVEY; LEO V; SPHEROIDAL GALAXIES; FORMATION HISTORY; SEGUE; KINEMATICS; MODELS; MASS; HALO;

D O I：

10.1088/0004-637X/801/2/74

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Gamma-ray searches for dark matter annihilation and decay in dwarf galaxies rely on an understanding of the dark matter density profiles of these systems. Conversely, uncertainties in these density profiles propagate into the derived particle physics limits as systematic errors. In this paper we quantify the expected dark matter signal from 20 Milky Way dwarfs using a uniform analysis of the most recent stellar-kinematic data available. Assuming that the observed stellar populations are equilibrium tracers of spherically symmetric gravitational potentials that are dominated by dark matter, we find that current stellar-kinematic data can predict the amplitudes of annihilation signals to within a factor of a few for the ultra-faint dwarfs of greatest interest. On the other hand, the expected signal from several classical dwarfs (with high-quality observations of large numbers of member stars) can be localized to the similar to 20% level. These results are important for designing maximally sensitive searches in current and future experiments using space and ground-based instruments.

引用

页数：18

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