Dark matter at the end of the Galaxy

被引：113

作者：

Lisanti, Mariangela ^{[1
,2
]}

Strigari, Louis E. ^{[3
,4
]}

Wacker, Jay G. ^{[2
]}

Wechsler, Risa H. ^{[2
,3
,4
]}

机构：

[1] Princeton Univ, PCTS, Princeton, NJ 08540 USA

[2] SLAC Natl Accelerator Lab, Particle & Particle Astrophys Dept, Menlo Pk, CA 94025 USA

[3] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA

[4] Stanford Univ, Dept Phys, Stanford, CA 94305 USA

来源：

PHYSICAL REVIEW D | 2011年 / 83卷 / 02期

基金：

美国国家科学基金会;

关键词：

STATISTICAL-MECHANICS; SPHERICAL GALAXIES; GALACTIC HALO; MASS; KINEMATICS; PROFILE; MODELS; ORIGIN; SHAPE; GAS;

D O I：

10.1103/PhysRevD.83.023519

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Dark matter density profiles based upon ACDM cosmology motivate an ansatz velocity distribution function with fewer high-velocity particles than the Maxwell-Boltzmann distribution or proposed variants. The high-velocity tail of the distribution is determined by the outer slope of the dark matter halo-the large radius behavior of the Galactic dark matter density. N-body simulations of Galactic halos reproduce the high-velocity behavior of this ansatz. Predictions for direct detection rates are dramatically affected for models where the threshold scattering velocity is within 30% of the escape velocity.

引用

页数：10

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