Dark matter at the end of the Galaxy

被引:111
|
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.
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页数:10
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