The Halo Concentration and Mass Relation Traced by Satellite Galaxies  

作　　者：Qing Gu Qi Guo Tianchi Zhang Wenting Wang Quan Guo Liang Gao 

机构地区：[1]Key Laboratory for Computational Astrophysics,National Astronomical Observatories,Chinese Academy of Sciences,Beijing 100101,China [2]School of Astronomy and Space Science,University of Chinese Academy of Sciences,Beijing 100049,China [3]Beijing Planetarium,Beijing Academy of Science and Technology,Beijing 100044,China [4]Department of Astronomy,Shanghai Jiao Tong University,Shanghai 200240,China [5]Shanghai Key Laboratory for Particle Physics and Cosmology,Shanghai 200240,China [6]Shanghai Astronomical Observatory,Chinese Academy of Sciences,Shanghai 200030,China [7]Institute of Computational Cosmology,Department of Physics,University of Durham,Science Laboratories,South Road,Durham DH13LE,UK

出　　处：《Research in Astronomy and Astrophysics》2022年第12期292-298,共7页天文和天体物理学研究（英文版）

基　　金：supported by the National Key Research and Development of China (No. 2018YFA0404503);NSFC (grant Nos. 12033008 and 11988101);the K.C.Wong Education Foundation, and the science research grants from the China Manned Space Project with Nos. CMS-CSST-2021-A03 and CMS-CSST-2021-A07;support from the joint Sino-German DFG research Project The Cosmic Web and its impact on galaxy formation and alignment (DFG-LI 2015/5-1, NSFC No. 11861131006);the support of the Shanghai International partners project (No. 19590780200);the support from NSFC (12022307);the Yangyang Development Fund。

摘　　要：We study the relation between halo concentration and mass(c-M relation) using galaxy catalogs of the Seventh and Eighth Data Releases of the Sloan Digital Sky Survey(SDSS DR7 and DR8). Assuming that the satellite galaxies follow the distribution of dark matter, we derive the halo concentration by fitting the satellite radial profile with a Nararro Frank and White(NFW) format. The derived c-M relation covers a wide halo mass range from10^(11.6)to 10^(14.1)M_(⊙). We confirm the anti-correlation between the halo mass and concentration as predicted in cosmological simulations. Our results are in good agreement with those derived using galaxy dynamics and gravitational lensing for halos of 10^(11.6)– 10^(12.9)M_(⊙), while they are slightly lower for halos of 10^(12.9)– 10^(14.1)M_(⊙).This is because blue satellite galaxies are less concentrated, especially in the inner regions. Instead of using all satellite galaxies, red satellites could be better tracers of the underlying dark matter distribution in galaxy groups.

关 键 词：galaxies:halos galaxies:evolution galaxies:abundances 

分 类 号：P148[天文地球—天体物理]