论文标题
卫星星系追踪的光晕浓度和质量关系
The halo concentration and mass relation traced by satellite galaxies
论文作者
论文摘要
我们使用Sloan数字天空调查（SDSS DR7和DR8）银河系目录的第七和第八个数据发布来研究Halo浓度与质量关系（C-M关系）之间的关系。假设卫星星系遵循暗物质的分布，我们通过将卫星径向剖面与Nararro Frank和White（NFW）格式拟合来得出光晕浓度。派生的C-M关系涵盖了宽的Halo质量范围从$ 10^{11.6} $到$ 10^{14.1} \ rm \ m_ \ odot $。我们证实了宇宙学模拟中预测的光环质量与浓度之间的抗相关性。我们的结果与使用星系动力学和重力镜片的衍生成$ 10^{{11.6} -10^{12.9} \ rm \ m_ \ odot $衍生的结果非常吻合，而它们的光环略低于$ 10^{12.9}} {12.9} -10} -10^{14.1} {14.1} {14.1} \ rm \ rm \ m_ \ odoot。这是因为蓝色卫星星系的集中程度较小，尤其是在内部区域。红色卫星不使用所有卫星星系，而是更好的示踪星系组的暗物质分布。
We study the relation between halo concentration and mass (c-M relation) using the Seventh and Eighth Data Release of the Sloan Digital Sky Survey (SDSS DR7 and DR8) galaxy catalogue. 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 from $10^{11.6}$ to $10^{14.1} \rm\ M_\odot$. 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 $10^{11.6}-10^{12.9} \rm\ M_\odot$, while they are slightly lower for halos of $10^{12.9}-10^{14.1}\rm\ M_\odot$. It 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.
