Can I read Halo Mass-observable Proxy Scaling Relations and Their Dependencies on Galaxy and Group Properties on EtoBox?

Halo Mass-observable Proxy Scaling Relations and Their Dependencies on Galaxy and Group Properties by Zhang, Ziwen; Wang, Huiyuan; Luo, Wentao; Mo, Houjun; Zhang, Jun; Yang, Xiaohu; Li, Hao; Li, Qinxun is a scholarly article available to read on EtoBox.

What is Halo Mass-observable Proxy Scaling Relations and Their Dependencies on Galaxy and Group Properties about?

Based on the DECaLS shear catalog, we study the scaling relations between halo mass($M_{\rm h}$) and various proxies for SDSS central galaxies, including stellar mass($M_*$), stellar velocity dispersion($\sigma_*$), abundance matching halo mass($M_{\rm AM}$) and satellite velocity dispersion($\sigma_{\rm s}$), and their dependencies on galaxy and group properties. In general, these proxies all have strong positive correlations with $M_{\rm h}$, consistent with previous studies. We find that the $M_{\rm h}$-$M_*$ and $M_{\rm h}$-$\sigma_*$ relations depend strongly on group richness($N_{\rm sat}$), while the $M_{\rm h}$-$M_{\rm AM}$ and $M_{\rm h}$-$\sigma_{\rm s}$ relations are independent of it. Moreover, the dependence on star formation rate(SFR) is rather weak in the $M_{\rm h}$-$\sigma_*$ and $M_{\rm h}$-$\sigma_{\rm s}$ relations, but very prominent in the other two. $\sigma_{\rm s}$ is thus the best proxy among them, and its scaling relation is in good agreement with hydro-dynamical simulations. However, estimating $\sigma_{\rm s}$ accurately for individual groups/clusters is challenging because of interlopers and the requirement for sufficient satellites. We construct new pr

Author

Zhang, Ziwen; Wang, Huiyuan; Luo, Wentao; Mo, Houjun; Zhang, Jun; Yang, Xiaohu; Li, Hao; Li, Qinxun

Published

2023

Language

EN