Stellar Mass to Halo Mass Scaling Relation for X-ray Selected Low Mass Galaxy Clusters and Groups out to Redshift $z\approx 1$

Abstract

We present the stellar mass-halo mass scaling relation for 46 X-ray selected low-mass clusters or groups detected in the XMM-BCS survey with masses $2\times 10^{13}{M}_{\odot }\lesssim M_{500}\lesssim 2.5\times 10^{14}{M}_{\odot }$ at redshift $0.1\le z\le 1.02$. The cluster binding masses $M_{500}$ are inferred from the measured X-ray luminosities \Lx, while the stellar masses $M_{\star }$ of the galaxy populations are estimated using near-infrared imaging from the SSDF survey and optical imaging from the BCS survey. With the measured \Lx\ and stellar mass $M_{\star }$, we determine the best fit stellar mass-halo mass relation, accounting for selection effects, measurement uncertainties and the intrinsic scatter in the scaling relation. The resulting mass trend is $M_{\star }\propto M_{500}^{0.69\pm 0.15}$, the intrinsic (log-normal) scatter is ${\sigma }_{\ln M_{\star }|M_{500}}=0.36_{-0.06}^{+0.07}$, and there is no significant redshift trend $M_{\star }\propto (1+z{)}^{-0.04\pm 0.47}$, although the uncertainties are still large. We also examine $M_{\star }$ within a fixed projected radius of $0.5$~Mpc, showing that it provides a cluster binding mass proxy with intrinsic scatter of $\approx 93\%$ (1$\sigma$ in $M_{500}$). We compare our $M_{\star }=M_{\star }(M_{500},z)$ scaling relation from the XMM-BCS clusters with samples of massive, SZE-selected clusters ($M_{500}\approx 6\times 10^{14}{M}_{\odot }$) and low mass NIR-selected clusters ($M_{500}\approx 10^{14}{M}_{\odot }$) at redshift $0.6\lesssim z\lesssim 1.3$. After correcting for the known mass measurement systematics in the compared samples, we find that the scaling relation is in good agreement with the high redshift samples, suggesting that for both groups and clusters the stellar content of the galaxy populations within $R_{500}$ depends strongly on mass but only weakly on redshift out to $z\approx 1$.

15 pages, 10 figures. Accepted for publication in MNRAS

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