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We present the stellar mass-halo mass scaling relation for 46 X-ray selectedlow-mass clusters or groups detected in the XMM-BCS survey with masses$2\times10^{13}M_{\odot}\lesssim M_{500}\lesssim2.5\times10^{14}M_{\odot}$ atredshift $0.1\le z \le1.02$. The cluster binding masses $M_{500}$ are inferredfrom the measured X-ray luminosities \Lx, while the stellar masses $M_{\star}$of the galaxy populations are estimated using near-infrared imaging from theSSDF survey and optical imaging from the BCS survey. With the measured \Lx\ andstellar mass $M_{\star}$, we determine the best fit stellar mass-halo massrelation, accounting for selection effects, measurement uncertainties and theintrinsic scatter in the scaling relation. The resulting mass trend is$M_{\star}\propto M_{500}^{0.69\pm0.15}$, the intrinsic (log-normal) scatter is$\sigma_{\ln M_{\star}|M_{500}}=0.36^{+0.07}_{-0.06}$, and there is nosignificant redshift trend $M_{\star}\propto (1+z)^{-0.04\pm0.47}$, althoughthe uncertainties are still large. We also examine $M_{\star}$ within a fixedprojected radius of $0.5$~Mpc, showing that it provides a cluster binding massproxy with intrinsic scatter of $\approx93\%$ (1$\sigma$ in $M_{500}$). Wecompare our $M_{\star}=M_{\star}(M_{500}, z)$ scaling relation from the XMM-BCSclusters with samples of massive, SZE-selected clusters($M_{500}\approx6\times10^{14}M_{\odot}$) and low mass NIR-selected clusters($M_{500}\approx10^{14}M_{\odot}$) at redshift $0.6\lesssim z \lesssim1.3$.After correcting for the known mass measurement systematics in the comparedsamples, we find that the scaling relation is in good agreement with the highredshift samples, suggesting that for both groups and clusters the stellarcontent of the galaxy populations within $R_{500}$ depends strongly on mass butonly weakly on redshift out to $z\approx1$.

Stellar Mass to Halo Mass Scaling Relation for X-ray Selected Low Mass Galaxy Clusters and Groups out to Redshift $z\approx1$