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Chiu, I.; Saro, A.; Mohr, J.; Desai, S.; Bocquet, S.; Capasso, R.; Gangkofner, C.; Gupta, N. and Liu, J. (2016): Stellar mass to halo mass scaling relation for X-ray-selected low-mass galaxy clusters and groups out to redshift z≈1. In: Monthly Notices of the Royal Astronomical Society, Vol. 458, No. 1: pp. 379-393

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We present the stellar mass halo mass scaling relation for 46 X-ray-selected low-mass clusters or groups detected in the XMM Newton Blanco Cosmology Survey (XMM-BCS) survey with masses 2 x 10(13) M-circle dot less than or similar to M-500 less than or similar to 2.5 x 10(14) M-circle dot (median mass 8 x 10(13) M-circle dot) at redshift 0.1 <= z <= 1.02 (median redshift 0.47). The cluster binding masses M-500 are inferred from the measured X-ray luminosities L-X, while the stellar masses M-star of the galaxy populations are estimated using near-infrared (NIR) imaging from the South Pole Telescope Deep Field survey and optical imaging from the BCS survey. With the measured L-X and stellar mass M-star, we determine the best-fitting 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 proportional to M-500(0.69 +/- 0.15) the intrinsic (lognormal) scatter is sigma(ln) (M star vertical bar M500) = 0.36(-0.06)(+0.07), and there is no significant redshift trend M-star proportional to (1 + Z)(-0.04 +/- 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 approximate to 93 per cent (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, Sunyaev Zel'dovich Effect selected clusters (M-500 approximate to 6 x 10(14) M-circle dot) and low-mass NIRselected clusters (M-500 approximate to 10(14) M-circle dot) at redshift 0.6 less than or similar to z less than or similar to 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 approximate to 1.

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