Stellar mass to halo mass scaling relation for X-ray-selected low-mass galaxy clusters and groups out to redshift z≈1

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 × 1013 M☉ ≲ M500 ≲ 2.5 × 1014 M☉ (median mass 8 × 1013 M☉) at redshift 0.1 ≤ z ≤ 1.02 (median redshift 0.47). The...

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Bibliographic Details
Published in:Monthly Notices of the Royal Astronomical Society
Main Authors: Chiu, I., Saro, A., Mohr, J., Desai, S., Bocquet, S., Capasso, R., Gangkofner, C., Gupta, N., Liu, J.
Format: Article in Journal/Newspaper
Language:English
Published: 2016
Subjects:
Online Access:http://hdl.handle.net/11368/2962590
https://doi.org/10.1093/mnras/stw292
https://academic.oup.com/mnras/article/458/1/379/2622880
Description
Summary: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 × 1013 M☉ ≲ M500 ≲ 2.5 × 1014 M☉ (median mass 8 × 1013 M☉) at redshift 0.1 ≤ z ≤ 1.02 (median redshift 0.47). The cluster binding masses M500 are inferred from the measured X-ray luminosities LX, while the stellar masses M⋆ 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 LX and stellar mass M⋆, 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 }∝ M_{500}^{0.69± 0.15}, the intrinsic (lognormal) scatter is σ _{ln M_{star }|M_{500}}=0.36^{+0.07}_{-0.06}, and there is no significant redshift trend M⋆ ∝ (1 + z)-0.04 ± 0.47, although the uncertainties are still large. We also examine M⋆ within a fixed projected radius of 0.5 Mpc, showing that it provides a cluster binding mass proxy with intrinsic scatter of ≈93 per cent (1σ in M500). We compare our M⋆ = M⋆(M500, z) scaling relation from the XMM-BCS clusters with samples of massive, Sunyaev-Zel'dovich Effect selected clusters (M500 ≈ 6 × 1014 M☉) and low-mass NIR-selected clusters (M500 ≈ 1014 M☉) at redshift 0.6 ≲ z ≲ 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 R500 depends strongly on mass but only weakly on redshift out to z ≈ 1.