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

• 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: Text
• Language: English
• Published: Oxford University Press 2016
• Subjects: Article; South Pole; Blanco; South pole
• Online Access: http://mnras.oxfordjournals.org/cgi/content/short/458/1/379; https://doi.org/10.1093/mnras/stw292

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 ⊙ ≲ M 500 ≲ 2.5 × 1014 M ⊙ (median mass 8 × 1013 M ⊙ ) 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 ⋆ 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 ⋆ , 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 <f>$M_{\star }\propto M_{500}^{0.69\pm 0.15}$</f>, the intrinsic (lognormal) scatter is <f>$\sigma _{\ln M_{\star }|M_{500}}=0.36^{+0.07}_{-0.06}$</f>, 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 M 500 ). We compare our M ⋆ = M ⋆ ( M 500 , z ) scaling relation from the XMM -BCS clusters with samples of massive, Sunyaev–Zel'dovich Effect selected clusters ( M 500 ≈ 6 × 1014 M ⊙ ) and low-mass NIR-selected clusters ( M 500 ≈ 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 R 500 depends strongly on mass but only weakly on redshift out to z ≈ 1.