Brightest group galaxies-II: the relative contribution of BGGs to the total baryon content of groups at z<1.3

Abstract

We performed a detailed study of the evolution of the star formation rate (SFR) and stellar mass of the brightest group galaxies (BGGs) and their relative contribution to the total baryon budget within $R_{200}$ ($f_{b,200}^{BGG}$). The sample comprises 407 BGGs selected from X-ray galaxy groups ($M_{200}=10^{12.8}-10^{14}{M}_{\odot }$) out to $z\sim 1.3$ identified in the COSMOS, XMM-LSS, and AEGIS fields. We find that BGGs constitute two distinct populations of quiescent and star-forming galaxies and their mean SFR is $\sim 2$ dex higher than the median SFR at $z<1.3$. Both the mean and the median SFRs decline with time by $>2$ dex. The mean (median) of stellar mass of BGGs has grown by $0.3$ dex since $z=1.3$ to the present day. We show that up to $\sim 45\%$ of the stellar mass growth in a star-forming BGG can be due to its star-formation activity. With respect to $f_{b,200}^{BGG}$, we find it to increase with decreasing redshift by $\sim 0.35$ dex while decreasing with halo mass in a redshift dependent manner. We show that the slope of the relation between $f_{b,200}^{BGG}$ and halo mass increases negatively with decreasing redshift. This trend is driven by an insufficient star-formation in BGGs, compared to the halo growth rate. We separately show the BGGs with the 20\% highest $f_{b,200}^{BGG}$ are generally non-star-forming galaxies and grow in mass by processes not related to star formation (e.g., dry mergers and tidal striping). We present the $M_{\star }-M_h$ and $M_{\star }/M_h-M_h$ relations and compare them with semi-analytic model predictions and a number of results from the literature. We quantify the intrinsic scatter in stellar mass of BGGs at fixed halo mass (${\sigma }_{log{M}_{\star }}$) and find that ${\sigma }_{log{M}_{\star }}$ increases from 0.3 dex at $z\sim 0.2$ to 0.5 dex at $z\sim 1.0$ due to the bimodal distribution of stellar mass.

Accepted for publication in MNRAS, 25 pages, 11 figures

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• ALMA measures molecular gas reservoirs comparable to field galaxies in a low-mass galaxy cluster at z=1.3
• Star formation quenching precedes morphological transformation in COSMOS-WEB's richest galaxy groups
• Forged by Feedback: Stellar Properties of Brightest Group Galaxies in Cosmological Simulations