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| Paper IPM / Astronomy / 15220 |
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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 ( ). The sample comprises 407 BGGs selected from X-ray galaxy groups ( ) out to 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 dex higher than the median SFR at . Both the mean and the median SFRs decline with time by dex. The mean (median) of stellar mass of BGGs has grown by dex since to the present day. We show that up to of the stellar mass growth in a star-forming BGG can be due to its star-formation activity. With respect to , we find it to increase with decreasing redshift by dex while decreasing with halo mass in a redshift dependent manner. We show that the slope of the relation between 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 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 and 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 ( ) and find that increases from 0.3 dex at to 0.5 dex at due to the bimodal distribution of stellar mass.
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