Stellar mass–halo mass relation for the brightest central galaxies of X-ray clusters since z ∼ 0.65

¹ Max Planck institute for extraterrestrial physics, Garching by Munich, Germany
e-mail: erfanian@mpe.mpg.de
² University of Helsinki, Department of Physics, PO Box 64, 00014 Helsinki, Finland
³ Astrophysics Research Institute, Liverpool John Moores University, IC2, Liverpool Science Park, 146 Brownlow Hill, Liverpool L3 5RF, UK
⁴ Excellence Cluster Universe, Boltzmannstr. 2, 85748 Garching bei München, Germany
⁵ INAF/Osservatorio Astronomico di Trieste, Via G. B. Tiepolo 11, 34131 Trieste, Italy
⁶ Department of Physics, University of Bath, Claverton Down, Bath BA2 7AY, UK
⁷ School of Astronomy, Institute for Research in Fundamental Sciences (IPM), Tehran 19395-5531, Iran
⁸ Faculty of Physics, Ludwig-Maximilians-Universität, Scheinerstr. 1, 81679 Munich, Germany
⁹ Kavli Institute for Particle Astrophysics & Cosmology, Stanford University, PO Box 2450, Stanford, CA 94305, USA
¹⁰ SLAC National Accelerator Laboratory, Menlo Park, CA 94025, USA
¹¹ IRAP, Université de Toulouse, CNRS, UPS, CNES, Toulouse, France
¹² Finnish centre for Astronomy with ESO (FINCA), University of Turku, Quantum, Vesilinnantie 5, 20014 Turku, Finland
¹³ Helsinki Institute of Physics, University of Helsinki, PO Box 64, 00014 Helsinki, Finland
¹⁴ School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews KY16 9SS, UK
¹⁵ Department of Physics and Astronomy, University of Utah, 115 S. 1400 E., Salt Lake City, UT 84112, USA
¹⁶ Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA
¹⁷ Department of Astronomy and Astrophysics, The Pennsylvania State University, University Park, PA 16802, USA
¹⁸ Institute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, PA 16802, USA

Received: 26 February 2019
Accepted: 12 July 2019

Abstract

We present the brightest cluster galaxies (BCGs) catalog for SPectroscoic IDentification of eROSITA Sources (SPIDERS) DR14 cluster program value-added catalog. We list the 416 BCGs identified as part of this process, along with their stellar mass, star formation rates (SFRs), and morphological properties. We identified the BCGs based on the available spectroscopic data from SPIDERS and photometric data from SDSS. We computed stellar masses and SFRs of the BCGs on the basis of SDSS, WISE, and GALEX photometry using spectral energy distribution fitting. Morphological properties for all BCGs were derived by Sersic profile fitting using the software package SIGMA in different optical bands (g,r,i). We combined this catalog with the BCGs of galaxy groups and clusters extracted from the deeper AEGIS, CDFS, COSMOS, XMM-CFHTLS, and XMM-XXL surveys to study the stellar mass–halo mass relation using the largest sample of X-ray groups and clusters known to date. This result suggests that the mass growth of the central galaxy is controlled by the hierarchical mass growth of the host halo. We find a strong correlation between the stellar mass of BCGs and the mass of their host halos. This relation shows no evolution since z ∼ 0.65. We measure a mean scatter of 0.21 and 0.25 for the stellar mass of BCGs in a given halo mass at low (0.1 <  z <  0.3) and high (0.3 <  z <  0.65) redshifts, respectively. We further demonstrate that the BCG mass is covariant with the richness of the host halos in the very X-ray luminous systems. We also find evidence that part of the scatter between X-ray luminosity and richness can be reduced by considering stellar mass as an additional variable.