Baryon content of massive galaxy clusters at 0.57

• Main Authors: Chiu, I (Author), Mohr, J (Author), McDonald, M (Author), Bocquet, S (Author), Ashby, MLN (Author), Bayliss, M (Author), Benson, BA (Author), Bleem, LE (Author), Brodwin, M (Author), Desai, S (Author), Dietrich, JP (Author), Forman, WR (Author), Gangkofner, C (Author), Gonzalez, AH (Author), Hennig, C (Author), Liu, J (Author), Reichardt, CL (Author), Saro, A (Author), Stalder, B (Author), Stanford, SA (Author), Song, J (Author), Schrabback, T (Author), Šuhada, R (Author), Strazzullo, V (Author), Zenteno, A (Author)
• Format: Article
• Language: English
• Published: Oxford University Press (OUP), 2021-10-27T20:04:08Z.
• Subjects: Article
• Online Access: Get fulltext

 © 2015 The Authors. We study the stellar, brightest cluster galaxy (BCG) and intracluster medium (ICM) masses of 14 South Pole Telescope (SPT) selected galaxy clusters with median redshift z = 0.9 and mass M500 = 6 × 1014M⊙. We estimate stellar masses for each cluster and BCG using six photometric bands, the ICM mass using X-ray observations and the virial masses using the SPT Sunyaev-Zel'dovich effect signature. At z = 0.9, the BCG mass M*BCG constitutes 0.12 ± 0.01 per cent of the halo mass for a 6 × 1014M⊙ cluster, and this fraction falls as M 500-0.58±0.07. The cluster stellar mass function has a characteristic mass M0 = 1011.0 ± 0.1M⊙, and the number of galaxies per unit mass in clusters is larger than in the field by a factor of 1.65 ± 0.20. We combine our SPT sample with previously published samples at low redshift and correct to a common initial mass function and for systematic virial mass differences. We then explore mass and redshift trends in the stellar fraction f*, the ICM fraction fICM, the collapsed baryon fraction fc and the baryon fraction fb. At a pivot mass of 6 × 1014M⊙ and redshift z = 0.9, the characteristic values are f* = 1.1 ± 0.1 per cent, fICM = 9.6 ± 0.5 per cent, fc = 10.7 ± 1.1 per cent and fb = 10.7 ± 0.6 per cent. These fractions all vary with cluster mass at high significance, with higher mass clusters having lower f* and fc and higher fICM and fb. When accounting for a 15 per cent systematic virial mass uncertainty, there is no statistically significant redshift trend at fixed mass. Our results support the scenario where clusters grow through accretion from subclusters (higher f*, lower fICM) and the field (lower f*, higher fICM), balancing to keep f* and fICM approximately constant since z ~ 0.9.