2006/09/05 by P. Popesso, A. Biviano, M. Romaniello +1 · 38 citations
Physics and Astronomy · #Abell 2744 #Astronomy #Astronomy and Astrophysical Research #Astrophysics #Brightest cluster galaxy #Cluster (spacecraft) #Galaxies: Formation, Evolution, Phenomena #Galaxy #Galaxy cluster #Luminosity #Physics #Star formation #Stellar mass #Stellar, planetary, and galactic studies #Velocity dispersion #Virial mass #astro-ph
paper · pdf · doi:10.1051/0004-6361:20065357
published in Astronomy and Astrophysics 461(2), 411-421 (EDP Sciences) · 14 pages, 12 figures, accepted for publication on A&A; corrected coefficient in Tab. 2
arxiv created 2006/09/05 · openalex publication_date 2006/09/12 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/30
We aim at quantifying the relationships between star formation in cluster galaxies and global cluster properties. Using a subsample of 79 nearby clusters from the RASS-SDSS galaxy cluster catalogue of Popesso et al. (2005, A&A, 433, 431), we perform a regression analysis between the cluster integrated star formation rate (), the cluster total stellar mass (), the fractions of star forming (fSF) and blue (fb) galaxies and other cluster global properties, namely its richness (Ngal, i.e. the total number of cluster members within the cluster virial radius, corrected for incompleteness), velocity dispersion (), virial mass (M200), and X-ray luminosity (LX). All cluster global quantities are corrected for projection effects before the analysis. Galaxy s and stellar masses are taken from the catalog of Brinchmann et al. (2004), which is based on SDSS spectra. We only consider galaxies with in our analysis, and exclude AGNs. We find that both and are correlated with all the cluster global quantities. A partial correlation analysis shows that all the correlations are induced by the fundamental one between and Ngal, hence there is no evidence that the cluster properties affect the mean or per galaxy. The relations between and , on the one side, and both Ngal and M200, on the other side, are linear, i.e. we see no evidence that different clusters have different or different per galaxy and per unit mass. The fraction fSF does not depend on any cluster property considered, while fb does depend on LX. We note that a significant fraction of star-forming cluster galaxies are red (~25% of the whole cluster galaxy population). We conclude that the global cluster properties are unable to affect the properties of cluster galaxies, but the presence of the X-ray luminous intra-cluster medium can affect their colors, perhaps through the ram-pressure stripping mechanism.