2006/09/04 by Steffen Mieske, Andres Jordan, Patrick Cote +9 · 10 citations
Physics and Astronomy · #Astronomy and Astrophysical Research #Blue straggler #Cluster (spacecraft) #Galaxies: Formation, Evolution, Phenomena #Galaxy cluster #Galaxy groups and clusters #Globular cluster #Star cluster #Stellar, planetary, and galactic studies #Virgo Cluster #astro-ph
paper · pdf · doi:10.1086/508986
published as Astrophys.J.653:193-206,2006 · 15 pages, 12 figures, accepted for publication in the Astrophysical Journal. Uses emulateapj.cls
arxiv created 2006/09/04 · openalex publication_date 2006/12/05 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We examine the correlation between globular cluster (GC) color and magnitude using HST ACS imaging for a sample of 79 early-type galaxies (-21.7 < M B < -15.2 mag) with accurate SBF distances from the ACS Virgo Cluster Survey. Using the KMM mixture modeling algorithm, we find a highly significant correlation, γ z ≡ d ( g - z )/ dz = -0.037 ± 0.004, between color and magnitude for the subpopulation of blue GCs in the co-added GC color-magnitude diagram of the three brightest Virgo Cluster galaxies (M49, M87, and M60): brighter GCs are redder than their fainter counterparts. For the single GC systems of M87 and M60, we find similar correlations; M49 does not appear to show a significant trend. There is no correlation between ( g - z ) and M z for GCs of the red subpopulation. The correlation γ g ≡ d ( g - z )/ dg for the blue subpopulation is much weaker than d ( g - z )/ dz . Using Monte Carlo simulations, we attribute this finding to the fact that the blue subpopulation in M g extends to higher luminosities than does the red subpopulation, which biases the KMM fit results. The correlation between color and M z thus is a real effect: this conclusion is supported by biweight fits to the same color distributions. We identify two environmental dependencies that influence the derived color-magnitude relation: (1) the slope decreases in significance with decreasing galaxy luminosity; and (2) the slope is stronger for GC populations located at smaller galactocentric distances. We examine several physical mechanisms that might give rise to the observed color-magnitude relation: (1) presence of contaminators; (2) accretion of GCs from low-mass galaxies; (3) stochastic effects; (4) the capture of field stars by individual GCs; and (5) GC self-enrichment. We conclude that self-enrichment and field-star capture, or a combination of these processes, offer the most promising means of explaining our observations.