The ACS Virgo Cluster Survey. XIV. Analysis of Color-Magnitude Relations in Globular Cluster Systems

• Published in: The Astrophysical journal 2006-12, Vol.653 (1), p.193-206
• Main Authors: Mieske, Steffen, Jordán, Andrés, Côté, Patrick, Kissler-Patig, Markus, Peng, Eric W, Ferrarese, Laura, Blakeslee, John P, Mei, Simona, Merritt, David, Tonry, John L, West, Michael J
• Format: Article
• Language: English
• Subjects: Astronomy; Earth, ocean, space; Exact sciences and technology
• ISSN: 0004-637X; 1538-4357
• DOI: 10.1086/508986

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 sub(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, g sub(z) = d(g - z)ldz = -0.037 c 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 sub(z) for GCs of the red subpopulation. The correlation g sub(g) = d(g - z)/dg for the blue subpopulation is much weaker than d(g - z)ldz. Using Monte Carlo simulations, we attribute this finding to the fact that the blue subpopulation in M extends to higher luminosities than does the red subpopulation, which biases the KMM fit results. The correlation between color and M sub(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.