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Date and Time of the Query: 2019-06-26 T16:10:17 PDT
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For refcode 1999AJ....118.1526G:
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1999AJ....118.1526G GLOBULAR CLUSTER SYSTEMS. I. V-I COLOR DISTRIBUTIONS KARL GEBHARDT UCO/Lick Observatory, University of California, Santa Cruz, CA 95064; gebhardt@ucolick.org AND MARKUS KISSLER-PATIG European Southern Observatory, Karl-Schwarzschild-Strasse 2, D-85748 Garching, Germany; and UCO/Lick Observatory, University of California, Santa Cruz, CA 95064; mkissler@eso.org Received 1999 May 20; accepted 1999 June 15 ABSTRACT We have compiled data for the globular cluster systems of 50 galaxies from the Hubble Space Telescope Wide Field Planetary Camera 2 archive, of which 43 are type S0 or earlier. In this paper, we present the data set and derive the V-I color distributions. We derive the first four moments of the color distributions, as well as a measure for their nonunimodality. The number of globular clusters in each galaxy ranges from 18 (in NGC 2778) to 781 (NGC 5846). For those systems having more than 100 clusters, seven of 16 (44%) show significant bimodality. Overall, roughly half of all the systems in our sample show hints of a bimodal color distribution. In general, the distributions of the faint galaxies are consistent with unimodality, whereas those of the brighter galaxies are not. We also find a number of systems with narrow color distributions-with both mean red and blue colors-suggesting that systems exist with only metal-rich or only metal-poor globular clusters. We discuss their possible origins. In comparing the moments of the V-I distributions with various galaxy properties for the early-type galaxies, we find the following difference in the correlations between the field and cluster galaxy populations: the peak V-I color of the globular cluster distribution correlates well with the central velocity dispersion-and hence the Mg_2_ index and total luminosity- for galaxies in cluster environments; there exists no such correlation for field galaxies. This difference between cluster and field galaxies possibly reflects different formation scenarios for their globular cluster systems. Among the explanations for such a correlation, we consider either a larger age spread in the field populations or the possibility that cluster galaxies are always affected by significant accretion whereas some field galaxies could host pure "in situ" formed populations. Key words: galaxies: elliptical and lenticular, cD-galaxies: star clusters
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