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For refcode 1993AJ....106.2281A:
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1993AJ....106.2281A GLOBULAR CLUSTER CLUSTERING IN M31 KEITH M. ASHMAN AND CHRISTINA M. BIRD Canadian Institute for Theoretical Astrophysics, University of Toronto, 60 St. George Street, Toronto, Ontario M5S lAl Canada Electronic mail: ashman@kusmos.phsx.ukans.edu, tbird@kula.phsx.ukans.edu Received 1993 June 10; revised 1993 August 20 ABSTRACT We present an analysis of the positions and velocities of M31 globular clusters, which indicates the presence of significant substructure in the globular cluster system. We suggest this clustering is the surviving signature of gaseous clumps out of which the halo of M31 formed. A mixture-modeling analysis of the metallicity distribution of the M31 globulars indicates that, like the Milky Way, the metallicity distribution is bimodal. We show that the metallicity of genuine halo clusters in the Milky Way and M31 is similar to that of globulars around nearby dwarf galaxies. This suggests that such clusters formed from primordial material, whereas the disk globulars in the Galaxy and M31, as well as metal-rich globulars in elliptical galaxies, formed in some secondary event. Implications of these findings for formation models of galaxies and globular clusters are discussed.
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