Published in "Globular Clusters", 1999, Cambridge
University Press
GLOBULAR CLUSTER SYSTEMS: FORMATION MODELS AND CASE STUDIES
William E. Harris
Department
of Physics & Astronomy, McMaster University, Hamilton ON L8S 4M1 Canada
Abstract. Globular cluster systems represent only a small
fraction of the
total stellar mass of galaxy halos, but provide unique tracers
which can be used to address models of galaxy formation.
Several "case studies" of individually important galaxies
are presented, in which we look at the characteristics of their
globular clusters including the metallicity distributions,
specific frequencies,
luminosity (mass) distributions, and kinematics. Among these
galaxies are the Milky Way, the nearby giant elliptical NGC 5128,
the Virgo ellipticals NGC 4472 and M87, and the supergiant
cD galaxies at the centers of rich clusters. In each case the
possible roles of mergers, small-satellite accretions, and
in situ formation in the growth of the galaxy are discussed.
We also briefly touch on the connection between the globular clusters
and the much more numerous field-halo stars. We conclude that
in all formation scenarios, the presence or absence of gas at any
stage of the galaxy's evolution plays
a crucial role in determining the total cluster population, the
number of distinguishable subpopulations, and the metallicity
distribution of the clusters.
Table of Contents
CASE STUDIES: THE MILKY WAY GCS
- INTERLUDE: SYSTEMIC PROPERTIES IN OTHER
GALAXIES
- Specific Frequencies
- Metallicity Distributions
- Luminosity and Mass Distributions
- CASE STUDIES: NGC 5128
- CASE STUDIES: NGC 4472 AND M87
- Velocities and Kinematics
- MDFs and Specific Frequencies: How Many
Components?
- Merger Scenarios
- Accretion Scenarios
- CASE STUDIES: THE BRIGHTEST CLUSTER ELLIPTICALS
- The Role of the Halo Gas: Understanding High
SN
- The Coma Ellipticals: New Anomalies and
Challenges
- A BRIEF SYNTHESIS
- REFERENCES
