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Nuclear clusters in dwarf irregular galaxies and their connection to massive galactic clusters

Published online by Cambridge University Press:  18 January 2010

Iskren Y. Georgiev ,
Michael Hilker ,
Thomas H. Puzia ,
Paul Goudfrooij  and
Holger Baumgardt
Iskren Y. Georgiev
Affiliation:
Argelander-Institut für Astronomie, Universität Bonn, Auf dem Hügel 71, 53121 Bonn, Germany Space Telescope Science Institute, Baltimore, MD, USA
Michael Hilker
Affiliation:
ESO, Garching, Germany
Thomas H. Puzia
Affiliation:
Dominion Astrophysical Observatory, Herzberg Institute of Astrophysics, National Research Council of Canada, Victoria, BC, Canada
Paul Goudfrooij
Affiliation:
Space Telescope Science Institute, Baltimore, MD, USA
Holger Baumgardt
Affiliation:
Argelander-Institut für Astronomie, Universität Bonn, Auf dem Hügel 71, 53121 Bonn, Germany
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Abstract

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We compare nuclear globular clusters (nGCs) in dwarf galaxies and Galactic GCs with extended (hot) horizontal branches (EHB–GCs) to test the suggested external origin of the latter and the conditions under which GC self-enrichment can operate. We show that the present-day escape velocity (vesc) of stellar ejecta to reach the cluster tidal radius compares with those of EHB–GCs. For EHB–GCs, we find a correlation between the present-day vesc and their metallicity as well as (V − I) colour. The similar vesc and (V − I) distribution of nGCs and EHB–GCs implies that nGCs could also have complex stellar populations. The vesc–[Fe/H] relation could reflect the known relation of increasing stellar-wind velocity with metallicity, which in turn explains why more metal-poor clusters typically show more peculiarities in their stellar population than more metal-rich clusters of the same mass.

Keywords

galaxies: star clustersgalaxies: dwarfgalaxies: nuclei
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S266: Star clusters: basic galactic building blocks throughout time and space , August 2009 , pp. 401
Copyright
Copyright © International Astronomical Union 2010