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Title:
Evidence for top-heavy stellar initial mass functions with increasing density and decreasing metallicity [ Erratum: 2014MNRAS.442.3315M ]
Authors:
Marks, Michael; Kroupa, Pavel; Dabringhausen, Jörg; Pawlowski, Marcel S.
Affiliation:
AA(Argelander Institute for Astronomy, University of Bonn, Auf dem Hügel 71, 53121 Bonn, Germany; Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, D-53121 Bonn, Germany), AB(Argelander Institute for Astronomy, University of Bonn, Auf dem Hügel 71, 53121 Bonn, Germany), AC(Argelander Institute for Astronomy, University of Bonn, Auf dem Hügel 71, 53121 Bonn, Germany), AD(Argelander Institute for Astronomy, University of Bonn, Auf dem Hügel 71, 53121 Bonn, Germany)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 422, Issue 3, pp. 2246-2254. (MNRAS Homepage)
Publication Date:
05/2012
Origin:
WILEY
Astronomy Keywords:
stars: early-type, stars: formation, stars: late-type, stars: luminosity function, mass function, globular clusters: general
Abstract Copyright:
© 2012 The Authors Monthly Notices of the Royal Astronomical Society © 2012 RAS
DOI:
10.1111/j.1365-2966.2012.20767.x
Bibliographic Code:
2012MNRAS.422.2246M

Abstract

Residual-gas expulsion after cluster formation has recently been shown to leave an imprint in the low-mass present-day stellar mass function (PDMF) which allowed the estimation of birth conditions of some Galactic globular clusters (GCs) such as mass, radius and star formation efficiency. We show that in order to explain their characteristics (masses, radii, metallicity and PDMF) their stellar initial mass function (IMF) must have been top heavy. It is found that the IMF is required to become more top heavy the lower the cluster metallicity and the larger the pre-GC cloud-core density are. The deduced trends are in qualitative agreement with theoretical expectation. The results are consistent with estimates of the shape of the high-mass end of the IMF in the Arches cluster, Westerlund 1, R136 and NGC 3603, as well as with the IMF independently constrained for ultra-compact dwarf galaxies (UCDs). The latter suggests that GCs and UCDs might have formed along the same channel or that UCDs formed via mergers of GCs. A Fundamental Plane is found which describes the variation of the IMF with density and metallicity of the pre-GC cloud cores. The implications for the evolution of galaxies and chemical enrichment over cosmological times are expected to be major.

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