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The Interplay Between Globular Clusters and the Halo and Disk

Published online by Cambridge University Press:  17 September 2012

I. McDonald ,
J.Th. van Loon  and
M.L. Boyer
I. McDonald
Affiliation:
Astrophysics Group, Lennard-Jones Laboratories, Keele University, Staffordshire, ST5 5BG, UK
J.Th. van Loon
Affiliation:
Astrophysics Group, Lennard-Jones Laboratories, Keele University, Staffordshire, ST5 5BG, UK
M.L. Boyer
Affiliation:
Department of Astronomy, School of Physics and Astronomy, 116 Church Street, S.E., University of Minnesota, Minneapolis, MN 55455, USA
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Abstract

Globular clusters (GC) are powerful tools to analyse the Halo environment: spread throughout the Halo at distances of 2– 122 kpc, moving with space velocities of ∼200 km s−1, they provide unique tracers of local Halo conditions. Each cluster enriches the Halo with several M⊙ Myr−1 through stellar winds. The interaction of these winds with the Halo can be used as a probe of the local Halo environment.

Using spectral energy distributions of 6875 stars in the GC ω Cen, we quantify the cluster’s total mass loss. Comparing this to observed limits on intra-cluster material (ICM), we find the ICM is being cleared from these clusters on timescales of <105 yr. We also present new 21 cm observations of the high velocity H i cloud near ω Cen in the context of recent Spitzer observations, discussing its structure and likely associations.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 56: The Role of the Disk-Halo Interaction in Galaxy Evolution: Outflow vs. Infall? , 2012 , pp. 305 - 308
Copyright
© EAS, EDP Sciences, 2012

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