EAS Publications Series
Volume 56, 2012The Role of the Disk-Halo Interaction in Galaxy Evolution: Outflow vs. Infall?
|Page(s)||305 - 308|
|Section||The Active Disk-Halo Connection: Infall vs. Outflows|
|Published online||17 September 2012|
Miguel A. de Avillez (ed)
EAS Publications Series, 56 (2012) 305–308
The Interplay Between Globular Clusters and the Halo and Disk
1 Astrophysics Group, Lennard-Jones Laboratories, Keele University, Staffordshire, ST5 5BG, UK
2 Department of Astronomy, School of Physics and Astronomy, 116 Church Street, S.E., University of Minnesota, Minneapolis, MN 55455, USA
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.
© EAS, EDP Sciences, 2012