Formation of Globular Clusters in Merging Galaxies
| dc.creator | Schweizer, Francois | |
| dc.date | 2002-12-10 | |
| dc.date.accessioned | 2026-07-07T02:06:49Z | |
| dc.date.available | 2026-07-07T02:06:49Z | |
| dc.description | Collisions and mergers of gas-rich galaxies trigger bursts of star and cluster formation. Of the thousands of clusters typically formed during a major merger, only the most massive and compact survive for Gigayears as globular clusters (GCs). In <~1 Gyr old merger remnants, these `second-generation' GCs appear by the hundreds as young halo clusters of about solar metallicity. Their likely descendants, metal-rich GCs of intermediate age (2 - 5 Gyr), have recently been found in ~10 elliptical galaxies, where they appear as slightly overluminous red GCs with a still power-law-like luminosity function. Their color and radial distributions suggest that they evolve into the red metal-rich GCs observed in old ellipticals. There is good evidence that second-generation GCs form from giant molecular clouds shocked by the rapid pressure increase in merger-induced starbursts. This mechanism supports the view that the universal pressure increase during cosmological reionization may have triggered the formation of the metal-poor globulars observed in galaxies of all types. | |
| dc.description | 11 pages, LaTeX, 6 figures (= 10 EPS files); uses newpasp.sty. To appear in "New Horizons in Globular Cluster Astronomy," eds. G. Piotto, G. Meylan, G. Djorgovski, & M. Riello (ASP, San Francisco), 2003 | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0212243 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0212243 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/5495 | |
| dc.subject | Astrophysics | |
| dc.title | Formation of Globular Clusters in Merging Galaxies | |
| dc.type | text |