2008/06/09 by F. Bournaud, P. -A. Duc, P.-A. Duc +1
Physics and Astronomy · #Astronomy and Astrophysical Research #Galaxies: Formation, Evolution, Phenomena #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1111/j.1745-3933.2008.00511.x
MNRAS letters accepted. Version with high-resolution figures available at http://aramis.obspm.fr/~bournaud/GC.pdf
arxiv created 2008/06/09 · openalex publication_date 2008/07/08 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/07/28
Abstract Massive star clusters observed in galaxy mergers are often suggested to be progenitors of globular clusters. To study this hypothesis, we performed the highest resolution simulation of a gas-rich galaxy merger so far. The formation of massive star clusters of 105 to 107 M⊙, triggered by the galaxy interaction, is directly resolved in this model. We show that these clusters are tightly bound structures with little net rotation, due to evolve into compact long-lived stellar systems. Massive clusters formed in galaxy mergers are thus robust candidates for progenitors of long-lived globular clusters. The simulated cluster mass spectrum is consistent with theory and observations. Tidal dwarf galaxies of 108–9 M⊙ can form at the same time, and appear to be part of a different class of objects, being more extended and rotating.