2013/07/23 by D. D. Carpintero, Daniel D. Carpintero, Facundo A. Gómez +2 · 1 citation
Physics and Astronomy · #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Cluster (spacecraft) #Demography #Galaxies: Formation, Evolution, Phenomena #Galaxy #Intergalactic travel #Large Magellanic Cloud #Metallicity #Physics #Population #Redshift #Small Magellanic Cloud #Star cluster #Star formation #Stellar, planetary, and galactic studies #astro-ph.GA
paper · pdf · doi:10.1093/mnrasl/slt096
5 pages, 3 figures, accepted for publication in MNRAS Letters
arxiv created 2013/07/23 · openalex publication_date 2013/08/21 · arxiv updated 2015/06/16 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/06
Abstract We model the dynamical interaction between the Small and Large Magellanic Clouds and their corresponding stellar cluster populations. Our goal is to explore whether the lack of old clusters (≳7 Gyr) in the Small Magellanic Cloud (SMC) can be the result of the capture of clusters by the Large Magellanic Cloud (LMC) as well as their ejection due to the tidal interaction between the two galaxies. For this purpose, we perform a suite of numerical simulations probing a wide range of parameters for the orbit of the SMC about the LMC. We find that, for orbital eccentricities e ≥ 0.4, approximately 15 per cent of the SMC clusters are captured by the LMC. In addition, another 20–50 per cent of its clusters are ejected into the intergalactic medium. In general, the clusters lost by the SMC are the less tightly bound cluster population. The final LMC cluster distribution shows a spatial segregation between clusters that originally belonged to the LMC and those that were captured from the SMC. Clusters that originally belonged to the SMC are more likely to be found in the outskirts of the LMC. Within this scenario, it is possible to interpret the difference observed between the star field and cluster SMC age–metallicity relationships for ages ≳7 Gyr.