The Initial Properties of Young Star Clusters in M83
arXiv:2012.07831 · doi:10.1093/mnras/staa3832
Abstract
The initial sizes and masses of massive star clusters provide information about the cluster formation process and also determine how cluster populations are modified and destroyed, which have implications for using clusters as tracers of galaxy assembly. Young massive cluster populations are often assumed to be unchanged since cluster formation, and therefore their distribution of masses and radii are used as the initial values. However, the first few hundred million years of cluster evolution does change both cluster mass and cluster radius, through both internal and external processes. In this paper, we use a large suite of -body cluster simulations in an appropriate tidal field to determine the best initial mass and initial size distributions of young clusters in the nearby galaxy M83. We find that the initial masses follow a power-law distribution with a slope of -2.7 0.4, and the half-mass radii follow a log-normal distribution with a mean of 2.57 0.04 pc and a dispersion of 1.59 0.01 pc. The corresponding initial projected half-light radius function has a mean of 2.7 0.3 pc and a dispersion of 1.7 0.2 pc. The evolution of the initial mass and size distribution functions are consistent with mass loss and expansion due to stellar evolution, independent of the external tidal field and the cluster's initial density profile. Observed cluster sizes and masses should not be used as the initial values, even when clusters are only a few hundred million years old.
8 pages, 6 figures, accepted for publication in MNRAS
References in corpus (11)
- Star cluster disruption by giant molecular clouds
- Legacy ExtraGalactic UV Survey (LEGUS) with The Hubble Space Telescope. I. Survey Description
- Black holes and core expansion in massive star clusters
- Probing the role of the galactic environment in the formation of stellar clusters; using M83 as a test bench
- Star clusters near and far; tracing star formation across cosmic time
- The GRIFFIN project -- Formation of star clusters with individual massive stars in a simulated dwarf galaxy starburst
- Sizes and Shapes of Young Star Cluster Light Profiles in M83
- A Gentle Introduction to the Kernel Distance
- Simulating radiative feedback and star cluster formation in GMCs: II. Mass dependence of cloud destruction and cluster properties
- The Effects of Orbital Inclination on the Scale Size and Evolution of Tidally Filling Star Clusters
- A tight relation between the age distributions of stellar clusters and the properties of the interstellar medium in the host galaxy