2016/10/07 by A. Sollima, E. Dalessandro, G. Beccari +2
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics #Astrophysics and Star Formation Studies #Cluster (spacecraft) #Galactic Center #Galaxy #Globular cluster #Hubble space telescope #Mass distribution #Mass segregation #Physics #Star cluster #Stars #Stellar, planetary, and galactic studies #astro-ph.GA #astro-ph.SR
paper · pdf · doi:10.1093/mnras/stw2628
12 pages, 7 figures, accepted for publication by MNRAS
arxiv created 2016/10/07 · openalex publication_date 2016/10/11 · openalex created_date 2016/10/21 · arxiv updated 2016/12/07 · openalex updated_date 2026/08/05
We present the results of the analysis of deep photometric data for a sample of three Galactic globular clusters (NGC5466, NGC6218 and NGC 6981) with the aim of estimating their degree of mass segregation and testing the predictions of analytic dynamical models. The adopted data set, composed of both Hubble Space Telescope and ground-based data, reaches the low-mass end of the mass functions of these clusters from the centre up to their tidal radii allowing us to derive the radial distribution of stars with different masses. All the analysed clusters show evidence of mass segregation with the most massive stars being more concentrated than the low-mass ones. The structures of NGC5466 and NGC6981 are well reproduced by multimass dynamical models adopting a lowered Maxwellian distribution function and the prescription for mass segregation given by Gunn & Griffin. Instead, NGC6218 appears to be more mass segregated than model predictions. By applying the same technique to mock observations derived from snapshots selected from suitable N-body simulations, we show that the deviation from the behaviour predicted by these models depends on the particular stage of dynamical evolution regardless of initial conditions.