2011/08/29 by E. Dalessandro, B. Lanzoni, G. Beccari +3
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysical Phenomena and Observations #Binary number #Binary star #Cluster (spacecraft) #Core (optical fiber) #Globular cluster #Mass segregation #RADIUS #Star cluster #Stars #Stellar, planetary, and galactic studies #astro-ph.SR
paper · pdf · doi:10.1088/0004-637x/743/1/11
Accepted for publication in ApJ (22 pages, 7 figures, 3 tables)
arxiv created 2011/08/29 · openalex publication_date 2011/11/17 · arxiv updated 2015/05/29 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We study the binary fraction of the globular cluster M10 (NGC 6254) as a function of the radius from the cluster core to the outskirts, by means of a quantitative analysis of the color distribution of stars relative to the fiducial main sequence. By taking advantage of two data sets, acquired with the Advanced Camera for Survey and the Wide Field Planetary Camera 2 on board the Hubble Space Telescope , we have studied both the core and the external regions of the cluster. The binary fraction is found to decrease from ∼14% within the core, to ∼1.5% in a region between 1 and 2 half-mass radii from the cluster center. Such a trend and the derived values are in agreement with previous results obtained in clusters of comparable total magnitude. The estimated binary fraction is sufficient to account for the suppression of mass segregation observed in M10, without any need to invoke the presence of an intermediate-mass black hole in its center.