Volume 540, April 2012
|Number of page(s)||41|
|Section||Galactic structure, stellar clusters and populations|
|Published online||16 March 2012|
The ACS survey of Galactic globular clusters
XII. Photometric binaries along the main sequence⋆
1 Instituto de Astrofìsica de Canarias, 38200 La Laguna, Canary Islands, Spain
2 Department of Astrophysics, University of La Laguna, 38200 La Laguna, Tenerife, Canary Islands, Spain
3 Dipartimento di Astronomia, Università di Padova, Vicolo dell’Osservatorio 3, 35122 Padova, Italy
4 INAF – Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, 35122 Padova, Italy
5 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
6 Department of Astronomy, University of Florida, 211 Bryant Space Science Center, Gainesville, FL 32611, USA
7 Max Plank Institute for Astrophysics, Postfach 1317, 85741 Garching, Germany
8 Lund Observatory, Box 43, 221-00 Lund, Sweden
9 Department of Physics and Astronomy, Dartmouth College, 6127 Wilder Laboratory, Hanover, NH 03755, USA
10 Department of Physics and Astronomy, University of Victoria, PO Box 3055, STN CSC, Victoria, BC, V8W 3P6 Canada
11 P. Universidad Católica de Chile, Departamento de Astronomía y Astrofísica, Casilla 306, Santiago 22, Chile
12 Centro de Estudios de Física del Cosmos de Aragón (CEFCA), 44001 Teruel, Spain
13 Dept. of Astronomy, University of Virginia, PO Box 400325, Charlottesville, VA 22904-4325, USA
14 Department of Astronomy and Astrophysics, Pennsylvania State University, 525 Davey Laboratory, State College, PA 16801, USA
Received: 21 December 2010
Accepted: 31 October 2011
Context. The fraction of binary stars is an important ingredient to interpret globular cluster dynamical evolution and their stellar population.
Aims. We investigate the properties of main-sequence binaries measured in a uniform photometric sample of 59 Galactic globular clusters that were observed by HST WFC/ACS as a part of the Globular Cluster Treasury project.
Methods. We measured the fraction of binaries and the distribution of mass-ratio as a function of radial location within the cluster, from the central core to beyond the half-mass radius. We studied the radial distribution of binary stars, and the distribution of stellar mass ratios. We investigated monovariate relations between the fraction of binaries and the main parameters of their host clusters.
Results. We found that in nearly all the clusters, the total fraction of binaries is significantly smaller than the fraction of binaries in the field, with a few exceptions only. Binary stars are significantly more centrally concentrated than single MS stars in most of the clusters studied in this paper. The distribution of the mass ratio is generally flat (for mass-ratio parameter q > 0.5). We found a significant anti-correlation between the binary fraction in a cluster and its absolute luminosity (mass). Some, less significant correlation with the collisional parameter, the central stellar density, and the central velocity dispersion are present. There is no statistically significant relation between the binary fraction and other cluster parameters. We confirm the correlation between the binary fraction and the fraction of blue stragglers in the cluster.
Key words: techniques: photometric / binaries: general / stars: Population II / globular clusters: general
Tables 1–3 and Appendices are only available in electronic form at http://www.aanda.org
© ESO, 2012
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