Permanent URL to this publication: http://dx.doi.org/10.5167/uzh-30876
Mapelli, M; Ripamonti, E; Battaglia, G; Tolstoy, E; Irwin, M J; Moore, B; Sigurdsson, S (2009). Blue straggler stars in dwarf spheroidal galaxies – II. Sculptor and Fornax. Monthly Notices of the Royal Astronomical Society, 396(3):1771-1782.
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The existence of blue straggler stars (BSSs) in dwarf spheroidal galaxies (dSphs) is still an open question. In fact, many BSS candidates have been observed in the Local Group dSphs, but it is unclear whether they are real BSSs or young stars. Shedding light on the nature of these BSS candidates is crucial in order to understand the star formation history of dSphs. In this paper, we consider BSS candidates in Sculptor and Fornax. In Fornax, there are strong hints that the BSS population is contaminated by young stars, whereas in Sculptor there is no clear evidence of recent star formation. We derive the radial and luminosity distribution of BSS candidates from wide field imaging data extending beyond the nominal tidal radius of these galaxies. The observations are compared with the radial distribution of BSSs expected from dynamical simulations. In Sculptor, the radial distribution of BSS candidates is consistent with that of red horizontal branch (RHB) stars and is in agreement with theoretical expectations for BSSs generated via mass transfer in binaries. On the contrary, in Fornax, the radial distribution of BSS candidates is more concentrated than that of all the considered stellar populations. This result supports the hypothesis that most of BSS candidates in Fornax are young stars, and this is consistent with previous studies.
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|Item Type:||Journal Article, refereed, original work|
|Communities & Collections:||07 Faculty of Science > Institute for Computational Science|
|Uncontrolled Keywords:||stellar dynamics; blue stragglers; galaxies: dwarf; galaxies: individual: Fornax; galaxies: individual: Sculptor|
|Deposited On:||26 Feb 2010 13:43|
|Last Modified:||27 Nov 2013 19:25|
|Additional Information:||The attached file is a preprint (accepted version) of an article published in Monthly Notices of the Royal Astronomical Society. The definitive version is available at www3.interscience.wiley.com|
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