Abstract
We present a quantitative star formation history derivation of the four suspected tidal dwarf galaxies in the M 81 group: Holmberg IX, BK3N, Arp-loop (A0952 + 69) and Garland using HST/WFPC2 images of these galaxies. We construct a library of synthetic Colour-Magnitude Diagrams (CMDs) based on theoretical isochrones and data-derived determinations of photometric errors. These synthetic CMDs were combined linearly and X 2-compared to observed photometry. All the galaxies show continuous star formation between about 20 and 200 Myr ago with star formation rates between 7.5·10−3 M⊙/yr and 7.6·10−4 M⊙/yr. The metallicity of the detected stars is spanning rather a wide range, being lower than solar abundance. We suppose, that all the galaxies were formed out of material from metal-poor outer part of the giant spiral galaxy M81 after tidal interaction about 200 Myr ago. However, this suggestion requires significantly more deep color-magnitude diagrams to be sure with the scenario of the galaxy evolution.
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© 2003 Springer Science+Business Media Dordrecht
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Makarova, L. et al. (2003). Tidal Dwarfs in the M81 Group: The Second Generation?. In: Lobo, C., Serote Roos, M., Biviano, A. (eds) Galaxy Evolution in Groups and Clusters. Springer, Dordrecht. https://doi.org/10.1007/978-94-010-0107-6_14
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DOI: https://doi.org/10.1007/978-94-010-0107-6_14
Publisher Name: Springer, Dordrecht
Print ISBN: 978-94-010-3975-8
Online ISBN: 978-94-010-0107-6
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