Tidal dwarfs in the M81 group: the second generation?

Details Tidal dwarfs in the M81 group: the second generation? Tidal dwarfs in the M81 group: the second generation?

2002-10-10

arxiv.org/abs/astro-ph/0210235v1

Astron.Astrophys. 396 (2002) 473-488; Astrophys.Space Sci. 285 (2003) 107-111

Astronomy and Astrophysics

Astrophysics

Scientific paper

10.1023/A:1024670028046

We derive quantitative star formation histories of the four suspected tidal dwarf galaxies in the M81 group, HolmbergIX, BK3N, Arp-loop (A0952+69), and Garland, using Hubble Space Telescope/Wide Field Planetary Camera2 images in F606W and F814W obtained as part of a Snapshot survey of dwarf galaxies in the Local Universe. We consider the spatial distribution and ages of resolved stellar populations in these dwarf irregular galaxies. We use synthetic color-magnitude diagrams to derive the ages of the major star formation episodes, star formation rates, and approximate metallicity ranges. All the galaxies show evidence of continuous star formation between about 20 and 200 Myr ago with star formation rates in the range 7.5*10^(-3)- 7.6*10^(-4) M(sun)/yr. The metallicity of the detected stars spans a wide range, and have lower than solar abundance. A possible scenario is that all four dwarf galaxies were formed from material in the metal-poor outer part of the giant spiral galaxy M81 after the tidal interaction between M81, M82, and NGC3077 about 200 Myr ago. While we do not directly detect pronounced old stellar populations, the photometric limits of our data are such that the presence of such a population is not entirely ruled out.

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