Volume 388, Number 2, June III 2002
|Page(s)||439 - 445|
|Section||Cosmology (including clusters of galaxies)|
|Published online||31 May 2002|
Dust-to-gas ratio and star formation history of blue compact dwarf galaxies
Osservatorio Astrofisico di Arcetri, Largo E. Fermi, 5, 50125 Firenze, Italy
2 Department of Astronomy, Faculty of Science, Kyoto University, Sakyo-ku, Kyoto 606-8502, Japan e-mail: tajiri, email@example.com
Corresponding author: H. Hirashita, firstname.lastname@example.org
Accepted: 29 March 2002
This paper investigates the origin of the observed large variety in dust-to-gas ratio, , among blue compact dwarf galaxies (BCDs). By applying our chemical evolution model, we find that the dust destruction can largely suppress the dust-to-gas ratio when the metallicity of a BCD reaches , i.e., a typical metallicity level of BCDs. We also show that dust-to-gas ratio is largely varied owing to the change of dust destruction efficiency that has two effects: (i) a significant contribution of Type Ia supernovae to total supernova rate; (ii) variation of gas mass contained in a star-forming region. While mass loss from BCDs was previously thought to be the major cause for the variance of , we suggest that the other two effects are also important. We finally discuss the intermittent star formation history, which naturally explains the large dispersion of dust-to-gas ratio among BCDs.
Key words: ISM: dust, extinction / galaxies: dwarf / galaxies: evolution / galaxies: ISM / stars: formation
© ESO, 2002
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