Star formation history of galaxies from z = 0 to z = 0.7
A backward approach to the evolution of star-forming galaxies
Observatoire Astronomique Marseille Provence, Laboratoire d'Astrophysique de Marseille, BP 8, 13376 Marseille Cedex 12, France e-mail: email@example.com
2 Institute for Advanced Research, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8601, Japan
3 Spitzer fellow, Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822, USA
4 Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA
5 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
6 Faculty of Education, Nagasaki University, Nagasaki 852-8521, Japan
7 Faculty of Bussiness Administration, Tokyo Keizai University, 1-7-34, Minami-cho, Kokubunji, Tokyo, 185-8502, Japan
Accepted: 1 February 2008
Aims. We investigate whether the mean star formation activity of star-forming galaxies from to in the GOODS-S field can be reproduced by simple evolution models of these systems. In this case, such models might be used as first-order references for studies at higher z to decipher when and to what extent a secular evolution is sufficient to explain the star formation history in galaxies.
Methods. We selected star-forming galaxies at and at in IR and in UV to have access to all the recent star formation. We focused on galaxies with a stellar mass ranging between 1010 and for which the results are not biased by the selections. We compared the data to chemical evolution models developed for spiral galaxies and originally built to reproduce the main characteristics of the Milky Way and nearby spirals without fine-tuning them for the present analysis.
Results. We find a shallow decrease in the specific star formation rate (SSFR) when the stellar mass increases. The evolution of the SSFR characterizing both UV and IR selected galaxies from to is consistent with the models built to reproduce the present spiral galaxies. There is no need to strongly modify of the physical conditions in galaxies to explain the average evolution of their star formation from to . We use the models to predict the evolution of the star formation rate and the metallicity on a wider range of redshift and we compare these predictions with the results of semi-analytical models.
Key words: galaxies: evolution / galaxies: stellar content / infrared: galaxies / ultraviolet: galaxies
© ESO, 2008