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The Star Formation History of the GRB 050730 Host Galaxy

Published online by Cambridge University Press:  01 June 2008

Francesco Calura
Francesco Calura*
Affiliation:
Dipartimento di Astronomia, Universita' di Trieste, via G. B. Tiepolo 11, 34131 TRIESTE - ITALY email: [email protected]
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Abstract

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The long GRB 050730 observed at redshift z ~ 4 allowed the determination of the elemental abundances for a set of different chemical elements. We use detailed chemical evolution models taking into account also dust production to constrain the star formation history of the host galaxy of this long GRB. For the host galaxy of GRB 050730, we derive also some dust-related quantities and the specific star formation rate, namely the star formation rate per unit stellar mass. Finally, we compare the properties of the GRB host galaxy with those of Quasar Damped Lyman Alpha absorbers.

Keywords

Gamma rays: burstsGalaxies: high-redshiftGalaxies: abundancesISM: general
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Issue S255: Low-Metallicity Star Formation: From the First Stars to Dwarf Galaxies , June 2008 , pp. 217 - 223
Copyright
Copyright © International Astronomical Union 2008

References

Bloom, J. S.; Djorgovski, S. G.; Kulkarni, S. R.; Frail, D. A., 1998, ApJ, 507, L25CrossRefGoogle Scholar
Bradamante, F., Matteucci, F., D'Ercole, A. 1998, A&A, 337, 338Google Scholar
Calura, F.; Pipino, A.; Matteucci, F., 2008, A&A, 479, 669 (CPM08)Google Scholar
Clayton Geoffrey, C., Green, J., Wolff, , Michael, J., Zellner, , Nicolle, E. B., Code, A. D., Davidsen, , Arthur, F., WUPPE Science Team, HUT Science Team, 1996, ApJ, 460 313CrossRefGoogle Scholar
Dessauges-Zavadsky, M.; Calura, F.; Prochaska, J. X.; D'Odorico, S.; Matteucci, F., 2004, A&A, 416, 79Google Scholar
Dessauges-Zavadsky, M.; Calura, F.; Prochaska, J. X.; D'Odorico, S.; Matteucci, F., 2007, A&A, 470, 431 (D07)Google Scholar
Edmunds, M. G., 2001, MNRAS, 328, 223CrossRefGoogle Scholar
Grevesse, N.; Asplund, M.; Sauval, A. J., 2007, SSRv, 130, 105Google Scholar
Jones, A. P., Tielens, A. G. G. M., Hollenbach, D. J., McKee, C. F., 1994, ApJ, 433, 797CrossRefGoogle Scholar
Iwamoto, K.; Brachwitz, F.; Nomoto, K.; Kishimoto, N.; Umeda, H.; Hix, W. R.; Thielemann, F.-K., 1999, ApJS, 125, 439CrossRefGoogle Scholar
Lanfranchi, G., Matteucci, F., 2003, MNRAS, 345, 71CrossRefGoogle Scholar
Matteucci, F., 1992, ApJ, 397, 32CrossRefGoogle Scholar
Matteucci, F., 2001, The chemical evolution of the Galaxy, Astrophysics and space science library, Volume 253, Dordrecht: Kluwer Academic PublishersGoogle Scholar
McKee, C. F., 1989, in Allamandola, L. J., Tielens, A. G. G. M., eds, Interstellar Dust, Proc. IAU Symposium 135. Kluwer, Dordrecht, p. 431CrossRefGoogle Scholar
Meynet, G., Maeder, A., 2002, A&A, 381, L25Google Scholar
Prochaska, J. X.; Bloom, J. S.; Chen, H.-W.; Hurley, K. C.; Melbourne, J.; Dressler, A.; Graham, J. R.; Osip, D. J.; Vacca, W. D., 2004, ApJ, 611, 200CrossRefGoogle Scholar
Prochaska, J. X.; Chen, H.-W.; Dessauges-Zavadsky, M.; Bloom, J. S., 2007, ApJ, 666, 267CrossRefGoogle Scholar
Savaglio, S., Fall, S. M., Fiore, F., 2003, ApJ, 585, 638CrossRefGoogle Scholar
Savaglio, S., Glazebrook, K., Le Borgne, D., 2008, ApJ, submitted, arXiv0803.271Google Scholar
Sugerman, B. E. K., et al. , 2006, Science, 313, 196CrossRefGoogle Scholar
Vreeswijk, P. M., et al. , 2004, A&A, 419, 927Google Scholar
Whalen, D., Prochaska, J. X., Heger, A., Tumlinson, J., 2008, ApJ, submittedGoogle Scholar
Woosley, S.E., Weaver, T.A., 1995, ApJS, 101, 181CrossRefGoogle Scholar