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Properties of a Gamma-Ray Burst Host Galaxy at z ~ 5*

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Published 18 June 2007 • © 2007. The American Astronomical Society. All rights reserved. Printed in U.S.A.
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Author affiliations

1 Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822

2 Astrophysics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH, UK

3 Observatories of the Carnegie Institution of Washington, 813 Santa Barbara Street, Pasadena, CA 91101

4 Department of Astronomy and Astrophysics, Pennsylvania State University, 525 Davey Laboratory, University Park, PA 16802

5 Mail Code 105-24, Astronomy, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125

6 Pomona College, 610 North College Avenue, Claremont, CA 91711

7 Gemini Observatory, 670 North A'ohoku Street, Hilo, HI 96720

8 Research School of Astronomy and Astrophysics, Australian National University, Mount Stromlo Observatory, Cotter Road, Weston Creek, Canberra, ACT 2611, Australia

Dates

Received 29 March 2007
Accepted 22 May 2007
Published

Citation

P. A. Price et al 2007 ApJ 663 L57

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DOI

https://doi.org/10.1086/520047

Keywords

cosmology: observations; galaxies: abundances; galaxies: distances and redshifts; galaxies: evolution; gamma rays: bursts

Journal RSS feed

1538-4357/663/2/L57

Abstract

We describe the properties of the host galaxy of the gamma-ray burst GRB 060510B based on a spectrum of the burst afterglow obtained with the Gemini North 8 m telescope. The galaxy lies at a redshift of z = 4.941, making it the fourth highest spectroscopically identified burst host. However, it is the second highest redshift galaxy for which the quality of the spectrum permits a detailed metallicity analysis. The neutral hydrogen column density has a logarithmic value of 21.0-21.2 cm-2, and the weak metal lines of Ni, S, and Fe show that the metallicity is in excess of a tenth of solar, which is far above the metallicities in damped Lyα absorbers at high redshift. The tightest constraint is from the Fe lines, which place [Fe/H] in excess of -0.8. We argue that the results suggest that metallicity bias could be a serious obstacle to inferring star formation from the GRB population, and we consider how future higher quality measurements could be used to resolve this issue.

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  • * 

    Based on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini Partnership: the National Science Foundation (US), the Particle Physics and Astronomy Research Council (UK), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), CNPq (Brazil), and CONICET (Argentina)

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