A MATURE DUSTY STAR-FORMING GALAXY HOSTING GRB 080607 AT z = 3.036
- Department of Astronomy and Astrophysics and Kavli Institute for Cosmological Physics, University of Chicago, Chicago, IL 60637 (United States)
- Department of Astronomy, 601 Campbell Hall, University of California, Berkeley, CA 94720 (United States)
- Department of Physics and Astronomy, McMaster University, Hamilton, Ontario, L8S 4M1 (Canada)
- Department of Physics, University of Warwick, Coventry CV4 7AL (United Kingdom)
- UCO/Lick Observatory, University of California, Santa Cruz, CA 95064 (United States)
- Department of Physics and Astronomy, University of Leicester, University Road, Leicester LE1 7RH (United Kingdom)
- Observatoire de Geneve, 51 Ch. des Maillettes, 1290 Sauverny (Switzerland)
- Institute of Astronomy, Madingley Rd., Cambridge CB3 0HA (United Kingdom)
We report the discovery of the host galaxy of Swift dark burst GRB 080607 at z {sub GRB} = 3.036. GRB 080607 is a unique case of a highly extinguished (A{sub V} {approx} 3 mag) afterglow that was yet sufficiently bright for high-quality absorption-line spectroscopy. The host galaxy is clearly resolved in deep Hubble Space Telescope (HST) WF3/IR F160W images and well detected in the Spitzer IRAC 3.5 {mu}m and 4.5 {mu}m channels, while displaying little/no fluxes in deep optical images from Keck and Magellan. The extremely red optical-infrared colors are consistent with the large extinction seen in the afterglow light, suggesting that the large amount of dust and gas surface mass density seen along the afterglow sight line is not merely local but likely reflects the global dust content across the entire host galaxy. Adopting the dust properties and metallicity of the host interstellar medium derived from studies of early-time afterglow light and absorption-line spectroscopy, we perform a stellar population synthesis analysis of the observed spectral energy distribution to constrain the intrinsic luminosity and stellar population of this dark burst host. The host galaxy is best described by an exponentially declining star formation rate of e-folding time {tau} = 2 Gyr and an age of {approx}2 Gyr. We also derive an extinction-corrected star formation rate of SFR {approx} 125 h {sup -2} M {sub sun} yr{sup -1} and a total stellar mass of M {sub *} {approx} 4 x 10{sup 11} h {sup -2} M {sub sun}. Our study provides an example of massive, dusty star-forming galaxies contributing to the {gamma}-ray burst (GRB) host galaxy population, supporting the notion that long-duration GRBs trace the bulk of cosmic star formation.
- OSTI ID:
- 21452688
- Journal Information:
- Astrophysical Journal Letters, Vol. 723, Issue 2; Other Information: DOI: 10.1088/2041-8205/723/2/L218; ISSN 2041-8205
- Country of Publication:
- United States
- Language:
- English
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