The luminous, massive and solar metallicity galaxy hosting the Swift γ-ray burst GRB 160804A at z = 0.737

Journal
Date Issued
2018
Author(s)
Heintz, K. E.
•
Malesani, D.
•
Wiersema, K.
•
Jakobsson, P.
•
Fynbo, J. P. U.
•
Savaglio, S.
•
Cano, Z.
•
•
D'Elia, V.
•
Gomboc, A.
•
Hammer, F.
•
Kaper, L.
•
Milvang-Jensen, B.
•
Møller, P.
•
•
Selsing, J.
•
Rhodin, N. H. P.
•
Tanvir, N. R.
•
Thöne, C. C.
•
de Ugarte Postigo, A.
•
Vergani, S. D.
•
Watson, D.
DOI
Abstract
We here present the spectroscopic follow-up observations with VLT/X-shooter of the Swift long-duration gamma-ray burst GRB 160804A at z = 0.737. Typically, GRBs are found in low-mass, metal-poor galaxies that constitute the sub-luminous population of star-forming galaxies. For the host galaxy of the GRB presented here, we derive a stellar mass of log (M*/ M☉) = 9.80 ± 0.07, a roughly solar metallicity (12 + log (O/H) = 8.74 ± 0.12) based on emission line diagnostics, and an infrared luminosity of M3.6/(1 + z) = -21.94 mag, but find it to be dust-poor (E(B - V) < 0.05 mag). This establishes the galaxy hosting GRB 160804A as one of the most luminous, massive and metal-rich GRB hosts at z < 1.5. Furthermore, the gas-phase metallicity is found to be representative of the physical conditions of the gas close to the explosion site of the burst. The high metallicity of the host galaxy is also observed in absorption, where we detect several strong Fe II transitions as well as Mg II and Mg I. Although host galaxy absorption features are common in GRB afterglow spectra, we detect absorption from strong metal lines directly in the host continuum (at a time when the afterglow was contributing to < 15 per cent). Finally, we discuss the possibility that the geometry and state of the absorbing and emitting gas are indicative of a galactic scale outflow expelled at the final stage of two merging galaxies.
Volume
474
Issue
2
Start page
2738
Uri
Url
Issn Identifier
0035-8711
Ads BibCode
2018MNRAS.474.2738H
Rights
open.access
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