The luminous, massive and solar metallicity galaxy hosting the Swift γ -ray burst GRB160804A at z = 0.737

K. E. Heintz, D. Malesani, K. Wiersema, P. Jakobsson, J. P.U. Fynbo, S. Savaglio, Z. Cano, S. Covino, V. D'Elia, A. Gomboc, F. Hammer, L. Kaper, B. Milvang-Jensen, P. Møller, S. Piranomonte, J. Selsing, N. H.P. Rhodin, N. R. Tanvir, C. C. Thöne, A. de Ugarte PostigoS. D. Vergani, D. Watson

Rannsóknarafurð: Framlag til fræðitímaritsGreinritrýni

4 Tilvitnanir (Scopus)


We here present the spectroscopic follow-up observations with VLT/X-shooter of the Swift long-duration gamma-ray burst GRB160804A at z=0.737. Typically, GRBs are found in lowmass, 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 GRB160804A as one of the most luminous, massive and metal-rich GRB hosts at z < 1.5. Furthermore, the gasphase 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 MgII and MgI. 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.

Upprunalegt tungumálEnska
Síður (frá-til)2738-2749
FræðitímaritMonthly Notices of the Royal Astronomical Society
Númer tölublaðs2
ÚtgáfustaðaÚtgefið - 2018


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© 2018 The Author(s).


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