Thöne, CC, Kann, DA, Jóhannesson, G, Selj, JH, Jaunsen, AO, Fynbo, JPU, Akerlof, CW, Baliyan, KS, Bartolini, C, Bikmaev, IF, Bloom, JS, Burenin, RA, Cobb, BE, Covino, S, Curran, PA, Dahle, H, Ferrero, A, Foley, S, French, J, Fruchter, AS et al, Ganesh, S, Graham, JF, Greco, G, Guarnieri, A, Hanlon, L, Hjorth, J, Ibrahimov, M, Israel, GL, Jakobsson, P, Jelínek, M, Jensen, BL, Jørgensen, UG, Khamitov, IM, Koch, TS, Levan, AJ, Malesani, D, Masetti, N, Meehan, S, Melady, G, Nanni, D, Näränen, J, Pakstiene, E, Pavlinsky, MN, Perley, DA, Piccioni, A, Pizzichini, G, Pozanenko, A, Roming, PWA, Rujopakarn, W, Rumyantsev, V, Rykoff, ES, Sharapov, D, Starr, D, Sunyaev, RA, Swan, H, Tanvir, NR, Terra, F, De Ugarte Postigo, A, Vreeswijk, PM, Wilson, AC, Yost, SA and Yuan, F (2010) Photometry and spectroscopy of GRB 060526: A detailed study of the afterglow and host galaxy of a z = 3.2 gamma-ray burst. Astronomy and Astrophysics, 523 (5). ISSN 0004-6361

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Abstract

Aims: With this paper we want to investigate the highly variable afterglow light curve and environment of gamma-ray burst (GRB) 060526 at z = 3.221. Methods: We present one of the largest photometric datasets ever obtained for a GRB afterglow, consisting of multi-color photometric data from the ultraviolet to the near infrared. The data set contains 412 data points in total to which we add additional data from the literature. Furthermore, we present low-resolution high signal-to-noise spectra of the afterglow. The afterglow light curve is modeled with both an analytical model using broken power law fits and with a broad-band numerical model which includes energy injections. The absorption lines detected in the spectra are used to derive column densities using a multi-ion single-component curve-of-growth analysis from which we derive the metallicity of the host of GRB 060526. Results: The temporal behaviour of the afterglow follows a double broken power law with breaks at t = 0.090 ± 0.005 and t = 2.401 ± 0.061 days. It shows deviations from the smooth set of power laws that can be modeled by additional energy injections from the central engine, although some significant microvariability remains. The broadband spectral-energy distribution of the afterglow shows no significant extinction along the line of sight. The metallicity derived from S and Fe of [S/H] = -0.57 ±0.25 and [Fe/H] = -1.09±0.24 is relatively high for a galaxy at that redshift but ii ii comparable to the metallicity of other GRB hosts at similar redshifts. At the position of the afterglow, no host is detected to F775W(AB) = 28.5 mag with the HST, implying an absolute magnitude of the host M(1500 Å) > -18.3 mag which is fainter than most long-duration hosts, although the GRB may be associated with a faint galaxy at a distance of 11 kpc. © ESO 2010.

Item Type:	Article
Uncontrolled Keywords:	0201 Astronomical And Space Sciences
Subjects:	Q Science > QB Astronomy Q Science > QC Physics Q Science > QD Chemistry
Divisions:	Astrophysics Research Institute
Publisher:	EDP Sciences
Date Deposited:	23 May 2017 10:42
Last Modified:	20 Apr 2022 09:42
DOI or ID number:	10.1051/0004-6361/200810340
URI:	https://researchonline.ljmu.ac.uk/id/eprint/6511

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