D'Elia, V.2; Fynbo, Johan Peter Uldall3; Goldoni, P.2; Covino, S.2; Postigo, A. de Ugarte2; Ledoux, C.2; Calura, F.2; Gorosabel, J.2; Malesani, D.3; Sanchez-Ramirez, F. Matteucci R.2; Savaglio, S.2; Castro-Tirado, A. J.2; Hartoog, O. E.2; Kaper, L.2; Munoz-Darias, T.2; Pian, E.2; Piranomonte, S.2; Tagliaferri, G.2; Tanvir, N.2; Vergani, S. D.2; Watson, D. J.3; Xu, Dong3
1 Dark Cosmology Centre, The Niels Bohr Institute, Faculty of Science, Københavns Universitet2 unknown3 Dark Cosmology Centre, The Niels Bohr Institute, Faculty of Science, Københavns Universitet
We present a study of the environment of the Swift long gamma-ray burst GRB 120327A at z ~2.8 through optical spectroscopy of its afterglow. We analyzed medium-resolution, multi-epoch spectroscopic observations (~7000 - 12000, corresponding to ~ 15 - 23 km/s, S/N = 15- 30 and wavelength range 3000-25000AA) of the optical afterglow of GRB 120327A, taken with X-shooter at the VLT 2.13 and 27.65 hr after the GRB trigger. The first epoch spectrum shows that the ISM in the GRB host galaxy at z = 2.8145 is extremely rich in absorption features, with three components contributing to the line profiles. The hydrogen column density associated with GRB 120327A has log NH / cm^(-2) = 22.01 +/- 0.09, and the metallicity of the host galaxy is in the range [X/H] = -1.3 to -1.1. In addition to the ground state lines, we detect absorption features associated with excited states of CII, OI, SiII, FeII, and NiII, which we used to derive information on the distance between the host absorbing gas and the site of the GRB explosion. The variability of the FeI\lambda2396 excited line between the two epochs proves that these features are excited by the GRB UV flux. Moreover, the distance of component I is found to be dI=200+100-60 pc, while component II is located closer to the GRB, at dII=100+40-30 pc. These values are among the lowest found in GRBs. Component III does not show excited transitions, so it should be located farther away from the GRB. The presence of H2 molecules is firmly established, with a molecular fraction in the range f=4 X 10^(-7) - 10^(-4). This particularly low value can be attributed to the small dust content. This represents the third positive detection of molecules in a GRB environment.
Astronomy and Astrophysics, 2014, Vol 564, p. 38-56