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Starling, R. L. C; Wiersema, K; Levan, A. J; Sakamoto, T; Bersier, D; Goldoni, P; Oates, S. R; Rowlinson, A; Campana, S; Sollerman, J; Tanvir, N. R; Malesani, D; Fynbo, J. P. U; Covino, S; D'Avanzo, P; O'Brien, P. T; Page, K. L; Osborne, J. P; Vergani, S. D; Barthelmy, S; Burrows, D. N; Cano, Z; Curran, P. A; De Pasquale, M; D'Elia, V; Evans, P. A; Flores, H; Fruchter, A. S; Garnavich, P; Gehrels, N; Gorosabel, J; Hjorth, J; Holland, S. T; van der Horst, A. J; Hurkett, C. P; Jakobsson, P; Kamble, A. P; Kouveliotou, C; Kuin, N. P. M; Kaper, L; Mazzali, P. A; Nugent, P. E; Pian, E; Stamatikos, M; Thöne, C. C; Woosley, S. E
Monthly notices of the Royal Astronomical Society, 03/2011, Volume: 411, Issue: 4Journal Article
We report the Swift discovery of the nearby long, soft gamma-ray burst GRB100316D, and the subsequent unveiling of its low-redshift host galaxy and associated supernova. We derive the redshift of the event to be z= 0.0591 ± 0.0001 and provide accurate astrometry for the gamma-ray burst (GRB) supernova (SN). We study the extremely unusual prompt emission with time-resolved γ-ray to X-ray spectroscopy and find that the spectrum is best modelled with a thermal component in addition to a synchrotron emission component with a low peak energy. The X-ray light curve has a remarkably shallow decay out to at least 800 s. The host is a bright, blue galaxy with a highly disturbed morphology and we use Gemini-South, Very Large Telescope and Hubble Space Telescope observations to measure some of the basic host galaxy properties. We compare and contrast the X-ray emission and host galaxy of GRB100316D to a subsample of GRB-SNe. GRB100316D is unlike the majority of GRB-SNe in its X-ray evolution, but resembles rather GRB060218, and we find that these two events have remarkably similar high energy prompt emission properties. Comparison of the host galaxies of GRB-SNe demonstrates, however, that there is a great diversity in the environments in which GRB-SNe can be found. GRB100316D is an important addition to the currently sparse sample of spectroscopically confirmed GRB-SNe, from which a better understanding of long GRB progenitors and the GRB-SN connection can be gleaned. PUBLICATION ABSTRACT
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