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Title:
The Prompt, High-Resolution Spectroscopic View of the "Naked-Eye" GRB080319B
Authors:
D'Elia, V.; Fiore, F.; Perna, R.; Krongold, Y.; Covino, S.; Fugazza, D.; Lazzati, D.; Nicastro, F.; Antonelli, L. A.; Campana, S.; Chincarini, G.; D'Avanzo, P.; Della Valle, M.; Goldoni, P.; Guetta, D.; Guidorzi, C.; Meurs, E. J. A.; Mirabel, F.; Molinari, E.; Norci, L.; Piranomonte, S.; Stella, L.; Stratta, G.; Tagliaferri, G.; Ward, P.
Affiliation:
AA(INAF, Osservatorio Astronomico di Roma, via Frascati 33, Monteporzio (Rm) I00040, Italy ), AB(INAF, Osservatorio Astronomico di Roma, via Frascati 33, Monteporzio (Rm) I00040, Italy), AC(JILA and Department of Astrophysical and Planetary Science, CU Boulder, Boulder, CO 80309, USA), AD(Instituto de Astronomia, Universidad Nacional Autonomica de Mexico, Apartado Postal 70-264, 04510 Mexico DF, Mexico), AE(INAF, Osservatorio Astronomico di Brera, via E. Bianchi 46, 23807 Merate (LC), Italy), AF(INAF, Osservatorio Astronomico di Brera, via E. Bianchi 46, 23807 Merate (LC), Italy), AG(JILA and Department of Astrophysical and Planetary Science, CU Boulder, Boulder, CO 80309, USA), AH(INAF, Osservatorio Astronomico di Roma, via Frascati 33, Monteporzio (Rm) I00040, Italy), AI(INAF, Osservatorio Astronomico di Roma, via Frascati 33, Monteporzio (Rm) I00040, Italy), AJ(INAF, Osservatorio Astronomico di Brera, via E. Bianchi 46, 23807 Merate (LC), Italy), AK(INAF, Osservatorio Astronomico di Brera, via E. Bianchi 46, 23807 Merate (LC), Italy; Università di Milano Bicocca, piazza della Scienza 3, 20126 Milano, Italy), AL(INAF, Osservatorio Astronomico di Brera, via E. Bianchi 46, 23807 Merate (LC), Italy), AM(INAF, Osservatorio Astronomico di Capodimonte, salita Moiarello 16, Napoli, Italy), AN(APC/UMR 7164, Service d'Astrophysique, CEA Centre de Saclay, France), AO(INAF, Osservatorio Astronomico di Roma, via Frascati 33, Monteporzio (Rm) I00040, Italy), AP(INAF, Osservatorio Astronomico di Brera, via E. Bianchi 46, 23807 Merate (LC), Italy), AQ(School of Cosmic Physics, DIAS, 31 Fitzwilliam Place, Dublin 4, Ireland; School of Physical Sciences and NCPST, DCU, Glasnevin, Dublin 9, Ireland), AR(European Southern Observatory, Casilla 19001, Santiago, Chile), AS(INAF, Osservatorio Astronomico di Brera, via E. Bianchi 46, 23807 Merate (LC), Italy), AT(School of Physical Sciences and NCPST, DCU, Glasnevin, Dublin 9, Ireland), AU(INAF, Osservatorio Astronomico di Roma, via Frascati 33, Monteporzio (Rm) I00040, Italy), AV(INAF, Osservatorio Astronomico di Roma, via Frascati 33, Monteporzio (Rm) I00040, Italy), AW(ASI Science Data Center, via Galileo Galilei, 00044 Frascati, Italy), AX(INAF, Osservatorio Astronomico di Brera, via E. Bianchi 46, 23807 Merate (LC), Italy), AY(School of Cosmic Physics, DIAS, 31 Fitzwilliam Place, Dublin 4, Ireland; Mullard Space Science Laboratory, Dorking, Surrey RH5 6NT, UK)
Publication:
The Astrophysical Journal, Volume 694, Issue 1, pp. 332-338 (2009). (ApJ Homepage)
Publication Date:
03/2009
Origin:
IOP
Astronomy Keywords:
gamma rays: bursts
DOI:
10.1088/0004-637X/694/1/332
Bibliographic Code:
2009ApJ...694..332D

Abstract

GRB080319B reached fifth optical magnitude during the burst prompt emission. Thanks to the Very Large Telescope (VLT)/Ultraviolet and Visual Echelle Spectrograph (UVES) rapid response mode, we observed its afterglow just 8m:30s after the gamma-ray burst (GRB) onset when the magnitude was R ~ 12. This allowed us to obtain the best signal-to-noise (S/N), high-resolution spectrum of a GRB afterglow ever (S/N per resolution element ~50). The spectrum is rich of absorption features belonging to the main system at z = 0.937, divided in at least six components spanning a total velocity range of 100 km s-1. The VLT/UVES observations caught the absorbing gas in a highly excited state, producing the strongest Fe II fine structure lines ever observed in a GRB. A few hours later, the optical depth of these lines was reduced by a factor of 4-20, and the optical/UV flux by a factor of ~60. This proves that the excitation of the observed fine structure lines is due to "pumping" by the GRB UV photons. A comparison of the observed ratio between the number of photons absorbed by the excited state and those in the Fe II ground state suggests that the six absorbers are ~2-6 kpc from the GRB site, with component I ~ 3 times closer to the GRB site than components III-VI. Component I is characterized also by the lack of Mg I absorption, unlike all other components. This may be both due to a closer distance and a lower density, suggesting a structured interstellar matter in this galaxy complex.

Based on observations collected at the European Southern Observatory (ESO) with the VLT/Kueyen telescope, Paranal, Chile, in the framework of program 080.A-0398.

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