Spectroscopy of GRB 050505 at z=4.275: A logN(HI)=22.1 DLA Host Galaxy and the Nature of the Progenitor

Details Spectroscopy of GRB 050505 at z=4.275: A logN(HI)=22.1 DLA Host Galaxy and the Nature of the Progenitor Spectroscopy of GRB 050505 at z=4.275: A logN(HI)=22.1 DLA Host Galaxy and the Nature of the Progenitor

2005-11-16

arxiv.org/abs/astro-ph/0511498v1

Astrophys.J.642:979-988,2006

Astronomy and Astrophysics

Astrophysics

19 pages, 8 figures, 2 tables; submitted to ApJ

Scientific paper

10.1086/501162

We present the discovery of the optical afterglow of GRB 050505 and an optical absorption spectrum obtained with the Keck I 10-m telescope. The spectrum exhibits three redshifted absorption systems with the highest, at z=4.2748, arising in the GRB host galaxy. The host absorption system is marked by a damped Ly-alpha (DLA) feature with a neutral hydrogen column density of logN(HI)=22.05+/-0.10, higher than that of any QSO-DLA detected to date, but similar to several other recent measurements from GRB spectra. In addition, we detect absorption lines from both low- and high-ionization species from which we deduce a metallicity, Z~0.06 Z_solar, with a depletion pattern that is roughly similar to that of the Galactic warm halo, warm disk, or disk+halo. More importantly, we detect strong absorption from SiII* indicating a dense environment, n_H>10^2 cm^-3, in the vicinity of the burst, with a size of about 4 pc. In addition, the CIV absorption system spans a velocity range of about 1000 km/s, which is not detected in any other absorption feature. We show that the most likely interpretation for this wide velocity range is absorption in the wind from the progenitor star. In this context, the lack of corresponding SiIV absorption indicates that the progenitor had a mass of <25 M_solar and a metallicity <0.1 Z_solar, and therefore required a binary companion to eject its hydrogen envelope prior to the GRB explosion. Finally, by extending the GRB-DLA sample to z~4.3 we show that these objects appear to follow a similar metallicity-redshift relation as in QSO-DLAs, but with systematically higher metallicities. It remains to be seen whether this trend is simply due to the higher neutral hydrogen columns in GRB-DLAs, or if it is a manifestation of different star formation properties in GRB-DLAs. [abridged]

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