Absorption systems in the spectrum of GRB 021004

Møller, P.; Fynbo, J. P. U.; Hjorth, J.; Thomsen, B.; Egholm, M. P.; Andersen, M. I.; Gorosabel, J.; Holland, S. T.; Jakobsson, P.; Jensen, B. L.; Pedersen, H.; Pedersen, K.; Weidinger, M.

doi:10.1051/0004-6361:20021612

Cited by 79 publications

(80 citation statements)

References 18 publications

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“…A similar inference was made in the case of GRB 021004, which exhibited a complex velocity structure extending from about 140 to 3000 km s À1 (Möller et al 2002;Mirabal et al 2003;Schaefer et al 2003;Fiore et al 2005;Starling et al 2005b). The presence of such a fast outflow led to the general conclusion that the progenitor was a Wolf-Rayet star.…”

Section: A C Iv Outflowsupporting

confidence: 64%

Spectroscopy of GRB 050505 atz= 4.275: A log N(Hi) = 22.1 DLA Host Galaxy and the Nature of the Progenitor

Berger

Penprase

Cenko

et al. 2006

ApJ

104

103

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We present optical spectroscopy of the afterglow of GRB 050505 obtained with the Keck I 10 m telescope. The spectrum exhibits three absorption systems with the highest, at z ¼ 4:2748, arising in the host galaxy. The host absorption is marked by a DLA with log N (H i) ¼ 22:05 AE 0:10, higher than that of any QSO-DLA detected to date but similar to several other recent measurements from GRB spectra. We further deduce a metallicity of Z % 0:06 Z , with a depletion pattern that is similar to that of the Galactic warm halo or warm disk. More importantly, we detect strong absorption from Si ii Ã indicating a dense environment, n H k 10 2 cm À3 , in the vicinity of the burst, with a size of $4 pc. The C iv absorption system spans a velocity range of about 10 3 km s À1 , most likely arising in the progenitor stellar wind. In this context the lack of corresponding Si iv absorption indicates that the progenitor had a mass P25 M and a metallicity P0.1 Z , 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 and/or sight lines which probe star-forming regions, or if it is a manifestation of different star formation properties in GRB-DLAs.

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Section: A C Iv Outflowsupporting

confidence: 64%

Spectroscopy of GRB 050505 atz= 4.275: A log N(Hi) = 22.1 DLA Host Galaxy and the Nature of the Progenitor

Berger

Penprase

Cenko

et al. 2006

ApJ

104

103

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“…Several absorption systems with outflow velocities of a few 1000 km s −1 were also reported (Salamanca et al 2002;Savaglio et al 2002) and studied in detail by Møller et al (2002b), Wang et al (2003), Matheson et al (2003), Schaefer et al (2003), Mirabal et al (2003), Starling et al (2005), and Lazzati et al (2006). Jakobsson et al (2005) also report the detection of the host galaxy Lyα line in narrow-band imaging.…”

Section: Introductionmentioning

confidence: 85%

“…1) exhibits a large number of absorption lines, as well as Lyα in emission (see Table 3 for a list, and also Møller et al 2002b;Starling et al 2005;Jakobsson et al 2005, on the Lyα emission line). Some of the absorption lines are due to two foreground systems at redshifts z = 1.3820 and z = 1.6020 (Møller et al 2002b;Mirabal et al 2003;see Tejos et al 2007see Tejos et al , 2009and Vergani et al 2009, for additional discussions about the foreground absorbers), but the remaining lines are from multiple systems found in the redshift range 2.2967 ≤ z ≤ 2.3291.…”

Section: The Blueshifted Absorption-line Systemsmentioning

confidence: 98%

“…However, this trough overlaps with Lyα of system C, and the extension is found to belong to system C (see below). It is remarkable that the D and E systems are separated in velocity by exactly the amount required to shift the C IV 1550 Å line complex right on top of the C IV 1548 Å one in the spectrum (Møller et al 2002b;Savaglio et al 2002). This shift is known as absorption-absorption "line-locking" and is not uncommon in QSO spectra where radiative acceleration is important (e.g., Srianand et al 2002).…”

Section: The Blueshifted Absorption-line Systemsmentioning

confidence: 98%

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GRB 021004: Tomography of a gamma-ray burst progenitor and its host galaxy

Castro-Tirado¹,

Møller

Garcı́a-Segura³

et al. 2010

A&A

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Aims. We analyse the distribution of matter around the progenitor star of gamma-ray burst GRB 021004 and the properties of its host galaxy with high-resolution echelle and near-infrared spectroscopy. Methods. Observations were taken by the 8.2 m Very Large Telescope with the Ultraviolet and Visual Echelle spectrograph (UVES) and the Infrared Spectrometer And Array Camera (ISAAC) between 10 and 14 h after the onset of the event.Results. We report the first detection of emission lines from a GRB host galaxy in the near-infrared, detecting Hα and the [O III] doublet. These allow us to independently measure the systemic redshift (z = 2.3304 ± 0.0005), which is not contaminated by absorption as the Lyα line is, and infer the host galaxy properties. From the visual echelle spectroscopy, we find several absorptionline groups spanning a range of about 3000 km s −1 in velocity relative to the redshift of the host galaxy. The absorption profiles are very complex with both velocity-broadened components extending over several 100 km s −1 and narrow lines with velocity widths of only ∼20 km s −1 . By analogy with QSO absorption line studies, the relative velocities, widths, and degrees of ionization of the lines ("line-locking", "ionization-velocity correlation") show that the progenitor had both an extremely strong radiation field and several distinct mass-loss phases (winds). Conclusions. These results are consistent with GRB progenitors being massive stars, such as luminous blue variables (LBVs) or Wolf-Rayet stars, providing a detailed picture of the spatial and velocity structure of the GRB progenitor star at the time of explosion. The host galaxy is a prolific star-forming galaxy with a SFR of ∼40 M yr −1 .

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“…Djorgovski et al 1998;Vreeswijk et al 2001b), that the afterglow is often situated behind a very large neutral hydrogen column (e.g. Hjorth et al 2003a;Vreeswijk et al 2004) with relatively high metal column densities and dust depletions compared to damped Lyα systems observed along QSO sight lines (Savaglio et al 2003;Savaglio & Fall 2004), and have provided evidence for high-velocity outflows (up to 3000 km s −1 , Møller et al 2002;Schaefer et al 2003;Mirabal et al 2003), presumably caused by the wind of the GRB massive-star progenitor. Finally, spectroscopic monitoring of GRB 030329/SN2003dh (Stanek et al 2003;Hjorth et al 2003b) has revealed a remarkable similarity with the spectral evolution of GRB 980425/SN1998bw (Galama et al 1998;Patat et al 2001), confirming the connection between GRBs and supernova explosions.…”

Section: Introductionmentioning

confidence: 99%

Low-resolution VLT spectroscopy of GRBs 991216, 011211 and 021211

Vreeswijk

Smette

Fruchter

et al. 2006

A&A

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We present low-resolution VLT spectroscopy of the afterglow of the gamma-ray bursts (GRBs) 991216, 011211 and 021211. Our spectrum of GRB 991216 is the only optical spectrum for this afterglow. It shows two probable absorption systems at z = 0.80 and z = 1.02, where the highest redshift most likely reflects the distance to the host galaxy. A third system may be detected at z = 0.77. HST imaging of the field, obtained 4 months after the burst, has resulted in the detection of two amorphous regions of emission, one at the projected afterglow position, and the other 0. 6 away. The spectrum shows a depression in flux in between 4000 Å and 5500 Å. This could be the result of a 2175 Å-type extinction feature in the host of GRB 991216, but at a rather red wavelength of 2360 Å. If this interpretation is correct, it is the first time the extinction feature is seen in a GRB afterglow spectrum. It is centered at a wavelength similar to that of the ultra-violet (UV) bumps inferred from observations of a few UV-strong, hydrogen-poor stars in the Galaxy. All significant absorption lines (except for one) detected in the spectrum of GRB 011211 are identified with lines originating in a single absorption system at z = 2.142 ± 0.002, the redshift of the GRB 011211 host galaxy. We also detect the Lyα absorption line in the host, to which we fit a neutral hydrogen column density of log N(H i) = 20.4 ± 0.2, which indicates that it is a damped Lyα system. Using a curve-of-growth analysis, we estimate the Si, Fe and Al metallicity at the GRB 011211 redshift to be [Si/H] = −0.9 Key words. gamma rays: bursts -galaxies: abundances -galaxies: distances and redshifts -galaxies: quasars: absorption lines IntroductionSpectroscopy of the afterglows of long-duration Gamma-Ray Bursts (GRBs) has been essential for our understanding of the Based on observations collected at the European Southern Observatory, Chile; proposals physical mechanism that produces these powerful explosions. Following the discovery of GRB afterglows (Costa et al. 1997;Van Paradijs et al. 1997), the first redshift determination by Metzger et al. (1997) provided conclusive evidence that the origin of the long-duration class of GRBs (Kouveliotou et al. 1993) is cosmological. Obviously, redshifts are required to deduce most meaningful quantities, such as the GRB energetics Article published by EDP Sciences and available at http://www.edpsciences.org/aa or http://dx

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Absorption systems in the spectrum of GRB 021004

Cited by 79 publications

References 18 publications

Spectroscopy of GRB 050505 atz= 4.275: A log N(Hi) = 22.1 DLA Host Galaxy and the Nature of the Progenitor

Spectroscopy of GRB 050505 atz= 4.275: A log N(Hi) = 22.1 DLA Host Galaxy and the Nature of the Progenitor

GRB 021004: Tomography of a gamma-ray burst progenitor and its host galaxy

Low-resolution VLT spectroscopy of GRBs 991216, 011211 and 021211

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