Probing cosmic chemical evolution with gamma-ray bursts:
 GRB 060206 at <i>z</i> = 4.048

Fynbo, J. P. U.; Starling, R. L. C.; Ledoux, C.; Wiersema, K.; Thöne, C. C.; Sollerman, J.; Jakobsson, P.; Hjorth, J.; Watson, Derrick G.; Vreeswijk, P. M.; Møller, P.; Rol, E.; Gorosabel, J.; Näränen, Jyri; Wijers, R. A. M. J.; Björnsson, G.; Cerón, J. M. Castro; Curran, P. A.; Hartmann, D. H.; Holland, S. T.; Jensen, B. L.; Levan, A. J.; Limousin, M.; Kouveliotou, C.; Nelemans, G.; Pedersen, K.; Priddey, R.; Tanvir, N. R.

doi:10.1051/0004-6361:20065056

Cited by 160 publications

(85 citation statements)

References 31 publications

(38 reference statements)

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“…Those finestructure lines are not found in QSO absorbers, but seem abundant in GRB lines-of-sight (e.g. Vreeswijk et al 2004;Starling et al 2005b;Prochaska et al 2006;Fynbo et al 2006;Kawai et al 2006;Penprase et al 2006). We measured their column densities through Voigt profile fitting, which is complicated by the blending of the lines of different velocity systems; for every velocity component, however, a diagnostic set of absorption lines can be measured.…”

Section: Discussionmentioning

confidence: 98%

The host of GRB 060206: kinematics of a distant galaxy

Thöne¹,

Wiersema

Ledoux

et al. 2008

A&A

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Context. GRB afterglow spectra are sensitive probes of interstellar matter along the line-of-sight in their host galaxies, as well as in intervening galaxies. The rapid fading of GRBs makes it very difficult to obtain spectra of sufficient resolution and S/N to allow for these kinds of studies. Aims. We investigate the state and properties of the interstellar medium in the host of GRB 060206 at z = 4.048 with a detailed study of groundstate and finestructure absorption lines in an early afterglow spectrum. This allows us to derive conclusions on the nature and origin of the absorbing structures and their connection to the host galaxy and/or the GRB. Methods. We used early (starting 1.6 h after the burst) WHT/ISIS optical spectroscopy of the afterglow of the gamma-ray burst GRB 060206 detecting a range of metal absorption lines and their finestructure transitions. Additional information is provided by the afterglow lightcurve. The resolution and wavelength range of the spectra and the bright afterglow have facilitated a detailed study and fitting of the absorption line systems in order to derive column densities. We also used deep imaging to detect the host galaxy and probe the nature of an intervening system at z = 1.48 seen in absorption in the afterglow spectra. Results. We detect four discrete velocity systems in the resonant metal absorption lines, best explained by shells within and/or around the host created by starburst winds. The finestructure lines have no less than three components with strengths decreasing from the redmost components. We therefore suggest that the finestructure lines are best explained as being produced by UV pumping from which follows that the redmost component is the one closest to the burst where N v was detected as well. The host is detected in deep HST imaging with F814W AB = 27.48 ± 0.19 mag and a 3σ upper limit of H = 20.6 mag (Vega) is achieved. A candidate counterpart for the intervening absorption system is detected as well, which is quite exceptional for an absorber in the sightline towards a GRB afterglow. The intervening system shows no temporal evolution as claimed by Hao et al. (2007, ApJ, 659, 99), which we prove from our WHT spectra taken before and Subaru spectra taken during those observations.

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Section: Discussionmentioning

confidence: 98%

The host of GRB 060206: kinematics of a distant galaxy

Thöne¹,

Wiersema

Ledoux

et al. 2008

A&A

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“…RAPTOR started observations 48.1 minutes after trigger and reported that, after an initial fading, the AG rebrightened 1 hr after burst by ∼1 mag within a couple of minutes (Wozniak et al 2006). Many observatories followed the bright optical AG (Monfardini et al 2006;Stanek et al 2007, and references therein), and Fynbo (2006) carried out spectral observations to determine its large redshift, z = 4.05, later confirmed by other groups. The RAPTOR data clearly show that the rebrightening was due to two flares (Wozniak et al 2006).…”

Section: Grbs With Large X-ray Flares During the Early X-ray Afterglowmentioning

confidence: 92%

THE DIVERSE BROADBAND LIGHT CURVES OFSWIFTGAMMA-RAY BURSTS REPRODUCED WITH THE CANNONBALL MODEL

Dado

Dar

Rújula

2009

ApJ

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Two radiation mechanisms, inverse Compton scattering (ICS) and synchrotron radiation (SR), suffice within the Cannonball (CB) model of long gamma-ray bursts (LGRBs) and X-ray flashes (XRFs) to provide a very simple and accurate description of their observed prompt emission and afterglows (AGs). Simple as they are, the two mechanisms and the burst environment generate the rich structure of the light curves at all frequencies and times. This is demonstrated for 33 selected Swift LGRBs and XRFs, which are well sampled from early until late time and faithfully represent the entire diversity of the broadband light curves of Swift LGRBs and XRFs. Their prompt gamma-ray and X-ray emission is dominated by ICS of "glory" light. During their fast decline phase, ICS is taken over by SR, which dominates their broadband AG. The pulse shape and spectral evolution of the gamma-ray peaks and the early-time X-ray flares, and even the delayed optical "humps" in XRFs, are correctly predicted. The "canonical" and noncanonical X-ray light curves and the chromatic behavior of the broadband AGs are well reproduced. In particular, in canonical X-ray light curves, the initial fast decline and rapid softening of the prompt emission, the transition to the plateau phase, the subsequent gradual steepening of the plateau to an asymptotic power-law decay, and the transition from chromatic to achromatic behavior of the light curves agree well with those predicted by the CB model. The Swift earlytime data on XRF 060218 are inconsistent with a blackbody emission from a shock breakout through a stellar envelope. Instead, they are well described by ICS of glory light by a jet breaking out from SN2006aj.

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“…Tumlinson et al 2007). Fynbo et al (2006) interpreted an absorption feature of the GRB 060206 afterglow spectrum as a possible H 2 detection. Prochaska et al (2009) and Sheffer et al (2009) report the presence of strong H 2 and CO absorption features in the spectrum of the GRB 080607 afterglow.…”

Section: Dust Content and Moleculesmentioning

confidence: 99%

VLT/X-shooter spectroscopy of the GRB 120327A afterglow

D’Elia

Fynbo

Goldoni

et al. 2014

A&A

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Aims. 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. Methods. We analyzed medium-resolution, multi-epoch spectroscopic observations (R ∼ 7000−12 000, corresponding to ∼15−23 km s −1 , S /N = 15−30 and wavelength range 3000−25 000 Å) of the optical afterglow of GRB 120327A, taken with X-shooter at the VLT 2.13 and 27.65 hr after the GRB trigger. Results. 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 N H /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 C ii, O i, Si ii, Fe ii, and Ni ii, 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 Fe ii λ2396 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 d I = 200 +100 −60 pc, while component II is located closer to the GRB, at d II = 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 H 2 molecules is firmly established, with a molecular fraction f in the range f = 4 × 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.

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Probing cosmic chemical evolution with gamma-ray bursts: GRB 060206 at z = 4.048

Cited by 160 publications

References 31 publications

The host of GRB 060206: kinematics of a distant galaxy

The host of GRB 060206: kinematics of a distant galaxy

THE DIVERSE BROADBAND LIGHT CURVES OFSWIFTGAMMA-RAY BURSTS REPRODUCED WITH THE CANNONBALL MODEL

VLT/X-shooter spectroscopy of the GRB 120327A afterglow

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