2008A&A...489...37T


C.D.S. - SIMBAD4 rel 1.7 - 2021.02.26CET18:02:15

2008A&A...489...37T - Astronomy and Astrophysics, volume 489, 37-48 (2008/10-1)

The host of GRB 060206: kinematics of a distant galaxy.

THOENE C.C., WIERSEMA K., LEDOUX C., STARLING R.L.C., DE UGARTE POSTIGO A., LEVAN A.J., FYNBO J.P.U., CURRAN P.A., GOROSABEL J., VAN DER HORST A.J., LLORENTE A., ROL E., TANVIR N.R., VREESWIJK P.M., WIJERS R.A.M.J. and KEWLEY L.J.

Abstract (from CDS):

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. We investigate the state and properties of the interstellar medium in the host of GRB060206 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. We used early (starting 1.6h after the burst) WHT/ISIS optical spectroscopy of the afterglow of the gamma-ray burst GRB060206 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. 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 NV was detected as well. The host is detected in deep HST imaging with F814WAB=27.48±0.19mag and a 3σ upper limit of H=20.6mag (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. (2007ApJ...659L..99H), which we prove from our WHT spectra taken before and Subaru spectra taken during those observations.

Abstract Copyright:

Journal keyword(s): gamma rays: bursts - galaxies: abundances - cosmology: observations

Simbad objects: 20

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Number of rows : 20

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 GRB 021004 gB 00 26 54.68 +18 55 41.6           ~ 518 0
2 GRB 050904 gB 00 54 50.794 +14 05 09.42           ~ 433 0
3 SN 2006aj SN* 03 21 39.670 +16 52 02.27 17.96 19.11 17.40     SNIc-BL 843 1
4 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 15195 1
5 [LDM2003] GRB J061331.1-515642 G 06 13 31.1 -51 56 42           ~ 6 1
6 M 82 IG 09 55 52.430 +69 40 46.93 9.61 9.30 8.41     ~ 5422 6
7 NGC 3079 Sy2 10 01 57.80342 +55 40 47.2428 11.57 11.54 10.86     ~ 1279 3
8 SN 2003dh SN* 10 44 50.030 +21 31 18.15     16.2     SNIcpec 1130 1
9 [VWR2003] GRB 030323 abs 3.372 G 11 06 09.4 -21 46 13           ~ 13 1
10 [LDM2003] GRB J115626.4+651200 G 11 56 26.55 +65 12 00.7           ~ 19 1
11 GRB 030429 gB 12 13 07.495 -20 54 49.54     23.70     ~ 121 0
12 NGC 4945 Sy2 13 05 27.279 -49 28 04.44   9.31 14.40 7.55   ~ 1300 2
13 GRB 060206 gB 13 31 43.420 +35 03 03.60   19.99 17.09     ~ 287 0
14 GRB 020405 gB 13 58 03.12 -31 22 22.2   21.9 21.5     ~ 238 1
15 GRB 050730 gB 14 08 17.090 -03 46 18.90   20.32 17.68     ~ 285 0
16 GRB 060418 gB 15 45 42.600 -03 38 20.00 15.73 16.19 14.98     ~ 325 0
17 GRB 020813A gB 19 46 41.874 -19 36 04.81           ~ 287 0
18 GRB 050922C gB 21 09 33.000 -08 45 30.10 15.15 15.86 14.69     ~ 254 0
19 GRB 050820A gB 22 29 38.110 +19 33 37.10 18.33 19.00 18.47     ~ 341 0
20 GRB 051111A gB 23 12 33.170 +18 22 28.80 19.77 20.08 19.50     ~ 187 0

    Equat.    Gal    SGal    Ecl

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