2001A&A...370..909J


C.D.S. - SIMBAD4 rel 1.7 - 2021.06.15CEST09:06:20

2001A&A...370..909J - Astronomy and Astrophysics, volume 370, 909-922 (2001/5-2)

The afterglow of the short/intermediate-duration gamma-ray burst GRB 000301C: a jet at (z)=2.04.

JENSEN B.L., FYNBO J.U., GOROSABEL J., HJORTH J., HOLLAND S., MOLLER P., THOMSEN B., BJOERNSSON G., PEDERSEN H., BURUD I., HENDEN A., TANVIR N.R., DAVIS C.J., VREESWIJK P., ROL E., HURLEY K., CLINE T., TROMBKA J., McCLANAHAN T., STARR R., GOLDSTEN J., CASTRO-TIRADO A.J., GREINER J., BAILER-JONES C.A.L., KUEMMEL M. and MUNDT R.

Abstract (from CDS):

We present Ulysses and NEAR data from the detection of the short or intermediate duration (2 s) gamma-ray burst GRB 000301C (2000 March 1.41 UT). The gamma-ray burst (GRB) was localised by the Inter Planetary Network (IPN) and RXTE to an area of ∼50arcmin2. A fading optical counterpart was subsequently discovered with the Nordic Optical Telescope (NOT) about 42 h after the burst. The GRB lies at the border between the long-soft and the short-hard classes of GRBs. If GRB 000301C belongs to the latter class, this would be the first detection of an afterglow to a short-hard burst. We present UBRI photometry from the time of the discovery until 11 days after the burst. We also present JHK photometry obtained with UKIRT on 2000 March 4.5 UT (3.1 days after the burst). Finally, we present spectroscopic observations of the optical afterglow obtained with the ESO VLT Antu telescope 4 and 5 days after the burst. The optical light curve is consistent with being achromatic from 2 to 11 days after the burst and exhibits a break. A broken power-law fit yields a shallow pre-break decay power-law slope of α1=-0.72±0.06, a break time of tbreak=4.39±0.26 days after the burst, and a post-break slope of α2=-2.29±0.17. These properties of the light curve are best explained by a sideways expanding jet in an ambient medium of constant mean density. In the optical spectrum we find absorption features that are consistent with FeII, CIV, CII, SiII and Lyα at a redshift of 2.0404 ±0.0008. We find evidence for a curved shape of the spectral energy distribution of the observed afterglow. It is best fitted with a power-law spectral distribution with index β~-0.7 reddened by an SMC-like extinction law with AV∼0.1mag. Based on the Lyα absorption line we estimate the HI column density to be log(N(HI))=21.2±0.5. This is the first direct indication of a connection between GRB host galaxies and Damped Lyα Absorbers.

Abstract Copyright:

Journal keyword(s): gamma rays: bursts - cosmology: observations - galaxies: distances and redshifts - ISM: dust, extinction - quasars: absorption lines

CDS comments: paragr. 4.2: S868-G and p389-d = GSPC S868-G and GSPC P389-D.

Simbad objects: 15

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Number of rows : 15

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 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 9831 1
2 GRB 970228 gB 05 01 46.7 +11 46 53           ~ 627 1
3 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 15421 1
4 GRB 970508 gB 06 53 49.2 +79 16 19           ~ 848 1
5 GRB 980326 gB 08 36 34.3 -18 51 24           ~ 259 0
6 GRB 971214 gB 11 56 26.4 +65 12 01           ~ 434 1
7 GRB 990510 gB 13 38 07.64 -80 29 48.8           ~ 470 1
8 FS 136 * 14 59 32.0174219124 -00 06 16.895065901   15.80 14.68     K2 7 0
9 GRB 990123 gB 15 25 29 +44 45.0     8.95     ~ 968 1
10 GRB 000301C gB 16 20 18.5 +29 26 35           ~ 344 0
11 GRB 991208 gB 16 33 53.51 +46 27 21.5           ~ 246 1
12 GRB 000926 gB 17 04 15 +51 46.0           ~ 346 0
13 FS 141 * 17 48 58.9910389754 +23 17 43.494982485   13.29 12.51     G2 6 0
14 SN 1998bw SN* 19 35 03.17 -52 50 46.1   14.09       SNIc 1689 2
15 GRB 980519 gB 23 22 21.5 +77 15 43           ~ 195 0

    Equat.    Gal    SGal    Ecl

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