Статья

The afterglow of the short/intermediate-duration gamma-ray burst GRB 000301C: A jet at $\mathsf{{\vec z}=2.04}$

B. L. JensenAstronomical Observatory, University of Copenhagen, Juliane Maries Vej 30, 2100 Copenhagen Ø, Denmark e-mail: [email protected], [email protected], [email protected]J. P. U. FynboEuropean Southern Observatory, Karl-Schwarzschild-Straße 2, 85748 Garching, Germany e-mail: [email protected]J. GorosabelJ. HjorthAstronomical Observatory, University of Copenhagen, Juliane Maries Vej 30, 2100 Copenhagen Ø, Denmark e-mail: [email protected], [email protected], [email protected]K. L. PageDepartment of Physics, University of Notre Dame, Notre Dame IN 46556-5670, USAP. MøllerEuropean Southern Observatory, Karl-Schwarzschild-Straße 2, 85748 Garching, Germany e-mail: [email protected]B. ThomsenInstitute of Physics and Astronomy, University of Aarhus, 8000 Århus C., Denmark e-mail: [email protected], [email protected], [email protected]G. BjörnssonScience Institute, Dunhagi 3, University of Iceland, 107 Reykjavik, Iceland, e-mail: [email protected]H. PedersenAstronomical Observatory, University of Copenhagen, Juliane Maries Vej 30, 2100 Copenhagen Ø, Denmark e-mail: [email protected], [email protected], [email protected]I. BurudInstitut d'Astrophysique et de Géophysique, Université de Liège, avenue de Cointe 5, 4000 Liège, Belgium e-mail: [email protected]A. A. HendenU.S. Naval Observatory, Flagstaff Station, Flagstaff, AZ 86002-1149, USA, e-mail: [email protected]N. R. TanvirDepartment of Physical Sciences, University of Hertfordshire, College Lane, Hatfield, Herts AL10 9AB, UK e-mail: [email protected]C. J. DavisJoint Astronomy Centre, 660 N. A'ohoku Place, Hilo, Hawaii 96720, USA e-mail: [email protected]P. M. VreeswijkUniversity of Amsterdam, Kruislaan 403, 1098 SJ Amsterdam, The Netherlands e-mail: [email protected], [email protected]E. RolUniversity of Amsterdam, Kruislaan 403, 1098 SJ Amsterdam, The Netherlands e-mail: [email protected], [email protected]K. HurleyUniversity of California, Berkeley, Space Sciences Laboratory, Berkeley, CA 94720-7450 USA e-mail: [email protected]T. L. ClineNASA Goddard Space Flight Center, Code 661, Greenbelt, MD 20771 USA e-mail: [email protected]J. I. TrombkaNASA Goddard Space Flight Center, Code 691, Greenbelt, MD 20771 USA e-mail: [email protected], [email protected]T. P. McClanahanNASA Goddard Space Flight Center, Code 691, Greenbelt, MD 20771 USA e-mail: [email protected], [email protected]R. StarrThe Catholic University of America, Department of Physics, Washington, DC 20064 USA e-mail: [email protected]J. GoldstenThe Johns Hopkins University, Applied Physics Laboratory, Laurel, MD 20723 USA e-mail: [email protected]A. J. Castro‐TiradoInstituto de Astrofísica de Andalucía (IAA-CSIC), PO Box 03004, 18080 Granada, SpainJ. GreinerAstrophysikalisches Institut, Potsdam, Germany, e-mail: [email protected]C. A. L. Bailer‐JonesMax-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany e-mail: [email protected], [email protected], [email protected]M KümmelMax-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany e-mail: [email protected], [email protected], [email protected]R. MundtMax-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany e-mail: [email protected], [email protected], [email protected]

2001en

ABI

Аннотация

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 ~50 arcmin2. 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 , a break time of days after the burst, and a post-break slope of . 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 . 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 reddened by an SMC-like extinction law with mag. Based on the Lyα absorption line we estimate the Hi column density to be (N(Hi). This is the first direct indication of a connection between GRB host galaxies and Damped Lyα Absorbers.

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Идентификаторы

DOI: 10.1051/0004-6361:20010291

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