Multicolor observations of the GRB 000926 afterglow

P. A. Price*, F. A. Harrison, T. J. Galama, D. E. Reichart, T. S. Axelrod, E. Berger, J. S. Bloom, J. Busche, T. Cline, A. Diercks, S. G. Djorgovski, D. A. Frail, A. Gal-Yam, J. Halpern, J. A. Holtzman, M. Hunt, K. Hurley, B. Jacoby, R. Kimble, S. R. KulkarniN. Mirabal, G. Morrison, E. Ofek, O. Pevunova, R. Sari, B. P. Schmidt, D. Turnshek, S. Yost

*Corresponding author for this work

Research output: Contribution to journalArticlepeer-review

43 Scopus citations


We present multicolor light curves of the optical afterglow of gamma-ray burst (GRB) 000926. Beginning ∼1.5 days after the burst, the light curves of this GRB steepen measurably. The existence of such achromatic breaks is usually taken to be an important observational signature that the ejecta are not expanding isotropically but rather have a collimated jetlike geometry. If we interpret the data ir this context, we derive an opening angle of 5°, which reduces the energy release compared with an isotropic model by a factor of ∼275, to 1.7 × 1051 ergs. To fit the data with a simple jet model requires extinction along the line of sight. The derived Av is in the range 0.11-0.82 mag, depending on the adopted extinction law and whether the electrons giving rise to the optical emission are undergoing synchrotron cooling or not. Since this is in excess of the expected extinction from our Galaxy, we attribute this to the GRB host. We note that this extinction is typical of a galactic disk, and therefore the event likely took place in the disk of its host.

Original languageAmerican English
Pages (from-to)L7-L10
JournalAstrophysical Journal
Issue number1 PART 2
StatePublished - 1 Mar 2001
Externally publishedYes

Bibliographical note

Funding Information:
We thank the staff of the Palomar, Keck, MDM, and Wise Observatories and also L. Cowie, A. Barger, R. Ellis, C. Steidel, and B. Madore for their assistance in obtaining observations. We thank E. Mazets and the Konus team for the IPN data. F. A. H. acknowledges support from a Presidential Early Career award. S. R. K., S. G. D., and J. P. H. thank NSF for support of their ground-based GRB programs. K. H. is grateful for Ulysses support under JPL contract 958056 and NEAR support under NAG5-9503.


  • Cosmology: Observations
  • Galaxies: ISM
  • Gamma rays: Bursts


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