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Zoekopdracht: journal id: "astrophysicalxjournal"

AuteursM.S. Briggs, D.L. Band, R.M. Kippen, R.D. Preece, C. Kouveliotou, J.A. van Paradijs, G.H. Share, R.J. Murphy, S.M. Matz, A. Connors, C. Winkler, M.L. McConnel, J.M. Ryan, O.R. Williams, C.A. Young, B. Dingus, J.R. Catelli, R.A.M.J. Wijers
TitelObservations of GRB 990123 by the Compton gamma ray observatory
TijdschriftAstrophysical Journal
Jaargang524
Jaar1999
Nummer1
Pagina's82-91
ISSN0004637X
FaculteitFaculteit der Natuurwetenschappen, Wiskunde en Informatica
Instituut/afd.FNWI: Astronomical Institute Anton Pannekoek (IAP)
TrefwoordenGamma ray bursts; X-ray bursts
SamenvattingGRB 990123 was the first burst from which simultaneous optical, X-ray, and gamma-ray emission was detected; its afterglow has been followed by an extensive set of radio, optical, and X-ray observations. We have studied the gamma-ray burst itself as observed by the Compton Gamma Ray Observatory detectors. We find that gamma-ray fluxes are not correlated with the simultaneous optical observations and that the gamma-ray spectra cannot be extrapolated simply to the optical fluxes. The burst is well fitted by the standard four-parameter GRB function, with the exception that excess emission compared with this function is observed below ~15 keV during some time intervals. The burst is characterized by the typical hard-to-soft and hardness-intensity correlation spectral evolution patterns. The energy of the peak of the nuf_nu spectrum, E_p, reaches an unusually high value during the first intensity spike, 1470+/-110 keV, and then falls to ~300 keV during the tail of the burst. The high-energy spectrum above ~1 MeV is consistent with a power law with a photon index of about -3. By fluence, GRB 990123 is brighter than all but 0.4% of the GRBs observed with BATSE, clearly placing it on the -3/2 power-law portion of the intensity distribution. However, the redshift measured for the afterglow is inconsistent with the Euclidean interpretation of the -3/2 power law. Using the redshift value of >=1.61 and assuming isotropic emission, the gamma-ray energy exceeds 10^54 ergs.
Opmerkingen©1999 The American Astronomical Society
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