Article

Prompt and Afterglow Emission Properties of Gamma‐Ray Bursts with Spectroscopically Identified Supernovae

Yuki KanekoUniversities Space Research Association, NSSTC, VP62, 320 Sparkman Drive, Huntsville, AL 35805E. Ramírez-RuizChandra FellowJonathan GranotKavli Institute for Particle Astrophysics and Cosmology, Stanford University, P.O. Box 20450, Mail Stop 29, Stanford, CA 94309C. KouveliotouNASA MSFC, NSSTC, VP62, 320 Sparkman Drive, Huntsville, AL 35805S. E. WoosleyDepartment of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064S. PatelNASA MSFC, NSSTC, VP62, 320 Sparkman Drive, Huntsville, AL 35805E. RolDepartment of Physics and Astronomy, University of Leicester, University Road, Leicester LE1 RH7, UKJ. J. M. in ’t ZandSRON Netherlands Institute for Space Research, Sorbonnelaan 2, 3584 CA, Utrecht, Netherlands; and Astronomical Institute, Utrecht University, P.O. Box 80,000, 3508 TA, Utrecht, NetherlandsA. J. van der HorstAstronomical Institute, University of Amsterdam, Kruislaan 403, 1098SJ Amsterdam, NetherlandsR. A. M. J. WijersAstronomical Institute, University of Amsterdam, Kruislaan 403, 1098SJ Amsterdam, NetherlandsR. G. StromASTRON, P.O. Box 2, 7990 AA Dwingeloo, Netherlands

2006en

ABI

Abstract

We present a detailed spectral analysis of the prompt and afterglow emission of four nearby long-soft gamma-ray bursts (GRBs 980425, 030329, 031203, and 060218) that were spectroscopically found to be associated with type Ic supernovae, and compare them to the general GRB population. For each event, we investigate the spectral and luminosity evolution, and estimate the total energy budget based upon broadband observations. The observational inventory for these events has become rich enough to allow estimates of their energy content in relativistic and sub-relativistic form. The result is a global portrait of the effects of the physical processes responsible for producing long-soft GRBs. In particular, we find that the values of the energy released in mildly relativistic outflows appears to have a significantly smaller scatter than those found in highly relativistic ejecta. This is consistent with a picture in which the energy released inside the progenitor star is roughly standard, while the fraction of that energy that ends up in highly relativistic ejecta outside the star can vary dramatically between different events.

Identifiers

DOI: 10.1086/508324

Citations and references

Cited by 20 references

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