GRB radiative efficiencies derived from the swift data: GRBs versus XRFs, long versus short

Abstract

We systematically analyze the prompt emission and the early afterglow data of a sample of 31 GRBs detected by Swift before 2005 September and estimate the GRB radiative efficiency. B AT's narrow band inhibits a precise determination of the GRB spectral parameters, and we have developed a method to estimate these parameters with the hardness ratio information. The shallow decay component commonly existing in early X-ray afterglows, if interpreted as continuous energy injection in the external shock, suggests that the GRB efficiencies previously derived from the late-time X-ray data were not reliable. We calculate two radiative efficiencies using the afterglow kinetic energy E<inf>K</inf> derived at the putative deceleration time (t<inf>dec</inf>) and at the break time (t<inf>b</inf>), when the energy injection phase ends, respectively. At t <inf>b</inf> XRFs appear to be less efficient than normal GRBs. However, when we analyze the data at t<inf>dec</inf>, XRFs are found to be as efficient as GRBs. Short GRBs have similar radiative efficiencies to long GRBs despite of their different progenitors. Twenty-two bursts in the sample are identified to have the afterglow cooling frequency below the X-ray band. Assuming ε<inf>e</inf> = 0.1, we find η<inf>γ</inf>(t<inf>b</inf>) usually <10% and η<inf>γ</inf>(t<inf>dec</inf>) varying from a few percent to >90%. Nine GRBs in the sample have the afterglow cooling frequency above the X-ray band for a very long time. This suggests a very small ε<inf>B</inf> and/or a very low ambient density n. © 2007. The American Astronomical Society. All rights reserved.