Several gamma-ray bursts (GRBs) last much longer (hours) in γ-rays than typical long GRBs (minutes), and it has recently been proposed that these "ultra-long GRBs" may form a distinct population, probably with a different (e.g., blue supergiant) progenitor than typical GRBs. However, Swift observations suggest that many GRBs have extended central engine activities manifested as flares and internal plateaus in X-rays. We perform a comprehensive study on a large sample of Swift GRBs with X-Ray Telescope observations to investigate GRB central engine activity duration and to determine whether ultra-long GRBs are unusual events. We define burst duration tburst based on both γ-ray and X-ray light curves rather than using γ-ray observations alone. We find that tburst can be reliably measured in 343 GRBs. Within this "good" sample, 21.9% GRBs have tburst ≳ 103 s and 11.5% GRBs have tburst ≳ 10 4 s. There is an apparent bimodal distribution of tburst in this sample. However, when we consider an "undetermined" sample (304 GRBs) with tburst possibly falling in the gap between GRB duration T 90 and the first X-ray observational time, as well as a selection effect against tburst falling into the first Swift orbital "dead zone" due to observation constraints, the intrinsic underlying t burst distribution is consistent with being a single component distribution. We found that the existing evidence for a separate ultra-long GRB population is inconclusive, and further multi-wavelength observations are needed to draw a firmer conclusion. We also discuss the theoretical implications of our results. In particular, the central engine activity duration of GRBs is generally much longer than the γ-ray T 90 duration and it does not even correlate with T 90. It would be premature to make a direct connection between T 90 and the size of the progenitor star.
All Science Journal Classification (ASJC) codes
- Astronomy and Astrophysics
- Space and Planetary Science