Swift multi-wavelength observations of the bright flaring burst GRB 051117A

¹ Department of Physics and Astronomy, University of Leicester, LE1 7RH, UK e-mail: mrg@star.le.ac.uk
² NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
³ Pennsylvania State University, University Park, PA 16802, USA
⁴ INAF-Osservatorio Astronomica di Brera, via Bianchi 46, 23807 Merate (LC), Italy
⁵ ASI Science Data Center, Via Galileo Galilei, 00044 Frascati, Italy

Received: 5 December 2006
Accepted: 15 March 2007

Abstract

We report on the temporal and spectral characteristics of the early X-ray emission from the Gamma Ray Burst 051117A as observed by Swift . The superb quality of the early X-ray light-curve and spectra of this source, one of the brightest seen by the X-ray Telescope at such early times, allows an unprecedented look at the spectral and temporal evolution of the prompt and early afterglow emission for this GRB and allows us to place stringent limits on the detection of lines. GRB 051117A displays a highly complex light-curve, with an apparent initial slow decline of slope () dominated by numerous superposed flares of varying amplitude and duration. Between orbits 2 and 3, the X-ray light-curve drops abruptly, highlighting the dominance of flaring activity at early times, and indicating that the central engine for this burst remains active for several kiloseconds after the initial explosion. The late time slope ( s) also decays relatively slowly with a powerlaw index of , breaking to a steeper slope of 1.1, 170 ks after the BAT trigger. The X-ray light-curve at early times is characteristic of a noise process, consisting of random shots superposed on an underlying powerlaw decay, with individual shots well-modelled by a fast-rise and exponential decay spanning a broad range in rise-times and decay rates. A temporal spectral analysis of the early light-curve shows that the photon index and source intensity are highly correlated with the spectrum being significantly harder when brighter, consistent with the movement of the peak of the Band function to lower energies following individual flares. The high quality spectrum obtained from the first orbit of WT mode data, enables us to place a upper limit on the strength of any emission line features of  eV, assuming a narrow emission-line of 100 eV at the peak of the effective area.