Статья

Methods and results of an automatic analysis of a complete sample of<i>Swift</i>-XRT observations of GRBs

N. GehrelsX-Ray and Observational Astronomy Group, Department of Physics & Astronomy, University of Leicester, Leicester LE1 7RHA. P. BeardmoreX-Ray and Observational Astronomy Group, Department of Physics & Astronomy, University of Leicester, Leicester LE1 7RHK. L. PageX-Ray and Observational Astronomy Group, Department of Physics & Astronomy, University of Leicester, Leicester LE1 7RHJ. P. OsborneX-Ray and Observational Astronomy Group, Department of Physics & Astronomy, University of Leicester, Leicester LE1 7RHP. T. O’BrienX-Ray and Observational Astronomy Group, Department of Physics & Astronomy, University of Leicester, Leicester LE1 7RHR. WillingaleX-Ray and Observational Astronomy Group, Department of Physics & Astronomy, University of Leicester, Leicester LE1 7RHR. L. C. StarlingX-Ray and Observational Astronomy Group, Department of Physics & Astronomy, University of Leicester, Leicester LE1 7RHD. N. BurrowsDepartment of Astronomy and Astrophysics, Pennsylvania State University, 525 Davey Lab, University Park, PA 16802, USAO. GodetX-Ray and Observational Astronomy Group, Department of Physics & Astronomy, University of Leicester, Leicester LE1 7RHL. VetereDepartment of Astronomy and Astrophysics, Pennsylvania State University, 525 Davey Lab, University Park, PA 16802, USAJ. L. RacusinDepartment of Astronomy and Astrophysics, Pennsylvania State University, 525 Davey Lab, University Park, PA 16802, USAM. R. GoadX-Ray and Observational Astronomy Group, Department of Physics & Astronomy, University of Leicester, Leicester LE1 7RHK. WiersemaX-Ray and Observational Astronomy Group, Department of Physics & Astronomy, University of Leicester, Leicester LE1 7RHL. AngeliniNASA Goddard Space Flight Center, Greenbelt, MD 20771 USAM. CapalbiASI Science Data Center, ASDC c/o ESRIN, via G. Galilei, 00044 Frascati, ItalyG. ChincariniUniversitá degli Studi di Milano‐Bicocca, Dipartimento di Fisica, Piazza della Scienza 3, 20126, Milano, ItalyN. GehrelsNASA Goddard Space Flight Center, Greenbelt, MD 20771 USAJ. A. KenneaDepartment of Astronomy and Astrophysics, Pennsylvania State University, 525 Davey Lab, University Park, PA 16802, USAR. MarguttiINAF, Osservatorio Astronomico di Brera Via E. Bianchi 46, I-23807,Merate (LC), ItalyDavid C. MorrisNASA Goddard Space Flight Center, Greenbelt, MD 20771, USAC. J. MountfordX-Ray and Observational Astronomy Group, Department of Physics & Astronomy, University of Leicester, Leicester LE1 7RHC. PaganiX-Ray and Observational Astronomy Group, Department of Physics & Astronomy, University of Leicester, Leicester LE1 7RHM. PerriASI Science Data Center, ASDC c/o ESRIN, via G. Galilei, 00044 Frascati, ItalyP. RomanoINAF – Istituto di Astrofisica Spaziale e Fisica Cosmica, Via U. La Malfa 153, I-90146 Palermo, Italy,N. R. TanvirX-Ray and Observational Astronomy Group, Department of Physics & Astronomy, University of Leicester, Leicester LE1 7RH

2009en

ABI

Аннотация

We present a homogeneous X-ray analysis of all 318 gamma-ray bursts detected by the X-ray telescope (XRT) on the Swift satellite up to 2008 July 23; this represents the largest sample of X-ray GRB data published to date. In Sections 2–3, we detail the methods which the Swift-XRT team has developed to produce the enhanced positions, light curves, hardness ratios and spectra presented in this paper. Software using these methods continues to create such products for all new GRBs observed by the Swift-XRT. We also detail web-based tools allowing users to create these products for any object observed by the XRT, not just GRBs. In Sections 4–6, we present the results of our analysis of GRBs, including probability distribution functions of the temporal and spectral properties of the sample. We demonstrate evidence for a consistent underlying behaviour which can produce a range of light-curve morphologies, and attempt to interpret this behaviour in the framework of external forward shock emission. We find several difficulties, in particular that reconciliation of our data with the forward shock model requires energy injection to continue for days to weeks.

Идентификаторы

DOI: 10.1111/j.1365-2966.2009.14913.x

Цитирования и источники

Цитирований: 16Использованных источников: 0

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