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<i>Swift</i>Observations of the X‐Ray–Bright GRB 050315

S. VaughanDepartment of Physics and Astronomy, University of Leicester, Leicester LE1 7RH, UKM. R. GoadDepartment of Physics and Astronomy, University of Leicester, Leicester LE1 7RH, UKA. P. BeardmoreDepartment of Physics and Astronomy, University of Leicester, Leicester LE1 7RH, UKP. T. O’BrienDepartment of Physics and Astronomy, University of Leicester, Leicester LE1 7RH, UKJ. P. OsborneDepartment of Physics and Astronomy, University of Leicester, Leicester LE1 7RH, UKK. L. PageDepartment of Physics and Astronomy, University of Leicester, Leicester LE1 7RH, UKD. N. BurrowsDepartment of Astronomy and Astrophysics, Pennsylvania State University, 525 Davey Lab, University Park, PA 16802S. CampanaINAF-Osservatorio Astronomico di Brera, Via Bianchi 46, 23807 Merate, ItalyJ. K. CannizzoJoint Center for Astrophysics, University of Maryland, Baltimore County, Baltimore, MD 21250M. CapalbiG. ChincariniINAF-Osservatorio Astronomico di Brera, Via Bianchi 46, 23807 Merate, ItalyJ. R. CummingsNASA Goddard Space Flight Center, Greenbelt, MD 20771G. CusumanoINAF-Istituto di Astrofisica Spaziale e Fisica Cosmica Sezione di Palermo, Via Ugo La Malfa 153, I-90146 Palermo, ItalyP. GiommiO. GodetDepartment of Physics and Astronomy, University of Leicester, Leicester LE1 7RH, UKJ. E. HillNASA Goddard Space Flight Center, Greenbelt, MD 20771S. KobayashiDepartment of Astronomy and Astrophysics, Pennsylvania State University, 525 Davey Lab, University Park, PA 16802Pawan KumarDepartment of Astronomy, University of Texas, Austin, TX 78712V. La ParolaINAF-Istituto di Astrofisica Spaziale e Fisica Cosmica Sezione di Palermo, Via Ugo La Malfa 153, I-90146 Palermo, ItalyA. J. LevanDepartment of Physics and Astronomy, University of Leicester, Leicester LE1 7RH, UKV. ManganoINAF-Istituto di Astrofisica Spaziale e Fisica Cosmica Sezione di Palermo, Via Ugo La Malfa 153, I-90146 Palermo, ItalyP. MészárosDepartment of Astronomy and Astrophysics, Pennsylvania State University, 525 Davey Lab, University Park, PA 16802A. MorettiINAF-Osservatorio Astronomico di Brera, Via Bianchi 46, 23807 Merate, ItalyD. MorrisDepartment of Astronomy and Astrophysics, Pennsylvania State University, 525 Davey Lab, University Park, PA 16802J. A. NousekDepartment of Astronomy and Astrophysics, Pennsylvania State University, 525 Davey Lab, University Park, PA 16802C. PaganiDepartment of Astronomy and Astrophysics, Pennsylvania State University, 525 Davey Lab, University Park, PA 16802D. M. PalmerLos Alamos National Laboratory, P.O. Box 1663, Los Alamos, NM 87545J. L. RacusinDepartment of Astronomy and Astrophysics, Pennsylvania State University, 525 Davey Lab, University Park, PA 16802P. RomanoINAF-Osservatorio Astronomico di Brera, Via Bianchi 46, 23807 Merate, ItalyG. TagliaferriINAF-Osservatorio Astronomico di Brera, Via Bianchi 46, 23807 Merate, ItalyBing ZhangDepartment of Physics, University of Nevada, Box 454002, Las Vegas, NV 89154-4002N. GehrelsNASA Goddard Space Flight Center, Greenbelt, MD 20771

2006en

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Annotatsiya

This paper discusses Swift observations of the gamma-ray burst GRB 050315 (z=1.949) from 80 s to 10 days after the onset of the burst. The X-ray light curve displayed a steep early decay (t^-5) for ~200 s and several breaks. However, both the prompt hard X-ray/gamma-ray emission (observed by the BAT) and the first ~ 300 s of X-ray emission (observed by the XRT) can be explained by exponential decays, with similar decay constants. Extrapolating the BAT light curve into the XRT band suggests the rapidly decaying, early X-ray emission was simply a continuation of the fading prompt emission; this strong similarity between the prompt gamma-ray and early X-ray emission may be related to the simple temporal and spectral character of this X-ray rich GRB. The prompt (BAT) spectrum was a steep down to 15 keV, and appeared to continue through the XRT bandpass, implying a low peak energy, inconsistent with the Amati relation. Following the initial steep decline the X-ray afterglow did not fade for ~1.2*10^4 s, after which time it decayed with a temporal index of alpha ~ 0.7, followed by a second break at ~2.5*10^5 s to a slope of alpha ~ 2. The apparent `plateau' in the X-ray light curve, after the early rapid decay, makes this one of the most extreme examples of the steep-flat-steep X-ray light curves revealed by Swift. If the second afterglow break is identified with a jet break then the jet opening angle was theta_0 ~ 5 deg, and implying E_gamma > 10^50 erg.

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DOI: 10.1086/499069

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