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GRB 050117: Simultaneous Gamma‐Ray and X‐Ray Observations with the<i>Swift</i>Satellite

J. E. HillNASA Goddard Space Flight Center, Greenbelt, MD 20771David C. MorrisDepartment of Astronomy and Astrophysics, 525 Davey Laboratory, Pennsylvania State University, University Park, PA 16802T. SakamotoNASA Goddard Space Flight Center, Greenbelt, MD 20771Goro SatoInstitute of Space and Astronautical Science/Japan Aerospace Exploration Agency, Building A, Room 1453, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 229-8510, JapanD. N. BurrowsDepartment of Astronomy and Astrophysics, 525 Davey Laboratory, Pennsylvania State University, University Park, PA 16802L. AngeliniDepartment of Physics and Astronomy, The Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218C. PaganiDepartment of Astronomy and Astrophysics, 525 Davey Laboratory, Pennsylvania State University, University Park, PA 16802A. MorettiINAF-Osservatorio Astronomico di Brera, Via Bianchi 46, 23807 Merate, ItalyA. F. AbbeySpace Research Centre, University of Leicester, Leicester LE1 7RH, UKA. P. BeardmoreDepartment of Physics and Astronomy, University of Leicester, Leicester LE1 7RH, UKVadim BiryukovS. CampanaINAF-Osservatorio Astronomico di Brera, Via Bianchi 46, 23807 Merate, ItalyM. CapalbiG. CusumanoINAF-Istituto di Astrofisica Spaziale e Fisica Cosmica Sezione di Palermo, Via Ugo La Malfa 153, 90146 Palermo, ItalyP. GiommiM. IbrahimovUlugh Beg Astronomical Institute, Tashkent 700052, UzbekistanJ. A. KenneaDepartment of Astronomy and Astrophysics, 525 Davey Laboratory, Pennsylvania State University, University Park, PA 16802S. KobayashiCenter for Gravitational Wave Physics, Pennsylvania State University, University Park, PA 16802Kunihito IokaCenter for Gravitational Wave Physics, Pennsylvania State University, University Park, PA 16802C. B. MarkwardtNASA Goddard Space Flight Center, Greenbelt, MD 20771P. MészárosDepartment of Astronomy and Astrophysics, 525 Davey Laboratory, Pennsylvania State University, University Park, PA 16802P. 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, UKA. PozanenkoSpace Research Institute, Moscow 117810, RussiaM. PerriV. RumyantsevCrimean Astrophysical Observatory, UkraineP. SchadyDmitri A. SharapovUlugh Beg Astronomical Institute, Tashkent 700052, UzbekistanG. TagliaferriINAF-Osservatorio Astronomico di Brera, Via Bianchi 46, 23807 Merate, ItalyBing ZhangDepartment of Physics, University of Nevada, Box 454002, Las Vegas, NV 89154-4002G. ChincariniINAF-Osservatorio Astronomico di Brera, Via Bianchi 46, 23807 Merate, ItalyN. GehrelsNASA Goddard Space Flight Center, Greenbelt, MD 20771Alan WellsDepartment of Astronomy and Astrophysics, 525 Davey Laboratory, Pennsylvania State University, University Park, PA 16802J. A. NousekDepartment of Astronomy and Astrophysics, 525 Davey Laboratory, Pennsylvania State University, University Park, PA 16802

The Astrophysical Journaljournal2006en

ABI

Annotatsiya

The Swift Gamma-Ray Burst Explorer performed its first autonomous, X-ray follow-up to a newly detected GRB on 2005 January 17, within 193 seconds of the burst trigger by the Swift Burst Alert Telescope. While the burst was still in progress, the X-ray Telescope obtained a position and an image for an un-catalogued X-ray source; simultaneous with the gamma-ray observation. The XRT observed flux during the prompt emission was 1.1 x 10^{-8} ergs cm^{-2} s^{-1} in the 0.5-10 keV energy band. The emission in the X-ray band decreased by three orders of magnitude within 700 seconds, following the prompt emission. This is found to be consistent with the gamma-ray decay when extrapolated into the XRT energy band. During the following 6.3 hours, the XRT observed the afterglow in an automated sequence for an additional 947 seconds, until the burst became fully obscured by the Earth limb. A faint, extremely slowly decaying afterglow, alpha=-0.21$, was detected. Finally, a break in the lightcurve occurred and the flux decayed with alpha<-1.2$. The X-ray position triggered many follow-up observations: no optical afterglow could be confirmed, although a candidate was identified 3 arcsecs from the XRT position.

Mavzular

Gamma-ray bursts and supernovae Pulsars and Gravitational Waves Research Astrophysical Phenomena and Observations

Identifikatorlar

DOI: 10.1086/498443

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