Maqola

<i>Swift</i>and<i>XMM‐Newton</i>Observations of the Extraordinary Gamma‐Ray Burst 060729: More than 125 Days of X‐Ray Afterglow

D. GrupeDepartment of Astronomy and Astrophysics, Pennsylvania State University, University Park, PA 16802C. GronwallDepartment of Astronomy and Astrophysics, Pennsylvania State University, University Park, PA 16802Xiangyu WangDepartment of Astronomy and Astrophysics, Pennsylvania State University, University Park, PA 16802Peter W. A. RomingDepartment of Astronomy and Astrophysics, Pennsylvania State University, University Park, PA 16802Jay CummingsAstrophysics Science Division, Astroparticle Physics Laboratory, NASA Goddard Space Flight Center, Greenbelt, MD 20771Bing ZhangDepartment of Physics, University of Nevada, Las Vegas, NV 89154P. MészárosDepartment of Astronomy and Astrophysics, Pennsylvania State University, University Park, PA 16802María Díaz TrigoXMM-Newton Science Operations Centre, European Space Agency, Villafranca del Castillo, 28080 Madrid, SpainP. T. O’BrienDepartment of Physics and Astronomy, University of Leicester, Leicester LE1 7RH, UKK. L. PageDepartment of Physics and Astronomy, University of Leicester, Leicester LE1 7RH, UKAndy BeardmoreDepartment of Physics and Astronomy, University of Leicester, Leicester LE1 7RH, UKO. GodetDepartment of Physics and Astronomy, University of Leicester, Leicester LE1 7RH, UKD. E. vanden BerkDepartment of Astronomy and Astrophysics, Pennsylvania State University, University Park, PA 16802Peter J. BrownDepartment of Astronomy and Astrophysics, Pennsylvania State University, University Park, PA 16802S. KochDepartment of Astronomy and Astrophysics, Pennsylvania State University, University Park, PA 16802David C. MorrisDepartment of Astronomy and Astrophysics, Pennsylvania State University, University Park, PA 16802M. C. StrohDepartment of Astronomy and Astrophysics, Pennsylvania State University, University Park, PA 16802D. N. BurrowsDepartment of Astronomy and Astrophysics, Pennsylvania State University, University Park, PA 16802J. A. NousekDepartment of Astronomy and Astrophysics, Pennsylvania State University, University Park, PA 16802M. ChesterDepartment of Astronomy and Astrophysics, Pennsylvania State University, University Park, PA 16802S. ImmlerAstrophysics Science Division, X-Ray Astrophysical Laboratory, NASA Goddard Space Flight Center, Greenbelt, MD 20771V. ManganoINAF-Istituto di Astrofisica Spaziale e Fisica Cosmica di Palermo, I-90146 Palermo, ItalyP. RomanoINAF-Osservatorio Astronomico di Brera, I-23807 Merate, ItalyG. ChincariniINAF-Osservatorio Astronomico di Brera, I-23807 Merate, ItalyJ. P. OsborneDepartment of Physics and Astronomy, University of Leicester, Leicester LE1 7RH, UKT. SakamotoAstrophysics Science Division, Astroparticle Physics Laboratory, NASA Goddard Space Flight Center, Greenbelt, MD 20771N. GehrelsAstrophysics Science Division, Astroparticle Physics Laboratory, NASA Goddard Space Flight Center, Greenbelt, MD 20771

2007en

ABI

Annotatsiya

We report the results of the Swift andXMM-Newtonobservations of the Swift-discoveredGRB060729 (T90 115 s). The afterglow of this burst was exceptionally bright in X-rays as well as at UV/optical wavelengths, showing an unusually long slow decay phase ( 0:14 0:02), suggesting a larger energy injection phase at early times than in other bursts. The X-ray light curve displays a break at about 60 ks after the burst. The X-ray decay slope after the break is 1:29 0:03. Up to 125 days after the burst we do not detect a jet break, suggesting that the jet opening angle is larger than 28. We find that the X-ray spectra of the early phase change dramatically and can all be fitted by an absorbed singleYpower-law models or alternatively by a blackbody plus power-law model. The power-law fits show that the X-ray spectrum becomes steeper while the absorption column density decreases. In the blackbody model the temperature decreases from kT 0:6 to 0.1 keV between 85 and 160 s after the burst in the rest frame. The afterglow was clearly detected up to 9 days after the burst in all six UVOT filters and in UVW1 even for 31 days. A break at about 50 ks is clearly detected in all six UVOT filters from a shallow decay slope of about 0.3 and a steeper decay slope of 1.3.The XMM-Newton observations started about 12 hr after the burst and show a typical afterglow X-ray spectrum with X 1:1 and absorption column density of 1; 1021 cm2. Subject headinggs: gamma rays: bursts — X-rays: bursts Online material: color figure 1.

Hali tarjima qilinmagan

Identifikatorlar

DOI: 10.1086/517868

Iqtiboslar va manbalar

5 ta iqtibos0 ta foydalanilgan manba

Koʻrsatkichlar — AkademScholar