Статья

Early‐Time Observations of the GRB 050319 Optical Transient

R. M. QuimbyDepartment of Astronomy, University of Texas, Austin, TX 78712E. S. RykoffUniversity of Michigan, 2477 Randall Laboratory, 450 Church Street, Ann Arbor, MI 48104S. A. YostUniversity of Michigan, 2477 Randall Laboratory, 450 Church Street, Ann Arbor, MI 48104Felix AharonianMax-Planck-Institut für Kernphysik, Saupfercheckweg 1, 69117 Heidelberg, GermanyC. W. AkerlofUniversity of Michigan, 2477 Randall Laboratory, 450 Church Street, Ann Arbor, MI 48104Katherine AlataloAstronomy, 601 Campbell Hall, University of California, Berkeley, CA 94720M. C. B. AshleySchool of Physics, Department of Astrophysics and Optics, University of New South Wales, Sydney, NSW 2052, AustraliaErsin GöğüşSabancι University, Orhanlι-Tuzla 34956, Istanbul, TurkeyTolga GüverIstanbul University Science Faculty, Department of Astronomy and Space Sciences, 34119, University of Istanbul, TurkeyD. HornsMax-Planck-Institut für Kernphysik, Saupfercheckweg 1, 69117 Heidelberg, GermanyR. KehoeDepartment of Physics, Southern Methodist University, Dallas, TX 75275U. KιzιloğluMiddle East Technical University, 06531 Ankara, TurkeyT. A. McKayUniversity of Michigan, 2477 Randall Laboratory, 450 Church Street, Ann Arbor, MI 48104M. E. ÖzelÇanakkale Onsekiz Mart Üniversitesi, Terzioğlu 17020, Çanakkale, TurkeyA. PhillipsSchool of Physics, Department of Astrophysics and Optics, University of New South Wales, Sydney, NSW 2052, AustraliaB. E. SchaeferDepartment of Physics and Astronomy, Louisiana State University, Baton Rouge, LA 70803D. A. SmithGuilford College, 5800 West Friendly Avenue, Greensboro, NC 27410H. SwanUniversity of Michigan, 2477 Randall Laboratory, 450 Church Street, Ann Arbor, MI 48104W. T. VestrandLos Alamos National Laboratory, NIS-2 MS D436, Los Alamos, NM 87545J. Craig WheelerDepartment of Astronomy, University of Texas, Austin, TX 78712J. WrenLos Alamos National Laboratory, NIS-2 MS D436, Los Alamos, NM 87545

2006en

ABI

Аннотация

We present the unfiltered ROTSE-III light curve of the optical transient associated with GRB 050319 beginning 4 s after the cessation of gamma-ray activity. We fit a power-law function to the data using the revised trigger time given by Chincarini et al. (2005), and a smoothly broken power-law to the data using the original trigger disseminated through the GCN notices. Including the RAPTOR data from Wozniak et al. (2005), the best fit power-law indices are alpha=-0.854 (+/- 0.014) for the single power-law and alpha_1=-0.364 (+/- 0.020), alpha_2= -0.881 (+/- 0.030), with a break at t_b = 418 (+/- 30) s for the smoothly broken fit. We discuss the fit results with emphasis placed on the importance of knowing the true start time of the optical transient for this multi-peaked burst. As Swift continues to provide prompt GRB locations, it becomes more important to answer the question, "when does the afterglow begin" to correctly interpret the light curves.

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Идентификаторы

DOI: 10.1086/499803

Цитирования и источники

Цитирований: 2Использованных источников: 0

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