Filgas 2010 GRB 080413B的余辉观测

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用双成分的喷流解释增亮。

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Title:		The two-component jet of GRB 080413B
Authors:		Filgas, R.; Krühler, T.; Greiner, J.; Rau, A.; Palazzi, E.; Klose, S.; Schady, P.; Rossi, A.; Afonso, P. M. J.;Antonelli, L. A.; Clemens, C.; Covino, S.; D'Avanzo, P.; Küpcü Yoldaş, A.; Nardini, M.; Nicuesa Guelbenzu, A.;Olivares, F.; Updike, E. A. C.; Yoldaş, A.
Affiliation:		AA(Max-Planck-Institut für extraterrestrische Physik, Giessenbachstraße 1, 85748 Garching, Germany,filgas@mpe.mpg.de), AB(Max-Planck-Institut für extraterrestrische Physik, Giessenbachstraße 1, 85748 Garching, Germany; Universe Cluster, Technische Universität München, Boltzmannstraße 2, 85748 Garching, Germany), AC(Max-Planck-Institut für extraterrestrische Physik, Giessenbachstraße 1, 85748 Garching, Germany), AD(Max-Planck-Institut für extraterrestrische Physik, Giessenbachstraße 1, 85748 Garching, Germany), AE(INAF - IASF di Bologna, via Gobetti 101, 40129 Bologna, Italy), AF(Thüringer Landessternwarte Tautenburg, Sternwarte 5, 07778 Tautenburg, Germany), AG(Max-Planck-Institut für extraterrestrische Physik, Giessenbachstraße 1, 85748 Garching, Germany), AH(Thüringer Landessternwarte Tautenburg, Sternwarte 5, 07778 Tautenburg, Germany), AI(Max-Planck-Institut für extraterrestrische Physik, Giessenbachstraße 1, 85748 Garching, Germany), AJ(INAF - Osservatorio Astronomico di Roma, via di Frascati 33, 00040 Monteporzio Catone (Roma), Italy), AK(Max-Planck-Institut für extraterrestrische Physik, Giessenbachstraße 1, 85748 Garching, Germany), AL(INAF - Osservatorio Astronomico di Brera, via Bianchi 46, 23807 Merate, Italy), AM(INAF - Osservatorio Astronomico di Brera, via Bianchi 46, 23807 Merate, Italy), AN(European Southern Observatory, Karl-Schwarzschild-Straße 2, 85748 Garching, Germany ; Institute of Astronomy, University of Cambridge, Madingley Road, CB3 0HA Cambridge, UK), AO(Max-Planck-Institut für extraterrestrische Physik, Giessenbachstraße 1, 85748 Garching, Germany), AP(Thüringer Landessternwarte Tautenburg, Sternwarte 5, 07778 Tautenburg, Germany), AQ(Max-Planck-Institut für extraterrestrische Physik, Giessenbachstraße 1, 85748 Garching, Germany), AR(Department of Physics and Astronomy, Clemson University, Clemson, SC 29634-0978, USA), AS(Max-Planck-Institut für extraterrestrische Physik, Giessenbachstraße 1, 85748 Garching, Germany; Institute of Astronomy, University of Cambridge, Madingley Road, CB3 0HA Cambridge, UK)
Publication:		Astronomy and Astrophysics, Volume 526, id.A113 (A&A Homepage)
Publication Date:		02/2011
Origin:		EDP Sciences
Keywords:		ISM: jets and outflows, gamma rays: general, X-rays: individuals: GRB 080413B
DOI:		10.1051/0004-6361/201015320
Bibliographic Code:		2011A&A...526A.113F

Abstract

Aims: The quick and precise localization of GRBs by the Swift telescope allows the early evolution of the afterglow light curve to be captured by ground-based telescopes. With GROND measurements we can investigate the optical/near-infrared light curve of the afterglow of gamma-ray burst 080413B in the context of late rebrightening.
Methods: Multi-wavelength follow-up observations were performed on the afterglow of GRB 080413B. X-ray emission was detected by the X-ray telescope onboard the Swift satellite and obtained from the public archive. Optical and near-infrared photometry was performed with the seven-channel imager GROND mounted at the MPG/ESO 2.2 m telescope and additionally with the REM telescope, both in La Silla, Chile. The light curve model was constructed using the obtained broad-band data.
Results: The broad-band light curve of the afterglow of GRB 080413B is well fitted with an on-axis two-component jet model. The narrow ultra-relativistic jet is responsible for the initial decay, while the rise of the moderately relativistic wider jet near its deceleration time is the cause of the rebrightening of the light curve. The later evolution of the optical/NIR light curve is then dominated by the wide component, the signature of which is almost negligible in the X-ray wavelengths. These components have opening angles of θ_n ~ 1.7° and θ_w ~ 9°, and Lorentz factors of Γ_n > 188 and Γ_w ~ 18.5. We calculated the beaming-corrected energy release to be E_γ = 7.9 × 10⁴⁸ erg.Tables 1-3 are only available in electronic form at http://www.aanda.org

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