Guidorzi 2009 GRB/XRF 080330的观测

主要内容:
说可能是一个偏轴的伽玛暴

精彩摘抄:


文章信息:

· Find Similar Abstracts (with default settings below)

· arXiv e-print (arXiv:0903.2958)

· References in the Article

·

· Translate This Page

Title:		Rise and fall of the X-ray flash 080330: an off-axis jet?
Authors:		Guidorzi, C.; Clemens, C.; Kobayashi, S.; Granot, J.; Melandri, A.; D'Avanzo, P.; Kuin, N. P. M.; Klotz, A.; Fynbo, J. P. U.; Covino, S.; Greiner, J.; Malesani, D.; Mao, J.; Mundell, C. G.; Steele, I. A.; Jakobsson, P.; Margutti, R.; Bersier, D.; Campana, S.; Chincarini, G.; D'Elia, V.; Fugazza, D.; Genet, F.; Gomboc, A.; Kruehler, T.; Kupcu Yoldacs, A.; Moretti, A.; Mottram, C. J.; O'Brien, P. T.; Smith, R. J.; Szokoly, G.; Tagliaferri, G.; Tanvir, N. R.; Gehrels, N.
Publication:		eprint arXiv:0903.2958
Publication Date:		03/2009
Origin:		ARXIV
Keywords:		Astrophysics - High Energy Astrophysical Phenomena
Comment:		accepted to A&A, 19 pages, 11 figures
Bibliographic Code:		2009arXiv0903.2958G

Abstract

X-ray flashes (XRFs) are a class of gamma-ray bursts (GRBs) with the peak energy of the time-integrated spectrum, Ep, below 30 keV, whereas classical GRBs have Ep of a few hundreds keV. Apart from Ep and the lower luminosity, the properties of XRFs are typical of the classical GRBs. Yet, the nature of XRFs and the differences from that of GRBs are not understood. In addition, there is no consensus on the interpretation of the shallow decay phase observed in most X-ray afterglows of both XRFs and GRBs. We examine in detail the case of XRF 080330 discovered by Swift at the redshift of 1.51. This burst is representative of the XRF class and exhibits an X-ray shallow decay. The rich and broadband (from NIR to UV) photometric data set we collected across this phase makes it an ideal candidate to test the off-axis jet interpretation proposed to explain both the softness of XRFs and the shallow decay phase. We present prompt gamma-ray, early and late IR/visible/UV and X-ray observations of the XRF 080330. We derive a SED from NIR to X-ray bands across the plateau phase with a power-law index of 0.79 +- 0.01 and negligible rest-frame dust extinction. The multi-wavelength evolution of the afterglow is achromatic from ~10^2 s out to ~8x10^4 s. We describe the temporal evolution of the multi-wavelength afterglow within the context of the standard afterglow model and show that a single-component jet viewed off-axis explains the observations (abriged).

---

Bibtex entry for this abstract Preferred format for this abstract (see Preferences)