Xu 2008 无超新星成协的GRB 060505和GRB 060614的余辉

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加了最新观测的数据

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Title:		In search of progenitors for supernova-less GRBs 060505 and 060614: re-examination of their afterglows
Authors:		Xu, D.; Starling, R. L. C.; Fynbo, J. P. U.; Sollerman, J.; Yost, S.; Watson, D.; Foley, S.; O'Brien, P. T.; Hjorth, J.
Publication:		eprint arXiv:0812.0979
Publication Date:		12/2008
Origin:		ARXIV
Keywords:		Astrophysics
Comment:		15 pages, 6 figures, 4 tables, submitted to ApJ
Bibliographic Code:		2008arXiv0812.0979X

Abstract

GRB060505 and GRB060614 are nearby long-duration gamma-ray bursts (LGRBs) without accompanying supernovae (SNe) down to very strict limits. They thereby challenge the conventional LGRB-SN connection and naturally give rise to the question: are there other peculiar features in their afterglows which would help shed light on their progenitors? To answer this question, we combine new observational data with published data and investigate the multi-band temporal and spectral properties of the two afterglows. We find that both afterglows can be well interpreted within the framework of the jetted standard external shock wave model, and that the afterglow parameters for both bursts fall well within the range observed for other LGRBs. Hence, from the properties of the afterglows there is nothing to suggest that these bursts should have another progenitor than other LGRBs. Recently, GRB080503 has been found to be a spike + tail burst similar to GRB060614. We analyse the prompt emission of this burst and find that this GRB is a hard-spike + hard-tail burst with a spectral lag of 0.8+/-0.4 s during its tail emission. Thus, GRB060614, featuring hard-spike + soft-tail and negligible lag, would be different from the new burst if these properties referred for GRB progenitor classification. Finally we note that, whereas the progenitor of the two SN-less bursts remains uncertain, the core-collapse origin for such bursts would be quite certain if a wind-like environment can be observationally established, e.g, from an optical decay faster than the X-ray decay in the afterglow's slow cooling phase.

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