Kann 2008 详细的长短暴余辉比较

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· arXiv e-print (arXiv:0804.1959)

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Title:		The Afterglows of Swift-era Gamma-Ray Bursts. II. Short/Hard (Type I) vs. Long/Soft (Type II) Optical Afterglows
Authors:		Kann, D. A.; Klose, S.; Zhang, B.; Wilson, A. C.; Butler, N. R.; Malesani, D.; Nakar, E.; Antonelli, L. A.; Chincarini, G.; Cobb, B. E.; Covino, S.; D'Avanzo, P.; D'Elia, V.; Della Valle, M.; Ferrero, P.; Fugazza, D.; Gorosabel, J.; Israel, . L.; Mannucci, F.; Piranomonte, S.; Schulze, S.; Stella, L.; Tagliaferri, G.; Wiersema, K.
Publication:		eprint arXiv:0804.1959
Publication Date:		04/2008
Origin:		ARXIV
Keywords:		Astrophysics
Comment:		Submitted to ApJ; 70 pages in referee format; 28 pages main text, 13 pages Appendix, 15 pages references, 2 tables, 10 figures; Figures 1 and 2 downgraded to fit arXiv space restrictions
Bibliographic Code:		2008arXiv0804.1959K

Abstract

We use a large sample of Gamma-Ray Burst (GRB) afterglow and prompt emission data to compare the optical afterglows (or the lack thereof) of ``short/hard'' Type I GRBs (those that are assumed not to be due to the death of massive stars, but, e.g., merger of compact objects) with those of ``long/soft'' Type II GRBs (those due to the core collapse of massive stars). In comparison to the afterglows of Type II GRBs, we find that those of Type I GRBs have a lower average luminosity and show a larger intrinsic spread of luminosities. From late and deep upper limits on the optical transients, we establish limits on the maximum optical luminosity of any associated supernova, confirming older works and adding new results. We use deep upper limits on Type I GRB optical afterglows to constrain the parameter space of possible Mini-SN emission associated with a compact-object merger. Using the prompt emission data, we search for correlations between the parameters of the prompt emission and the late optical afterglow luminosities. We find trends between the bolometric isotropic energy release and the optical afterglow luminosity at a fixed time after trigger, and between the host offset and the luminosity, bit no significant trend between the isotropic energy release and the duration of the GRBs. We also discuss three anomalous GRBs, GRB 060121, GRB 060505, and GRB 060614, in the light of their optical afterglow luminosities.

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