Ferrero 2008 GRB 060605 的余辉观测

主要内容:


精彩摘抄:
余辉的位置
余辉光变曲线，上面的是光学，下面的是X射线。
光学在其它暴中的位置

文章信息:

· arXiv e-print (arXiv:0804.2457)

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Title:		Analysing afterglows using integral field spectroscopy: GRB 060605, the first practical example
Authors:		Ferrero, Patrizia; Klose, Sylvio; Kann, David Alexander; Savaglio, Sandra; Palazzi, Eliana; Maiorano, Elisabetta; Böhm, Petra; Schulze, Steve; Grupe, Dirk; Oates, Samantha R.; Sánchez, Sebastián F.; Amati, Lorenzo; Greiner, Jochen; Hjorth, Jens; Malesani, Daniele; Barthelmy, Scott D.; Gorosabel, Javier; Masetti, Nicola; Roth, Martin M.
Publication:		eprint arXiv:0804.2457
Publication Date:		04/2008
Origin:		ARXIV
Keywords:		Astrophysics
Comment:		Submitted to A&A
Bibliographic Code:		2008arXiv0804.2457F

Abstract

GRB 060605 was a long and relatively faint gamma-ray burst detected by \emph{Swift}/BAT with a duration of about 20 sec. Its afterglow could be observed with \emph{Swift}/XRT for nearly 1 day while \emph{Swift}/UVOT could detect the afterglow during the first 6 hours after the event. Here, we report on integral field spectroscopy of its afterglow performed with PMAS/PPak mounted at the Calar Alto 3.5 m telescope. In addition, we report on a detailed analysis of XRT and UVOT data and on the results of deep late-time VLT observations, which reveal the GRB host galaxy. We find that the burst occured at a redshift of $z$=3.773, possibly associated with a faint, $R_C=26.4 \pm 0.3$ host. Based on the optical and X-ray data we deduce information on the SED of the afterglow, the position of the cooling frequency in the SED, the nature of the circumburst environment, its collimation factor, and its energetics. We find that the GRB fireball was expanding into a constant-density medium and that the explosion was collimated with a narrow half-opening angle of about 2.3 degrees. The initial Lorentz factor of the fireball was about 250, its beaming-corrected energy release in the gamma-ray band was comparably low, however. The optical as well as the X-ray afterglow, on the other hand, were rather luminous. Finally, we find that within the error bars the data is consistent with an achromatic evolution of the afterglow during the suspected jet break time at about 0.24 days after the burst.}

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