Ofek 2007 短暴GRB 060505的观测

主要内容:
认为此暴可能是在恒星形成区的短暴。红移0.09。但是也可能是一个没有超新星成协的长暴。

精彩摘抄:


文章信息:
GRB 060505: A possible short-duration gamma-ray burst in a star forming region at redshift of 0.09

Authors: E. O. Ofek, S. B. Cenko, A. Gal-Yam, D. B. Fox, E. Nakar, A. Rau, D. A. Frail, S. R. Kulkarni, P. A. Price, B. P. Schmidt, A. M. Soderberg, B. Peterson, E. Berger, K. Sharon, O. Shemmer, B. E. Penprase, R. A. Chevalier, P. J. Brown, D. N. Burrows, N. Gehrels, F. Harrison, S. T. Holland, V. Mangano, P. J. McCarthy, D.-S. Moon, J. A. Nousek, S. E. Persson, T. Piran, R. Sari

(Submitted on 8 Mar 2007)

Abstract: On 2006 May 5, a four second duration, low energy, ~10^49 erg, Gamma-Ray Burst (GRB) was observed, spatially associated with a z=0.0894 galaxy. Here, we report the discovery of the GRB optical afterglow and observations of its environment using Gemini-south, Hubble Space Telescope (HST), Chandra, Swift and the Very Large Array. The optical afterglow of this GRB is spatially associated with a prominent star forming region in the Sc-type galaxy 2dFGRS S173Z112. Its proximity to a star forming region suggests that the progenitor delay time, from birth to explosion, is smaller than about 10 Myr. Our HST deep imaging rules out the presence of a supernova brighter than an absolute magnitude of about -11 (or -12.6 in case of ``maximal'' extinction) at about two weeks after the burst, and limits the ejected mass of radioactive Nickel 56 to be less than about 2x10^-4 solar mass (assuming no extinction). Although it was suggested that GRB 060505 may belong to a new class of long-duration GRBs with no supernova, we argue that the simplest interpretation is that the physical mechanism responsible for this burst is the same as for short-duration GRBs.

Comments:

7 pages, 3 figures, ApJ submitted

Subjects:

Astrophysics (astro-ph)

Cite as:

arXiv:astro-ph/0703192v1