|
| | | | |
| | | |
| Stat |
Members: 3665
Articles: 2'599'751
Articles rated: 2609
25 January 2025 |
|
| | | | |
|
Article overview
| |
|
|
The nature of the X-Ray Flash of August 24 2005 | | J. Sollerman
; J. P. U. Fynbo
; J. Gorosabel
; J. P. Halpern
; J. Hjorth
; P. Jakobsson
; N. Mirabal
; D. Watson
; D. Xu
; A. J. Castro-Tirado
; C. Feron
; A. O. Jaunsen
; M. Jelinek
; B. L. Jensen
; D. A. Kann
; J.E. Ovaldsen
; A. Pozanenko
; M. Stritzinger
; C. C. Thoene
; A. de Ugarte Postigo
; S. Guziy
; M. Ibrahimov
; S. P. Jaervinen
; A. Levan
; V. Rumyantsev
; N. Tanvir
; | | Date: |
25 Jan 2007 | | Abstract: | We present comprehensive photometric R-band observations of the fading optical afterglow of the X-Ray Flash XRF050824, from 11 minutes to 104 days after the burst. The R-band lightcurve of the afterglow resembles the lightcurves of long duration Gamma-Ray Bursts (GRBs), i.e., a power-law albeit with a rather shallow slope of alpha=0.6. Our late R-band images reveal the host galaxy with a rest-frame B-band luminosity corresponding to roughly 0.5 Lstar. The star-formation rate as determined from the [O II] emission line luminosity is about 1.8 Msun per year. When accounting for the host contribution, the slope is alpha=0.65+-0.01 and a break in the lightcurve is also suggested. A potential lightcurve bump at 2 weeks can be interpreted as a supernova only if this is a supernova with a fast rise and a fast decay. However, the overall fit still show excess scatter in the lightcurve due to wiggles and bumps. The flat lightcurves in the optical and X-rays could be explained by a continuous energy injection scenario with an on-axis viewing angle and a wide jet opening angle (theta_j>10 deg). If the energy injections are episodic, this could potentially help explain the bumps and wiggles. Spectroscopy of the afterglow give a redshift of z=0.828+-0.005 from both absorption and emission lines. The spectral energy distribution (SED) of the afterglow has a power-law shape with slope beta=0.56+-0.04. This can be compared to the X-ray spectral index which is betaX=1.0+-0.1. The curvature of the SED constrain the dust reddening towards the burst to Av<0.5 mag. (abridged) | | Source: | arXiv, astro-ph/0701736 | | Services: | Forum | Review | PDF | Favorites | |
|
|
No review found.
Did you like this article?
Note: answers to reviews or questions about the article must be posted in the forum section.
Authors are not allowed to review their own article. They can use the forum section.
|
| |
|
|
|
REGISTER