The nature of the X-Ray Flash of August 24 2005

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dc.creatorSollerman, J.
dc.creatorFynbo, J. P. U.
dc.creatorGorosabel, J.
dc.creatorHalpern, J. P.
dc.creatorHjorth, J.
dc.creatorJakobsson, P.
dc.creatorMirabal, N.
dc.creatorWatson, D.
dc.creatorXu, D.
dc.creatorCastro-Tirado, A. J.
dc.creatorFeron, C.
dc.creatorJaunsen, A. O.
dc.creatorJelinek, M.
dc.creatorJensen, B. L.
dc.creatorKann, D. A.
dc.creatorOvaldsen, J. E.
dc.creatorPozanenko, A.
dc.creatorStritzinger, M.
dc.creatorThoene, C. C.
dc.creatorPostigo, A. de Ugarte
dc.creatorGuziy, S.
dc.creatorIbrahimov, M.
dc.creatorJaervinen, S. P.
dc.creatorLevan, A.
dc.creatorRumyantsev, V.
dc.creatorTanvir, N.
dc.date2007-01-25
dc.date.accessioned2026-07-07T10:21:37Z
dc.date.available2026-07-07T10:21:37Z
dc.descriptionWe 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)
dc.descriptionAccepted for publication in Astronomy & Astrophysics
dc.identifierhttps://arxiv.org/abs/astro-ph/0701736
dc.identifierhttp://arxiv.org/abs/astro-ph/0701736
dc.identifierAstron.Astrophys.466:839-846,2006
dc.identifierdoi:10.1051/0004-6361:20066683
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/175235
dc.subjectAstrophysics
dc.titleThe nature of the X-Ray Flash of August 24 2005
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