Multi-Wavelength Studies of the Optically Dark Gamma-Ray Burst 001025A

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dc.creatorPedersen, K.
dc.creatorHurley, K.
dc.creatorHjorth, J.
dc.creatorSmith, D. A.
dc.creatorAndersen, M. I.
dc.creatorChristensen, L.
dc.creatorCline, T.
dc.creatorFynbo, J. P. U.
dc.creatorGoldsten, J.
dc.creatorGolenetskii, S.
dc.creatorGorosabel, J.
dc.creatorJakobsson, P.
dc.creatorJensen, B. L.
dc.creatorMilvang-Jensen, B.
dc.creatorMcClanahan, T.
dc.creatorMoller, P.
dc.creatorPalshin, V.
dc.creatorSchartel, N.
dc.creatorTrombka, J.
dc.creatorUlanov, M.
dc.creatorWatson, D.
dc.date2005-09-15
dc.date.accessioned2026-07-07T06:24:23Z
dc.date.available2026-07-07T06:24:23Z
dc.descriptionWe identify the fading X-ray afterglow of GRB 001025A from XMM-Newton observations obtained 1.9-2.3 days, 2 years, and 2.5 years after the burst. The non-detection of an optical counterpart to an upper limit of R=25.5, 1.20 days after the burst, makes GRB 001025A a ``dark'' burst. Based on the X-ray afterglow spectral properties of GRB 001025A, we argue that some bursts appear optically dark because their afterglow is faint and their cooling frequency is close to the X-ray band. This interpretation is applicable to several of the few other dark bursts where the X-ray spectral index has been measured. The X-ray afterglow flux of GRB 001025A is an order of magnitude lower than for typical long-duration gamma-ray bursts. The spectrum of the X-ray afterglow can be fitted with an absorbed synchrotron emission model, an absorbed thermal plasma model, or a combination thereof. For the latter, an extrapolation to optical wavelengths can be reconciled with the R-band upper limit on the afterglow, without invoking any optical circumburst absorption, provided the cooling frequency is close to the X-ray band. Alternatively, if the X-ray afterglow is due to synchrotron emission only, seven magnitudes of extinction in the observed R-band is required to meet the R-band upper limit, making GRB 001025A much more obscured than bursts with detected optical afterglows. Based on the column density of X-ray absorbing circumburst matter, an SMC gas-to-dust ratio is insufficient to produce this amount of extinction. The X-ray tail of the prompt emission enters a steep temporal decay excluding that the tail of the prompt emission is the onset of the afterglow (abridged).
dc.description32 pages, 8 figures, ApJ in press
dc.identifierhttps://arxiv.org/abs/astro-ph/0509424
dc.identifierhttp://arxiv.org/abs/astro-ph/0509424
dc.identifierAstrophys.J. 636 (2006) 381-390
dc.identifierdoi:10.1086/497948
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/96523
dc.subjectAstrophysics
dc.titleMulti-Wavelength Studies of the Optically Dark Gamma-Ray Burst 001025A
dc.typetext

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