Prompt optical observations of GRB050319 with the Swift UVOT

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dc.creatorMason, K. O.
dc.creatorBlustin, A. J.
dc.creatorBoyd, P.
dc.creatorHolland, S. T.
dc.creatorPage, M. J.
dc.creatorRoming, P.
dc.creatorStill, M.
dc.creatorZhang, B.
dc.creatorBreeveld, A.
dc.creatorDe Pasquale, M.
dc.creatorGehrels, N.
dc.creatorGronwall, C.
dc.creatorHunsberger, S.
dc.creatorIvanushkina, M.
dc.creatorLandsman, W.
dc.creatorMcGowan, K.
dc.creatorNousek, J.
dc.creatorPoole, T.
dc.creatorRhoads, J.
dc.creatorRosen, S.
dc.creatorSchady, P.
dc.date2005-11-04
dc.date.accessioned2026-07-07T11:57:17Z
dc.date.available2026-07-07T11:57:17Z
dc.descriptionThe UVOT telescope on the Swift observatory has detected optical afterglow emission from GRB 050319. The flux declines with a power law slope of alpha = -0.57 between the start of observations some 230 seconds after the burst onset (90s after the burst trigger) until it faded below the sensitivity threshold of the instrument after ~5 x 10^4s. There is no evidence for the rapidly declining component in the early light curve that is seen at the same time in the X-ray band. The afterglow is not detected in UVOT shortward of the B-band, suggesting a redshift of about 3.5. The optical V-band emission lies on the extension of the X-ray spectrum, with an optical to X-ray slope of beta = -0.8. The relatively flat decay rate of the burst suggests that the central engine continues to inject energy into the fireball for as long as a few x 10^4s after the burst.
dc.description16 pages, 4 figures, accepted by ApJ
dc.identifierhttps://arxiv.org/abs/astro-ph/0511132
dc.identifierhttp://arxiv.org/abs/astro-ph/0511132
dc.identifierAstrophys.J.639:311-315,2006
dc.identifierdoi:10.1086/499293
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/205828
dc.subjectAstrophysics
dc.titlePrompt optical observations of GRB050319 with the Swift UVOT
dc.typetext

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