dc.contributor.author | Melandri, A. | |
dc.contributor.author | Mundell, C.G. | |
dc.contributor.author | Kobayashi, S. | |
dc.contributor.author | Guidorzi, C. | |
dc.contributor.author | Gomboc, A. | |
dc.contributor.author | Steele, I.A. | |
dc.contributor.author | Smith, R.J. | |
dc.contributor.author | Bersier, D. | |
dc.contributor.author | Mottram, C.J. | |
dc.contributor.author | Carter, D. | |
dc.contributor.author | Bode, M.F. | |
dc.contributor.author | O'Brien, P.T. | |
dc.contributor.author | Tanvir, N. | |
dc.contributor.author | Rol, E. | |
dc.contributor.author | Chapman, R. | |
dc.date.accessioned | 2009-01-08T10:40:46Z | |
dc.date.available | 2009-01-08T10:40:46Z | |
dc.date.issued | 2008 | |
dc.identifier.citation | Melandri , A , Mundell , C G , Kobayashi , S , Guidorzi , C , Gomboc , A , Steele , I A , Smith , R J , Bersier , D , Mottram , C J , Carter , D , Bode , M F , O'Brien , P T , Tanvir , N , Rol , E & Chapman , R 2008 , ' The Early-Time Optical Properties of Gamma-Ray Burst Afterglows ' , The Astrophysical Journal , vol. 686 , pp. 1209-1230 . https://doi.org/10.1086/591243 | |
dc.identifier.issn | 1538-4357 | |
dc.identifier.other | PURE: 154070 | |
dc.identifier.other | PURE UUID: d7d792f9-4059-4551-b041-573deb94c68b | |
dc.identifier.other | dspace: 2299/2771 | |
dc.identifier.other | Scopus: 54249160086 | |
dc.identifier.uri | http://hdl.handle.net/2299/2771 | |
dc.description | Original article can be found at: http://www.iop.org/EJ/journal/apj Copyright American Astronomical Society DOI: 10.1086/591243 [Full text of this article is not available in the UHRA] | |
dc.description.abstract | We present a multiwavelength analysis of 63 gamma-ray bursts observed with the world's three largest robotic optical telescopes, the Liverpool and Faulkes Telescopes (North and South). Optical emission was detected for 24 GRBs with brightnesses ranging from R = 10 to 22 mag in the first 10 minutes after the burst. By comparing optical and X-ray light curves from t = 100 to ~106 seconds, we introduce four main classes, defined by the presence or absence of temporal breaks at optical and/or X-ray wavelengths. While 14/24 GRBs can be modeled with the forward-shock model, explaining the remaining 10 is very challenging in the standard framework even with the introduction of energy injection or an ambient density gradient. Early X-ray afterglows, even segments of light curves described by a power law, may be due to additional emission from the central engine. Thirty-nine GRBs in our sample were not detected and have deep upper limits (R < 22 mag) at early time. Of these, only 10 were identified by other facilities, primarily at near infrared wavelengths, resulting in a dark burst fraction of ~50%. Additional emission in the early-time X-ray afterglow due to late-time central engine activity may also explain some dark bursts by making the bursts brighter than expected in the X-ray band compared to the optical band. | en |
dc.language.iso | eng | |
dc.relation.ispartof | The Astrophysical Journal | |
dc.title | The Early-Time Optical Properties of Gamma-Ray Burst Afterglows | en |
dc.contributor.institution | School of Physics, Astronomy and Mathematics | |
dc.description.status | Peer reviewed | |
rioxxterms.versionofrecord | https://doi.org/10.1086/591243 | |
rioxxterms.type | Journal Article/Review | |
herts.preservation.rarelyaccessed | true | |