dc.contributor.author | Page, M. J. | |
dc.contributor.author | Boyd, P. | |
dc.contributor.author | Cucchiara, A. | |
dc.contributor.author | Gehrels, N. | |
dc.contributor.author | Gronwall, C. | |
dc.contributor.author | DE PASQUALE, Massımılıano | |
dc.contributor.author | Holland, S. T. | |
dc.contributor.author | Marshall, F. E. | |
dc.contributor.author | McGowan, K. E. | |
dc.contributor.author | Nousek, J. A. | |
dc.contributor.author | Schady, P. | |
dc.contributor.author | Mason, K. O. | |
dc.contributor.author | Osborne, J. P. | |
dc.contributor.author | Roming, P. W. A. | |
dc.contributor.author | Still, M. | |
dc.contributor.author | Zhang, B. | |
dc.contributor.author | Blustin, A. J. | |
dc.date.accessioned | 2022-02-18T09:00:47Z | |
dc.date.available | 2022-02-18T09:00:47Z | |
dc.date.issued | 2006 | |
dc.identifier.citation | Schady P., Mason K. O. , Osborne J. P. , Page M. J. , Roming P. W. A. , Still M., Zhang B., Blustin A. J. , Boyd P., Cucchiara A., et al., "Swift UVOT observations of X-ray flash 050406", ASTROPHYSICAL JOURNAL, cilt.643, sa.1, ss.276-283, 2006 | |
dc.identifier.issn | 0004-637X | |
dc.identifier.other | av_108abc6b-9f41-4376-9129-6b62705f8f14 | |
dc.identifier.other | vv_1032021 | |
dc.identifier.uri | http://hdl.handle.net/20.500.12627/176318 | |
dc.identifier.uri | https://doi.org/10.1086/501449 | |
dc.description.abstract | We present Swift UVOT data on the optical afterglow of the X-ray flash of 2005 April 6 ( XRF 050406) from 88 to similar to 10(5) s after the initial prompt gamma-ray emission. Our observations in the V, B, and U bands are the earliest that have been taken of an XRF optical counterpart. Combining the early-time optical temporal and spectral properties with gamma-ray and simultaneous X-ray data taken with the BAT and XRT telescopes on board Swift, we are able to constrain possible origins of the XRF. The prompt emission had a FRED ( fast-rise, exponential decay) profile with a duration of T-90 = 5.7 +/- 0.2 s, putting it at the short end of the long-burst duration distribution. The absence of photoelectric absorption redward of 4000 (A) over circle in the UV/optical spectrum provides a firm upper limit of z <= 3.1 on the redshift, thus excluding a high redshift as the sole reason for the soft spectrum. The optical light curve is consistent with a power-law decay with slope alpha = 0.75 +/- 0.26( F-v proportional to t(alpha)) and a maximum occurring in the first 200 s after the initial gamma-ray emission. The softness of the prompt emission is well described by an off-axis structured jet model, which is able to account for the early peak flux and shallow decay observed in the optical and X- ray bands. | |
dc.language.iso | eng | |
dc.subject | Astronomy and Astrophysics | |
dc.subject | ASTRONOMİ VE ASTROFİZİK | |
dc.subject | Uzay bilimi | |
dc.subject | Temel Bilimler (SCI) | |
dc.subject | Fizik | |
dc.subject | Astronomi ve Astrofizik | |
dc.subject | Temel Bilimler | |
dc.subject | Physics and Astronomy (miscellaneous) | |
dc.subject | General Physics and Astronomy | |
dc.subject | Space and Planetary Science | |
dc.subject | Physical Sciences | |
dc.title | Swift UVOT observations of X-ray flash 050406 | |
dc.type | Makale | |
dc.relation.journal | ASTROPHYSICAL JOURNAL | |
dc.contributor.department | , , | |
dc.identifier.volume | 643 | |
dc.identifier.issue | 1 | |
dc.identifier.startpage | 276 | |
dc.identifier.endpage | 283 | |
dc.contributor.firstauthorID | 3373904 | |