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|Title:||Swift and optical observations of GRB 050401|
|Authors:||De Pasquale M.|
Mason, K. O.
Rosen, S. R.
Beardmore, A. P.
Page, K. L.
Wells, A. A.
Barthelmy, S. D.
Burrows, D. N.
Nousek, J. A.
Peterson, B. A.
Schmidt, B. P.
Palmer, D. M.
Price, P. A.
|Publisher:||Royal Astronomical Society (RAS)|
|Citation:||Monthly Notices of the Royal Astronomical Society, 2006, 365 (3), pp. 1031-1038|
|Abstract:||We present the results of the analysis of γ-ray and X-ray data of GRB 050401 taken with the Swift satellite, together with a series of ground-based follow-up optical observations. The Swift X-ray light curve shows a clear break at about 4900 s after the γ-ray burst (GRB). The decay indices before and after the break are consistent with a scenario of continuous injection of radiation from the ‘central engine’ of the GRB to the fireball. Alternatively, this behaviour could result if ejecta are released with a range of Lorentz factors, with the slower shells catching up the faster at the afterglow shock position. The two scenarios are observationally indistinguishable. The GRB 050401 afterglow is quite bright in the X-ray band, but weak in the optical, with an optical to X-ray flux ratio similar to those of ‘dark bursts’. We detect a significant amount of absorption in the X-ray spectrum, with NH= (1.7 ± 0.2) × 1022cm−2 at a redshift of z= 2.9, which is typical of a dense circumburst medium. Such high column density implies an unrealistic optical extinction of 30 mag if we adopt a Galactic extinction law, which would not be consistent with the optical detection of the afterglow. This suggests that the extinction law is different from the Galactic one.|
|Rights:||This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2005 the authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. Deposited with reference to the publisher’s archiving policy available on the SHERPA/RoMEO website.|
|Appears in Collections:||Published Articles, Dept. of Physics and Astronomy|
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