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The extraordinarily bright optical afterglow of GRB 991208 and its host galaxy | | A. J. Castro-Tirado
; V. V. Sokolov
; J. Gorosabel
; J. M. Castro Cerón
; J. Greiner
; R.A.M.J. Wijers
; B.L. Jensen
; J. Hjorth
; S. Toft
; H. Pedersen
; E. Palazzi
; E. Pian
; N. Masetti
; R. Sagar
; V. Mohan
; A.K. Pandey
; S.B. Pandey
; S.N. Dodonov
; T.A. Fatkhullin
; V.L. Afanasiev
; V.N. Komarova
; A.V. Moiseev
; R. Hudec
; V. Simon
; P. Vreeswijk
; E. Rol
; S. Klose
; B. Stecklum
; M.R. Zapatero-Osorio
; N. Caon
; C. Blake
; J. Wall
; D. Heinlein
; A. Henden
; S. Benetti
; A. Magazzu
; F. Ghinassi
; L. Tommasi
; M. Bremer
; C. Kouveliotou
; S. Guziy
; A. Shlyapnikov
; U. Hopp
; G. Feulner
; S. Dreizler
; D. Hartmann
; H. Boehnhardt
; J.M. Paredes
; J. Marti
; E. Xanthopoulos
; H.E. Kristen
; J. Smoker
; H. Hurley
; | | Date: |
9 Feb 2001 | | Journal: | Astron.Astrophys. 370 (2001) 398-406 DOI: 10.1051/0004-6361:20010247 | | Subject: | astro-ph | | Abstract: | Observations of the extraordinarily bright optical afterglow (OA) of GRB 991208 started 2.1 d after the event. The flux decay constant of the OA in the R-band is -2.30 +/- 0.07 up to 5 d, which is very likely due to the jet effect, and after that it is followed by a much steeper decay with constant -3.2 +/- 0.2, the fastest one ever seen in a GRB OA. A negative detection in several all-sky films taken simultaneously to the event implies either a previous additional break prior to 2 d after the occurrence of the GRB (as expected from the jet effect). The existence of a second break might indicate a steepening in the electron spectrum or the superposition of two events. Once the afterglow emission vanished, contribution of a bright underlying SN is found, but the light curve is not sufficiently well sampled to rule out a dust echo explanation. Our determination of z = 0.706 indicates that GRB 991208 is at 3.7 Gpc, implying an isotropic energy release of 1.15 x 10E53 erg which may be relaxed by beaming by a factor > 100. Precise astrometry indicates that the GRB coincides within 0.2" with the host galaxy, thus given support to a massive star origin. The absolute magnitude is M_B = -18.2, well below the knee of the galaxy luminosity function and we derive a star-forming rate of 11.5 +/- 7.1 Mo/yr. The quasi-simultaneous broad-band photometric spectral energy distribution of the afterglow is determined 3.5 day after the burst (Dec 12.0) implying a cooling frequency below the optical band, i.e. supporting a jet model with p = -2.30 as the index of the power-law electron distribution. | | Source: | arXiv, astro-ph/0102177 | | Services: | Forum | Review | PDF | Favorites | |
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