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27 April 2024 |
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The 999th Swift Gamma-Ray Burst: some like it thermal | | F. Nappo
; A. Pescalli
; G. Oganesyan
; G. Ghirlanda
; M. Giroletti
; A. Melandri
; S. Campana
; G. Ghisellini
; O.S. Salafia
; P. D'Avanzo
; M.G. Bernardini
; S. Covino
; E. Carretti
; A. Celotti
; V. D'Elia
; L. Nava
; E. Palazzi
; S. Poppi
; I. Prandoni
; S. Righini
; A. Rossi
; R. Salvaterra
; G. Tagliaferri
; V. Testa
; T. Venturi
; S.D. Vergani
; | | Date: |
27 Apr 2016 | | Abstract: | We present a multiwavelength study of GRB 151027A. This is the 999th GRB
detected by the Swift satellite and it has a densely sampled emission in the
X-ray and optical band and has been observed and detected in the radio up to
140 days after the prompt. The multiwavelength light curve from 500 s to 140
days can be modelled through a standard forward shock afterglow but requires an
additional component to reproduce the early X-ray and optical emission. We
present TNG and LBT optical observations performed 19.6, 33.9 and 92.3 days
after the trigger which show a bump with respect to a standard afterglow flux
decay and are possibly interpreted as due to the underlying SN and host galaxy
(of 0.4 uJy in the R band). Radio observations, performed with SRT, Medicina,
EVN and VLBA between day 4 and 140, suggest that the burst exploded in an
environment characterised by a density profile scaling with the distance from
the source (wind profile). A remarkable feature of the prompt emission is the
presence of a bright flare 100 s after the trigger, lasting 70 seconds in the
soft X-ray band, which was simultaneously detected from the optical band up to
the MeV energy range. By combining Swift-BAT/XRT and Fermi-GBM data, the
broadband (0.3-1000 keV) time resolved spectral analysis of the flare reveals
the coexistence of a non-thermal (power law) and thermal blackbody components.
The BB component contributes up to 35% of the luminosity in the 0.3-1000 keV
band. The gamma-ray emission observed in Swift-BAT and Fermi-GBM anticipates
and lasts less than the soft X-ray emission as observed by Swift-XRT, arguing
against a Comptonization origin. The BB component could either be produced by
an outflow becoming transparent or by the collision of a fast shell with a
slow, heavy and optically thick fireball ejected during the quiescent time
interval between the initial and later flares of the burst. | | Source: | arXiv, 1604.8204 | | Services: | Forum | Review | PDF | Favorites | |
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