Multi-wavelength observations of the energetic GRB 080810: detailed mapping of the broadband spectral evolution

Details Multi-wavelength observations of the energetic GRB 080810: detailed mapping of the broadband spectral evolution Multi-wavelength observations of the energetic GRB 080810: detailed mapping of the broadband spectral evolution

2009-07-27

arxiv.org/abs/0907.4578v1

Mon.Not.Roy.Astron.Soc. 400:134-146,2009

Astronomy and Astrophysics

Astrophysics

High Energy Astrophysical Phenomena

15 pages, 9 figures, 4 in colour. Accepted for publication in MNRAS

Scientific paper

10.1111/j.1365-2966.2009.15462.x

GRB 080810 was one of the first bursts to trigger both Swift and the Fermi Gamma-ray Space Telescope. It was subsequently monitored over the X-ray and UV/optical bands by Swift, in the optical by ROTSE and a host of other telescopes and was detected in the radio by the VLA. The redshift of z= 3.355 +/- 0.005 was determined by Keck/HIRES and confirmed by RTT150 and NOT. The prompt gamma/X-ray emission, detected over 0.3-10^3 keV, systematically softens over time, with E_peak moving from ~600 keV at the start to ~40 keV around 100 s after the trigger; alternatively, this spectral evolution could be identified with the blackbody temperature of a quasithermal model shifting from ~60 keV to ~3 keV over the same time interval. The first optical detection was made at 38 s, but the smooth, featureless profile of the full optical coverage implies that this originated from the afterglow component, not the pulsed/flaring prompt emission. Broadband optical and X-ray coverage of the afterglow at the start of the final X-ray decay (~8 ks) reveals a spectral break between the optical and X-ray bands in the range 10^15 - 2x10^16 Hz. The decay profiles of the X-ray and optical bands show that this break initially migrates blueward to this frequency and then subsequently drifts redward to below the optical band by ~3x10^5 s. GRB 080810 was very energetic, with an isotropic energy output for the prompt component of 3x10^53 erg and 1.6x10^52 erg for the afterglow; there is no evidence for a jet break in the afterglow up to six days following the burst.

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