2009MNRAS.400..134P

Query : 2009MNRAS.400..134P

2009MNRAS.400..134P - Mon. Not. R. Astron. Soc., 400, 134-146 (2009/November-3)

Multiwavelength observations of the energetic GRB 080810: detailed mapping of the broad-band spectral evolution.

PAGE K.L., WILLINGALE R., BISSALDI E., DE UGARTE POSTIGO A., HOLLAND S.T., McBREEN S., O'BRIEN P.T., OSBORNE J.P., PROCHASKA J.X., ROL E., RYKOFF E.S., STARLING R.L.C., TANVIR N.R., VAN DER HORST A.J., WIERSEMA K., ZHANG B., ACEITUNO F.J., AKERLOF C., BEARDMORE A.P., BRIGGS M.S., BURROWS D.N., CASTRO-TIRADO A.J., CONNAUGHTON V., EVANS P.A., FYNBO J.P.U., GEHRELS N., GUIDORZI C., HOWARD A.W., KENNEA J.A., KOUVELIOTOU C., PAGANI C., PREECE R., PERLEY D., STEELE I.A. and YUAN F.

Abstract (from CDS):

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 Robotic Optical Transient Search Experiment (ROTSE) and a host of other telescopes, and was detected in the radio by the Very Large Array. The redshift of z = 3.355±0.005 was determined by Keck/High Resolution Echelle Spectrometer (HIRES) and confirmed by RTT150 and NOT. The prompt gamma/X-ray emission, detected over 0.3-103 keV, systematically softens over time, with Epeak moving from ∼600 keV at the start to ∼40 keV around 100s after the trigger; alternatively, this spectral evolution could be identified with the blackbody temperature of a quasi-thermal model shifting from ∼60 to ∼3keV over the same time interval. The first optical detection was made at 38s, but the smooth, featureless profile of the full optical coverage implies that this is originated from the afterglow component, not from the pulsed/flaring prompt emission.

Broad-band optical and X-ray coverage of the afterglow at the start of the final X-ray decay (∼8ks) reveals a spectral break between the optical and X-ray bands in the range of 1015-2 x1016Hz. 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 ∼3x105s. GRB 080810 was very energetic, with an isotropic energy output for the prompt component of 3x1053 and 1.6x1052 erg for the afterglow; there is no evidence for a jet break in the afterglow up to 6d following the burst.


Abstract Copyright: © 2009 The Authors. Journal compilation © 2009 RAS

Journal keyword(s): gamma-rays: bursts - X-rays: individual: GRB 080810

CDS comments: In chap 3.3.3 : GRB 070710A is a misprint for GRB 071010A

Simbad objects: 12

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Number of rows : 12
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 GRB 021004 gB 00 26 54.68 +18 55 41.6           ~ 560 0
2 GRB 070616 gB 02 08 36.430 +56 56 44.91           ~ 79 0
3 GRB 061007 gB 03 05 19.510 -50 30 02.50 14.28 14.40 12.95     ~ 315 1
4 GRB 060124 gB 05 08 25.900 +69 44 26.98   18.91 17.35     ~ 280 0
5 GRB 070311 gB 05 50 08.220 +03 22 29.40           ~ 68 0
6 GRB 050502B gB 09 30 10.024 +16 59 48.07           ~ 169 0
7 GRB 061121 gB 09 48 54.570 -13 11 42.68 17.19 17.71 17.02     ~ 350 0
8 UGCS J162444.39-273226.8 G 16 24 44.38275 -27 32 26.8381     19.70     ~ 469 1
9 GRB 071010A gB 19 12 14.42 -32 24 06.2           ~ 138 0
10 GRB 020813A gB 19 46 41.874 -19 36 04.81           ~ 316 0
11 GRB 060607 gB 21 58 50.400 -22 29 46.70 18.49 16.67 15.09     ~ 318 0
12 Fermi bn080810549 gB 23 47 08.00 +00 18 35.1           ~ 240 0

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