2010A&A...521A..53C


C.D.S. - SIMBAD4 rel 1.7 - 2021.03.01CET21:55:18

2010A&A...521A..53C - Astronomy and Astrophysics, volume 521, A53-53 (2010/10-1)

Challenging gamma-ray burst models through the broadband dataset of GRB 060908.

COVINO S., CAMPANA S., CONCIATORE M.L., D'ELIA V., PALAZZI E., THOENE C.C., VERGANI S.D., WIERSEMA K., BRUSASCA M., CUCCHIARA A., COBB B.E., FERNANDEZ-SOTO A., KANN D.A., MALESANI D., TANVIR N.R., ANTONELLI L.A., BREMER M., CASTRO-TIRADO A.J., DE UGARTE POSTIGO A., MOLINARI E., NICASTRO L., STEFANON M., TESTA V., TOSTI G., VITALI F., AMATI L., CHAPMAN R., CONCONI P., CUTISPOTO G., FYNBO J.P.U., GOLDONI P., HENRIKSEN C., HORNE K.D., MALASPINA G., MEURS E.J.A., PIAN E., STELLA L., TAGLIAFERRI G., WARD P. and ZERBI F.M.

Abstract (from CDS):

Multiwavelength observations of gamma-ray burst prompt and afterglow emission are a key tool to separate the various possible emission processes and scenarios proposed to interpret the complex gamma-ray burst phenomenology. We collected a large dataset on GRB060908 in order to carry out a comprehensive analysis of the prompt emission as well as the early and late afterglow. Data from Swift-BAT, -XRT and -UVOT together with data from a number of different ground-based optical/near-infrared and millimeter telescopes allowed us to follow the afterglow evolution after about a minute from the high-energy event down to the host galaxy limit. We discuss the physical parameters required to model these emissions. The prompt emission of GRB060908 was characterised by two main periods of activity, spaced by a few seconds of low intensity, with a tight correlation between activity and spectral hardness. Observations of the afterglow began less than one minute after the high-energy event, when it was already in a decaying phase, and it was characterised by a rather flat optical/near-infrared spectrum which can be interpreted as due to a hard energy-distribution of the emitting electrons. On the other hand, the X-ray spectrum of the afterglow could be fit by a rather soft electron distribution. GRB060908 is a good example of a gamma-ray burst with a rich multi-wavelength set of observations. The availability of this dataset, built thanks to the joint efforts of many different teams, allowed us to carry out stringent tests for various interpretative scenarios, showing that a satisfactorily modelling of this event is challenging. In the future, similar efforts will enable us to obtain optical/near-infrared coverage comparable in quality and quantity to the X-ray data for more events, therefore opening new avenues to progress gamma-ray burst research.

Abstract Copyright:

Journal keyword(s): gamma-ray burst: individual: GRB 060908 - gamma-ray burst: general - radiation mechanisms: non-thermal

Simbad objects: 14

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Number of rows : 14

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 9698 1
2 GRB 060908 gB 02 07 18.360 +00 20 31.20 16.99 18.34 16.85     ~ 177 0
3 GRB 070802 gB 02 27 35.91 -55 31 39.1           ~ 138 0
4 QSO B0235+1624 BLL 02 38 38.93010 +16 36 59.2746   16.46 15.50 15.92   ~ 1412 2
5 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 15197 1
6 GRB 061126 gB 05 46 24.460 +64 12 38.49 18.62 18.79 19.20     ~ 155 1
7 SN 2002lt SN* 08 08 59.858 +06 43 37.52           SNIc: 339 1
8 GRB 090102 gB 08 32 59.50 +33 06 25.7           ~ 187 0
9 GRB 080319B gB 14 31 41.04 +36 18 09.2           ~ 424 0
10 GRB 990123 gB 15 25 29 +44 45.0     8.95     ~ 966 1
11 SA 110- reg 18 45 +00.6           ~ 95 0
12 EM* MWC 349 ** 20 32 45.499080 +40 39 36.74124   15.88 13.15 12.13   Bep 720 0
13 GRB 050820A gB 22 29 38.110 +19 33 37.10 18.33 19.00 18.47     ~ 341 0
14 3C 454.3 Bla 22 53 57.74798 +16 08 53.5611   16.57 16.10 15.22   ~ 2556 2

    Equat.    Gal    SGal    Ecl

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