Challenging GRB models through the broadband dataset of GRB060908

• Published in: Astronomy and astrophysics (Berlin) 2010-10, Vol.521
• Main Authors: Covino, S., Campana, S., Conciatore, M.L., d'Elia, V., Palazzi, E., Thöne, 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., Zerbi, F.M.
• Format: Article
• Language: English
• Subjects: Astrophysics; High Energy Astrophysical Phenomena; Physics; Sciences of the Universe
• ISSN: 0004-6361; 1432-0756
• DOI: 10.1051/0004-6361/201014994

Context: Multiwavelength observations of gamma-ray burst prompt and afterglow emission are a key tool to disentangle the various possible emission processes and scenarios proposed to interpret the complex gamma-ray burst phenomenology. Aims: 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. Methods: Data from Swift-BAT, -XRT and -UVOT together with data from a number of different ground-based optical/NIR and millimeter telescopes allowed us to follow the afterglow evolution from about a minute from the high-energy event down to the host galaxy limit. We discuss the physical parameters required to model these emissions. Results: The prompt emission of GRB060908 was characterized 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 characterized by a rather flat optical/NIR 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. Conclusions: 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 modeling of this event is challenging. In the future, similar efforts will enable us to obtain optical/NIR coverage comparable in quality and quantity to the X-ray data for more events, therefore opening new avenues to progress gamma-ray burst research.