The origin of the early-time optical emission of Swift GRB 080310★
| Autor: | D. Bersier, Nial R. Tanvir, O. M. Littlejohns, Wenxiong Li, Pierre Christian, Adam N. Morgan, F. Yuan, B. E. Cobb, Stefano Covino, Carole Mundell, P. D Avanzo, Atish Kamble, Alexei V. Filippenko, E. Rol, Daniel A. Perley, Richard Willingale, H. Flewelling, A. de Ugarte Postigo, Carl W. Akerlof, A. J. Castro-Tirado, Robert M. Quimby, Iain A. Steele, Eliana Palazzi, Phil Evans, P. T. O'Brien, Steve Schulze, A. P. Beardmore, K. L. Page, E. A. Hoversten, Shiho Kobayashi, D. Fugazza |
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| Rok vydání: | 2012 |
| Předmět: |
Physics
Spectral index Spectral shape analysis Astrophysics::High Energy Astrophysical Phenomena Phase (waves) Flux Astronomy and Astrophysics Astrophysics::Cosmology and Extragalactic Astrophysics 02 engineering and technology Astrophysics 021001 nanoscience & nanotechnology Light curve 01 natural sciences Redshift Afterglow Space and Planetary Science 0103 physical sciences 0210 nano-technology Gamma-ray burst 010303 astronomy & astrophysics |
| Zdroj: | Monthly Notices of the Royal Astronomical Society. 421:2692-2712 |
| ISSN: | 0035-8711 |
| DOI: | 10.1111/j.1365-2966.2012.20499.x |
| Popis: | We present broadband multi-wavelength observations of GRB 080310 at redshift z = 2.43. This burst was bright and long-lived, and unusual in having extensive optical and near IR follow-up during the prompt phase. Using these data we attempt to simultaneously model the gamma-ray, X-ray, optical and IR emission using a series of prompt pulses and an afterglow component. Initial attempts to extrapolate the high energy model directly to lower energies for each pulse reveal that a spectral break is required between the optical regime and 0.3 keV to avoid over predicting the optical flux. We demonstrate that afterglow emission alone is insufficient to describe all morphology seen in the optical and IR data. Allowing the prompt component to dominate the early-time optical and IR and permitting each pulse to have an independent low energy spectral indices we produce an alternative scenario which better describes the optical light curve. This, however, does not describe the spectral shape of GRB 080310 at early times. The fit statistics for the prompt and afterglow dominated models are nearly identical making it difficult to favour either. However one enduring result is that both models require a low energy spectral index consistent with self absorption for at least some of the pulses identified in the high energy emission model. |
| Databáze: | OpenAIRE |
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