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Author Ryde, F. ♦ Axelsson, M. ♦ Zhang, B. B. ♦ McGlynn, S. ♦ Pe'er, A. ♦ Lundman, C. ♦ Larsson, S. ♦ Battelino, M. ♦ Zhang, B. ♦ Bissaldi, E. ♦ Bregeon, J. ♦ Briggs, M. S. ♦ Chiang, J. ♦ de Palma, F. ♦ Guiriec, S. ♦ Larsson, J. ♦ Longo, F. ♦ McBreen, S. ♦ Omodei, N. ♦ Petrosian, V. ♦ Preece, R. ♦ van der Horst, A. J.
Source arXiv.org
Content type Text
File Format PDF
Date of Submission 2009-11-11
Language English
Subject Domain (in DDC) Computer science, information & general works ♦ Natural sciences & mathematics ♦ Astronomy & allied sciences ♦ Physics
Subject Keyword Astrophysics - High Energy Astrophysical Phenomena ♦ Astrophysics - Cosmology and Nongalactic Astrophysics ♦ physics:astro-ph
Abstract The Fermi Gamma-ray Space Telescope observed the bright and long GRB090902B, lying at a redshift of z = 1.822. Together the Large Area Telescope (LAT) and the Gamma-ray Burst Monitor (GBM) cover the spectral range from 8 keV to >300 GeV is covered. Here we show that the prompt burst spectrum is consistent with emission from the jet photosphere combined with non-thermal emission described by a single power-law with photon index -1.9. The photosphere gives rise to a strong quasi-blackbody spectrum which is somewhat broader than a single Planck function and has a characteristic temperature of ~290keV. We derive the photospheric radius Rph = (1.1 \pm 0.3) x 10^12 Y^{1/4} cm and the bulk Lorentz factor of the flow, which is found to vary by a factor of two and has a maximal value of Gamma = 750 Y^{1/4}. Here Y is the ratio between the total fireball energy and the energy emitted in the gamma-rays. We find that during the first quarter of the prompt phase the photospheric emission dominates, which explains the delayed onset of the observed flux in the LAT compared to the GBM. We model the photospheric emission with a multi-color blackbody and its shape indicates that the photospheric radius increases at higher latitudes. We interpret the broad band emission as synchrotron emission at R ~ 4x10^15 cm. Our analysis emphasize the importance of having high temporal resolution when performing spectral analysis on GRBs, since there is strong spectral evolution.
Description Comment: Accepted by ApJ Letters
Educational Use Research
Learning Resource Type Article


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