Please use this identifier to cite or link to this item: http://hdl.handle.net/2381/39067
Title: Panchromatic study of GRB 060124: From precursor to afterglow
Authors: Romano, P.
Campana, S.
Chincarini, G.
Cummings, J.
Cusumano, G.
Holland, S. T.
Mangano, V.
Mineo, T.
Page, K. L.
PaL'Shin, V.
Rol, E.
Sakamoto, T.
Zhang, B.
Aptekar, R.
Barbier, S.
Barthelmy, S.
Beardmore, A. P.
Boyd, P.
Burrows, D. N.
Capalbi, M.
Fenimore, E. E.
Boyd, P.
Frederiks, D.
Gehrels, N.
Giommi, P.
Goad, M. R.
Godet, O.
Golenetskii, S.
Guetta, D.
Kennea, J. A.
La Parola, V.
Malesani, D.
Marshall, F.
Moretti, A.
Nousek, J. A.
O'Brien, P. T.
Osborne, J. P.
Perri, M.
Tagliaferri, G.
First Published: 18-Apr-2007
Presented at: Workshop on Swift and GRBs - Unveiling the Relativistic University, Venice, ITALY
Start Date: 5-Jun-2006
End Date: 9-Jun-2006
Publisher: Società Italiana di Fisica, Springer Verlag (Germany)
Citation: Nuovo Cimento B, 2006, 121 (10-11), pp. 1067-1071 (5)
Abstract: We present observations of GRB 060124, the first event for which both the prompt and the afterglow emission could be observed simultaneously and in their entirety by the three Swift instruments and by Konus-Wind. Thanks to these exceptional circumstances, the temporal and spectral properties of the prompt emission could be studied in the optical, X-ray and gamma-ray ranges (up to 2 MeV). While the X-ray emission (0.2–10 keV) clearly tracks the gamma-ray burst, the optical component follows a different pattern, likely indicating a different origin, possibly the onset of external shocks. The prompt GRB spectrum shows significant spectral evolution, with both the peak energy and the spectral index varying. As observed in several long GRBs, significant lags are measured between the hard- and lowenergy components, showing that this behaviour extends over 3 decades in energy. The GRB peaks are also much broader at soft energies. This is related to the temporal evolution of the spectrum, and can be accounted for by the softening of the electron spectral index with time. The burst energy (Eiso ∼ 5 × 1053 erg at z = 2.297) and average peak energy (Ep ∼ 300 keV) make GRB 060124 consistent with the Amati relation. The X-ray afterglow is characterized by a decay which presents a break at tb ∼ 105 s.
DOI Link: 10.1393/ncb/i2007-10062-y
ISSN: 1594-9982
Links: http://www.sif.it/riviste/ncb/econtents/2006/121/10-11/article/49
http://hdl.handle.net/2381/39067
Version: Post-print
Status: Peer-reviewed
Type: Conference Paper
Rights: Creative Commons “Attribution Non-Commercial No Derivatives” licence CC BY-NC-ND, further details of which can be found via the following link: http://creativecommons.org/licenses/by-nc-nd/4.0/ Archived with reference to SHERPA/RoMEO and publisher website.
Appears in Collections:Conference Papers & Presentations, Dept. of Physics and Astronomy

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