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|Title: ||Panchromatic study of GRB 060124: from precursor to afterglow|
|Authors: ||Romano, Patrizia|
Page, Kim L.
Barthelmy, Scott D.
Beardmore, Andrew P.
Burrows, David N.
Goad, Michael R.
Kennea, Jamie A.
La Parola, V.
Nousek, John A.
O'Brien, Paul T.
Osborne, Julian P.
|Issue Date: ||2006|
|Publisher: ||EDP Sciences|
|Citation: ||Astronomy and Astrophysics, 2006, 456, pp.917-927.|
|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. Indeed, Swift-BAT triggered on a precursor ~570 s before the
main burst peak, and this allowed Swift to repoint the narrow field instruments to the burst position ~350 s before the main burst
occurred. GRB 060124 also triggered Konus-Wind, which observed the prompt emission in a harder gamma-ray band (up to 2 MeV).
Thanks to these exceptional circumstances, the temporal and spectral properties of the prompt emission can be studied in the optical, X-ray and gamma-ray ranges. 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 low-energy 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 assuming that the electron spectral index softened with time. The burst energy (Eiso ~ 5 × 1053 erg) and average peak energy (Ep ~ 300 keV) make GRB060124 consistent with the Amati relation. The X-ray afterglow is characterized by a decay which presents a break at tb ~ 105 s.|
|DOI Link: ||10.1051/0004-6361:20065071|
|Version: ||Publisher PDF|
|Rights: ||© The European Southern Observatory (ESO) 2006. Deposited with permission of the publisher.|
|Appears in Collections:||Published Articles, Dept. of Physics and Astronomy|
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