Panchromatic study of GRB 060124: From precursor to afterglow
Panchromatic study of GRB 060124: From precursor to afterglow
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DOI：
10.1393/ncb/i2007-10062-y
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发表时间：
2006-02
影响因子：
6.5
通讯作者：
P. Romano;S. Campana;G. Chincarini;J. Cummings;G. Cusumano;S. T. Holland;V. Mangano;T. Mineo;K. L. Page;V. Pal'shin;E. Rol;T. Sakamoto;Bing Zhang;R. Aptekar';Sebastien Barbier;S. Barthelmy;A. Beardmore;P. T. Boyd;D. Burrows;M. Capalbi;E. Fenimore;D. Frederiks;N. Gehrels;P. Giommi;M. Goad;O. Godet;S. Golenetskii;D. Guetta;J. Kennea;V. Parola;D. Malesani;F. Marshall;A. Moretti;J. Nousek;P. O'Brien;J. Osborne;M. Perri;Gianpiero Tagliaferri
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文献类型：
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作者：
P. Romano;S. Campana;G. Chincarini;J. Cummings;G. Cusumano;S. T. Holland;V. Mangano;T. Mineo;K. L. Page;V. Pal'shin;E. Rol;T. Sakamoto;Bing Zhang;R. Aptekar';Sebastien Barbier;S. Barthelmy;A. Beardmore;P. T. Boyd;D. Burrows;M. Capalbi;E. Fenimore;D. Frederiks;N. Gehrels;P. Giommi;M. Goad;O. Godet;S. Golenetskii;D. Guetta;J. Kennea;V. Parola;D. Malesani;F. Marshall;A. Moretti;J. Nousek;P. O'Brien;J. Osborne;M. Perri;Gianpiero Tagliaferri
我们目前的观察GRB 060124，第一个事件的提示和余辉发射可以同时观察到，并在其全部由三个雨燕仪器。事实上，Swift-BAT在主爆发峰值前570秒的前兆上触发，这使得Swift能够在主爆发发生前350秒将窄场仪器重新指向爆发位置。GRB 060124也触发了Konus-Wind，它观测到了更硬的伽马射线带（高达2 MeV）的瞬发辐射。由于这些特殊的情况下，即时发射的时间和光谱特性可以在光学，X射线和伽马射线范围内进行研究。虽然X射线发射（0.2-10千电子伏）清楚地跟踪伽马射线爆发，光学组件遵循一个di！这是一种模式，很可能表明一个差异！可能是外部冲击的开始。瞬发γ射线暴谱具有明显的谱演化，峰值能量和谱指数都发生了变化。正如在几个长伽玛暴中所观察到的那样，在硬能和低能成分之间测量到了显着的滞后，表明这种行为在能量上延续了30多年。在软能量下，伽玛射线暴的峰值也要宽得多。这与光谱的时间演化有关，并且可以通过假设电子光谱指数随时间软化来解释。GRB 060124的爆发能量（Eiso ~（-5）1053 erg）和平均峰值能量（Ep ~（-300）keV）符合Amati关系。X射线余辉的特征是衰减，在tb ~（10）5s处出现一个突变。
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 di! erent pattern, likely indicating a di! erent 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 # 10 53 erg) and average peak energy (Ep " 300 keV) make GRB060124 consistent with theAmati relation. TheX-ray afterglow ischaracterized by adecay which presents a break at tb " 10 5 s.