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SYNCHROTRON SELF-INVERSE COMPTON RADIATION FROM REVERSE SHOCK ON GRB 120326A
Urata, Yuji,Huang, Kuiyun,Takahashi, Satoko,Im, Myungshin,Yamaoka, Kazutaka,Tashiro, Makoto,Kim, Jae-Woo,Jang, Minsung,Pak, Soojong IOP Publishing 2014 The Astrophysical journal Vol.789 No.2
<P>We present multi-wavelength observations of a typical long duration GRB 120326A at z = 1.798, including rapid observations using a Submillimeter Array (SMA) and a comprehensive monitoring in the X-ray and optical. The SMA observation provided the fastest detection to date among seven submillimeter afterglows at 230 GHz. The prompt spectral analysis, using Swift and Suzaku, yielded a spectral peak energy of E-peak(src) = 107.8(- 15.3)(+15.3) keV and an equivalent isotropic energy of E-iso as 3.18(-0.32)(+0.40) x 10(52) erg. The temporal evolution and spectral properties in the optical were consistent with the standard forward shock synchrotron with jet collimation (6 degrees.69 +/- 0 degrees.16). The forward shock modeling, using a two-dimensional relativistic hydrodynamic jet simulation, was also determined by the reasonable burst explosion and the synchrotron radiation parameters for the optical afterglow. The X-ray light curve showed no apparent jet break and the temporal decay index relation between the X-ray and optical (alpha o - alpha x = -1.45 +/- 0.10) indicated different radiation processes in each of them. Introducing synchrotron self-inverse Compton radiation from reverse shock is a possible solution, and the detection and slow decay of the afterglow in submillimeter supports that this is a plausible idea. The observed temporal evolution and spectral properties, as well as forward shock modeling parameters, enabled us to determine reasonable functions to describe the afterglow properties. Because half of the events share similar properties in the X- ray and optical as the current event, GRB 120326A will be a benchmark with further rapid follow-ups, using submillimeter instruments such as an SMA and the Atacama Large Millimeter/submillimeter Array.</P>
Urata, Yuji,Huang, Kuiyun,Im, Myungshin,Lee, Induk,Deng, Jinsong,Ip, WingHuen,Krimm, Hans,Liping, Xin,Ohno, Masanori,Qiu, Yulei,Sugita, Satoshi,Tashiro, Makoto,Wei, Jianyan,Yamaoka, Kazutaka,Zheng, We IOP Publishing 2009 ASTROPHYSICAL JOURNAL LETTERS - Vol.706 No.1
<P>We present multi-band results for GRB071010B based on Swift, Suzaku, and ground-based optical observations. This burst is an ideal target to evaluate the robustness of the E-peak(src) - E-iso and E-peak(src) - E-gamma relations, whose studies have been in stagnation due to the lack of the combined estimation of E-peak(src) and long-term optical monitoring. The joint prompt spectral fitting using Swift/Burst Alert Telescope and Suzaku/Wide-band All-sky Monitor data yielded the spectral peak energy as E-peak(src) of 86.5(-6.3)(+6.4) keV and E-iso of 2.25(-0.16)(+0.19) x 10(52) erg with z = 0.947. The optical afterglow light curve is well fitted by a simple power law with temporal index alpha = -0.60 +/- 0.02. The lower limit of temporal break in the optical light curve is 9.8 days. Our multi-wavelength analysis reveals that GRB071010B follows E-peak(src) - E-iso but violates the E-peak(src) - E-gamma and E-iso - E-peak(src) - t(jet)(src) at more than the 3 sigma level.</P>