2008年光-无线电和gamma-ray爆发期间3C 454.3的GASP-WEBT监测
The GASP-WEBT monitoring of 3C 454.3 during the 2008 optical-to-radio and gamma-ray outburst
摘要：
自2001年以来，射电类星体3C 454.3经历了一段高光学活动的时期，在2004-2005年的爆发中达到了有史以来最亮的光学状态。全球Blazar望远镜（WEBT）联合体已经开展了几次多频活动，以跟踪源的行为。GLAST-AGILE支持计划（GASP）诞生于WEBT，在AGILE和GLAST（现在称为费米GST）伽马射线卫星运行期间，对伽马大声耀变体样本进行长期连续的光-无线电监测。主要目的是通过与低能辐射的相关分析，阐明高能辐射产生的机制。因此，自2008年以来，3C 454.3的监测任务从WEBT转移到了GASP，而AGILE和费米都检测到了来自该源的强烈伽马射线发射。我们提出了在2008-2009年季节的光学，毫米，和射频的GASP获得的主要结果，并将它们与前几年的WEBT结果进行比较。2008年7月中旬，费米望远镜观测到了最亮的伽马射线，并观测到了一次光学爆发。一个同期毫米爆发保持其亮度较长的时间，直到厘米排放也达到最大水平。在三个波段的行为比较表明，不同频率的爆发的相对亮度的变量可能是由于一个弯曲的不均匀射流的方向变化。光学光变曲线在整个季节都得到了很好的采样，这也被AGILE和费米的各种观测周期很好地覆盖了。相关的互相关研究对于约束高能辐射模型具有重要意义。
英文摘要：
Since 2001, the radio quasar 3C 454.3 has undergone a period of high optical activity, culminating in the brightest optical state ever observed, during the 2004-2005 outburst. The Whole Earth Blazar Telescope (WEBT) consortium has carried out several multifrequency campaigns to follow the source behaviour. The GLAST-AGILE Support Program (GASP) was born from the WEBT to provide long-term continuous optical-to-radio monitoring of a sample of gamma-loud blazars, during the operation of the AGILE and GLAST (now known as Fermi GST) gamma-ray satellites. The main aim is to shed light on the mechanisms producing the high-energy radiation, through correlation analysis with the low-energy emission. Thus, since 2008 the monitoring task on 3C 454.3 passed from the WEBT to the GASP, while both AGILE and Fermi detected strong gamma-ray emission from the source. We present the main results obtained by the GASP at optical, mm, and radio frequencies in the 2008-2009 season, and compare them with the WEBT results from previous years. An optical outburst was observed to peak in mid July 2008, when Fermi detected the brightest gamma-ray levels. A contemporaneous mm outburst maintained its brightness for a longer time, until the cm emission also reached the maximum levels. The behaviour compared in the three bands suggests that the variable relative brightness of the different-frequency outbursts may be due to the changing orientation of a curved inhomogeneous jet. The optical light curve is very well sampled during the entire season, which is also well covered by the various AGILE and Fermi observing periods. The relevant cross-correlation studies will be very important in constraining high-energy emission models.
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