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首页> 外文期刊>The Astrophysical journal >MULTIWAVELENGTH OBSERVATIONS OF STRONG FLARES FROM THE TeV BLAZAR 1ES 1959+650
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MULTIWAVELENGTH OBSERVATIONS OF STRONG FLARES FROM THE TeV BLAZAR 1ES 1959+650

机译：TeV Blazar 1ES 1959 + 650的强耀斑的多波长观测

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Following the detection of strong TeV γ-ray flares from the BL Lac object 1ES 1959+650 with the Whipple 10m Cerenkov telescope on 2002 May 16 and 17, we performed intensive target of opportunity radio, optical, X-ray, and TeV γ-ray observations from 2002 May 18 to August 14. Observations with the X-ray telescope Rossi X-Ray Timing Explorer and the Whipple and HEGRA γ-ray telescopes revealed several strong flares, enabling us to sensitively test the X-ray-γ-ray flux correlation properties. Although the X-ray and γ-ray fluxes seemed to be correlated in general, we found an "orphan" γ-ray flare that was not accompanied by an X-ray flare. While we detected optical flux variability with the Boltwood and Abastumani observatories, the data did not give evidence for a correlation of the optical flux variability with the observed X-ray and γ-ray flares. Within statistical errors of about 0.03 Jy at 14.5 GHz and 0.05 Jy at 4.8 GHz, the radio fluxes measured with the University of Michigan Radio Astronomy Observatory stayed constant throughout the campaign; the mean values agreed well with the values measured on 2002 May 7 and June 7 at 4.9 and 15 GHz with the Very Large Array and at 4.8 GHz with archival flux measurements. After describing in detail the radio, optical, X-ray and γ-ray light curves, and spectral energy distributions (SEDs), we present initial modeling of the SED with a simple synchrotron self-Compton model. With the addition of another TeV blazar with good broadband data, we consider the set of all TeV blazars, to begin to look for a connection of the jet properties to the properties of the central accreting black hole thought to drive the jet. Remarkably, the temporal and spectral X-ray and γ-ray emission characteristics of TeV blazars are very similar, even though the mass estimates of their central black holes differ by up to 1 order of magnitude.
机译：在2002年5月16日和17日用Whipple 10m Cerenkov望远镜从BL Lac对象1ES 1959 + 650检测到强烈的TeVγ射线耀斑后，我们对机会射电，光学，X射线和TeVγ-进行了密集目标从2002年5月18日至8月14日进行X射线观测。使用X射线望远镜Rossi X射线定时资源管理器以及Whipple和HEGRAγ射线望远镜进行的观测显示出几个强烈的耀斑，使我们能够灵敏地测试X射线γ射线。通量相关特性。尽管X射线通量和γ射线通量似乎总体上是相关的，但我们发现“孤儿”γ射线耀斑没有伴随X射线耀斑。虽然我们用Boltwood和Abastumani天文台检测到光通量变化，但数据并未提供光通量变化与观测到的X射线和γ射线耀斑相关的证据。在14.5 GHz时约0.03 Jy和4.8 GHz时约0.05 Jy的统计误差范围内，密歇根大学射电天文台测得的无线电通量在整个战役中保持恒定。平均值与2002年5月7日和6月7日在甚大阵列上在4.9和15 GHz上以及在档案通量测量下在4.8 GHz上测得的值非常吻合。在详细描述了无线电，光学，X射线和γ射线的光曲线以及光谱能量分布（SED）之后，我们用简单的同步加速器自康普顿模型介绍了SED的初始模型。通过添加另一个具有良好宽带数据的TeV blazar，我们考虑所有TeV blazar的集合，开始寻找射流特性与认为是驱动射流的中央吸积黑洞的特性之间的联系。值得注意的是，TeV blazar的时间和光谱X射线和γ射线发射特性非常相似，即使其中心黑洞的质量估计相差最多1个数量级。

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