3C 66B as a TeV radio galaxy
3C 66B as a TeV radio galaxy
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3C 66B 作为 TeV 射电星系
DOI：
10.1111/j.1745-3933.2009.00629.x
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发表时间：
2008
影响因子：
--
通讯作者：
G. Ghisellini
中科院分区：
文献类型：
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作者：
F. Tavecchio;G. Ghisellini
主要大气伽马射线成像切伦科夫望远镜（MAGIC）合作报告了一个新的非常高的能量源MAGIC J 0223 +430的探测结果，它位于blazar 3C 66 A的位置附近，很长一段时间以来一直被认为是TeV blazar的候选者。仔细的分析显示，能量超过150 GeV的事件集中在Fanaro-Riley I型射电星系3C 66 B的位置（距离3C 66 A 6弧分），有95.4%的可能性（包括系统不确定性的85.4%），该来源与3C 66 A无关。我们提出了一个模型的基础上的结构喷流模型已经用来解释TeV的射电星系M87的排放的3C 66 B的可能的排放。该模型需要的参数类似于M87，但更大的光度层，占更明亮的TeV发射。我们还表明，通过MAGIC获得的光谱可以解释为3C 66 B的组合发射，占主导地位的超过200 GeV，和3C 66 A。来自后一个源的高能辐射，由于与河外背景光的相互作用而被强烈衰减，只能在低能量下起作用。如果我们在小视角下看到3C 66 B的喷流发射，我们会看到光谱能量分布与典型的耀变体S5 0716+714非常相似。
The Major Atmospheric Gamma-ray Imaging Cherenkov (MAGIC) Telescope collaboration reported the detection of a new very high energy source, MAGIC J0223+430, located close to the position of the blazar 3C 66A, considered a candidate TeV blazar since a long time. A careful analysis showed that the events with energies above 150 GeV are centred on the position of the Fanaro–Riley type I radio galaxy 3C 66B (at 6 arcmin from 3C 66A), with a probability of 95.4 per cent (85.4 per cent including systematic uncertainties) that the source is not related to 3C 66A. We present a model for the possible emission of 3C 66B based on the structured jet model already used to interpret the TeV emission of the radio galaxy M87. The model requires parameters similar to those used for M87 but a larger luminosity for the layer, to account for the more luminous TeV emission. We also show that the spectrum obtained by MAGIC can be interpreted as the combined emission of 3C 66B, dominating above ∼200 GeV, and 3C 66A. The high-energy emission from the latter source, being strongly attenuated by the interaction with the extragalactic background light, can only contribute at low energies. If we were to see the jet emission of 3C 66B at small viewing angles, we would see a spectral energy distribution closely resembling the one of S5 0716+714, a typical blazar.
从喷气式飞机方案到基础方案
DOI：
--
发表时间：
2009
期刊：
影响因子：
--
作者：
T.Kobayashi;G.Mano;S. Ogawa;M. Hino and T. Kumagai;間瀬 茂;S.Ishii
通讯作者：
S.Ishii