The results of 20‐year observations of the Perseus cluster centering on the NGC 1275 including IC 310 radio galaxy and extragalactic supernova SN 2006gy at energies 800 GeV to 45 TeV by the SHALON telescope are presented. Also, the emission from the galactic source of non‐thermal radio and X‐ray emission GK Per (Nova 1901) of classical nova type was found as it accompanied to the observations. For NGC 1275, it was found that the TeV γ‐ray emission at energies >800 GeV has an extended structure with a distinct core centered at the NGC 1275 nucleus and well correlates with the photon emission regions viewed in X‐rays by Chandra and anti‐correlates with radio‐structures. Also, the variations of TeV γ‐ray flux both at year‐ and day scales were found. The obtained data indicate that the part of TeV γ‐ray emission is generated by relativistic jets in the nucleus of NGC 1275. Whereas the presence of an extended structure around NGC 1275 and the slow rise of the γ‐ray flux is the evidence of the interaction of cosmic rays and magnetic fields generated in the jets at the galactic center with the gas of the Perseus cluster.

中文翻译：

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英仙座星团区域观测中的物体

介绍了SHALON望远镜以800 GeV至45 TeV的能量对英仙座星团以NGC 1275为中心的20年观测结果，这些星团包括IC 310射电星系和银河外超新星SN 2006gy。另外，还发现了银河源的非热辐射源和经典新星类型的X射线发射GK Per（Nova 1901），伴随着观测。对于NGC 1275，人们发现，TEV的γ在能量射线发射> 800 GeV的具有与不同的芯为中心在NGC 1275核的扩展结构和良好与由钱德拉和抗在X射线观察到的光子发射区域相关联与无线电结构相关。另外，TeV能的变化γ发现年和日尺度的射线通量。所获得的数据表明，TeV的部分γ射线发射被相对论射流产生的NGC 1275的细胞核周围而NGC 1275的扩展结构和的缓慢上升的存在γ射线通量的证据在银河系中心的射流中产生的宇宙射线和磁场与英仙座星团气体之间的相互作用。