The character of the interaction of two gaseous components which are a structural feature of the nucleus of the Seyfert galaxy NGC 1275 is established during the epoch of a minimum in its activity. A bank of emission line profiles (Hβ and O[III] λ5007Å) obtained from observations on the 1.5-m Russian-Turkish telescope (RTT-150) in January 2012 is used. The physical characteristics (Te, ne) of the emission region of the nebular line [OIII] are calculated for this observation epoch and are compared with other published data. The changes in an important spectral characteristic of the emission from the galaxy nucleus (Ewλ, the equivalent with of the Hβ and O[III] λ5007Å lines) are tracked during individual nights and from night-to-night. These studies show that the two “interpenetrating” gaseous components retain a high level of interaction over a long period of time.

中文翻译：

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2012年时代赛弗银河NGC 1275核的气体成分

塞弗特星系NGC 1275的核的结构特征是两个气态组分相互作用的特性，这是在其活性达到最小的时期开始的。的发射谱线轮廓银行（H β和O [III] λ 5007Å）从1.5米俄土耳其望远镜的观测得到的（RTT-150）在2012年1月被使用。为此观测时期计算了星云线[OIII]发射区域的物理特征（Te，ne），并将其与其他已发表的数据进行了比较。在从星系核（EW发光的一个重要的光谱特性的变化λ ，等效与H的β和O [III] λ5007Å线路）在各个晚上以及从黑夜到黑夜进行跟踪。这些研究表明，两种“相互渗透”的气态成分在很长一段时间内保持了高水平的相互作用。