论文标题
Chandra的衬里型核的视图在无线电大通星系CGCG中292-057：电离铁线和喷气主义相互作用
Chandra View of the LINER-type Nucleus in the Radio-Loud Galaxy CGCG 292-057: Ionized Iron Line and Jet-ISM Interactions
论文作者
论文摘要
我们介绍了对新的，深（94 \，ksec）{\ it chandra} acis-s观察的分析，该ACIS-S-S-S-S-S-S-S-S-S-S-S-S-S-S-S-S-S-S-S-S-S-S-S-S-S-S-S-S-S-S-S-S-S-S-S-S-S-S-S-S-S-S-S-S-S-S-S-S-S-S-S-S-S-S分析则分析，其特征是衬里型核和复杂的无线电结构，表明了间歇性喷射活性。在主机星系凸起的规模上，我们检测到过量的X射线发射，通过热等离子体模型最佳拟合，温度为$ \ sim 0.8 $ \，kev。我们认为，这种过量的发射是由于在此重新启动的射电星系中观察到的，由扩展的内部，$ \ sim 20 $ \，KPC-Scale Lobes置换的星际介质的热弥漫级数引起的。目标的核X射线频谱清楚地显示了一条电离铁线，以$ \ sim 6.7 $ \，keV显示，并且最好配合一个现象学模型，该模型由幂律（光子索引$ \ simeq 1.8 $）连续吸收，可被相对较大的冷物质（氢柱密度$ \ simeq 0.7 \ simeq 0.7 \ simeq 0.7 \ simeq 0.7 \ simeq 0.7 \ simeq 0.7 \ simeq 0.7 \ simeq 0.7 \ simeq。 10^{23} $ \，cm $^{ - 2} $），并通过电离气体部分分散（分数$ \ sim 3 \％$），从而产生了柔软的多余分量和铁离子的k $α$ line。我们证明，观察到的X射线频谱，尤其是Fe \，\ texttt {xxv} k $α$的等效宽度（原则上的$ 0.3 $ \，kev）可以在涉及该源属于该源的核型和核照片规模的compton-phin gas的情况下进行解释。我们将CGCG \，292 $ - $ 057核的一般光谱特性与附近的其他衬里的核心进行了比较。
We present an analysis of the new, deep (94\,ksec) {\it Chandra} ACIS-S observation of radio-loud active galaxy CGCG\,292$-$057, characterized by a LINER-type nucleus and a complex radio structure that indicates intermittent jet activity. On the scale of the host galaxy bulge, we detected excess X-ray emission with a spectrum best fit by a thermal plasma model with a temperature of $\sim 0.8$\,keV. We argue that this excess emission results from compression and heating of the hot diffuse fraction of the interstellar medium displaced by the expanding inner, $\sim 20$\, kpc-scale lobes observed in this restarted radio galaxy. The nuclear X-ray spectrum of the target clearly displays an ionized iron line at $\sim 6.7$\,keV, and is best fitted with a phenomenological model consisting of a power-law (photon index $\simeq 1.8$) continuum absorbed by a relatively large amount of cold matter (hydrogen column density $\simeq 0.7 \times 10^{23}$\,cm$^{-2}$), and partly scattered (fraction $\sim 3\%$) by ionized gas, giving rise to a soft excess component and K$α$ line from iron ions. We demonstrate that the observed X-ray spectrum, particularly the equivalent width of Fe\,\texttt{XXV} K$α$ (of order $0.3$\,keV) can in principle, be explained in a scenario involving a Compton-thin gas located at the scale of the broad-lined region in this source and photoionized by nuclear illumination. We compare the general spectral properties of the CGCG\,292$-$057 nucleus, with those of other nearby LINERs studied in X-rays.
