arXiv 0712.34452007-12-20astro-ph

2型射电噪类星体3C 234的XMM-牛顿谱中的重吸收和软X射线发射谱线

Heavy absorption and soft X-ray emission lines in the XMM-Newton spectrum of the Type 2 radio-loud quasar 3C 234

E. Piconcelli, S. Bianchi, G. Miniutti, F. Fiore, M. Guainazzi, E. Jimenez-Bailon, G. Matt

备注：: Accepted by Astronomy and Astrophysics
DOI：: 10.1051/0004-6361:20078746

摘要：

我们报告的结果，40 ksXMM牛顿观测的2型类星体3C 234。光学偏振光谱数据表明，在这个强有力的窄线FRII射电星系中（经红化和星光校正后，M_V <~ -24.2）存在着一个隐藏的宽线区。我们的分析旨在研究这个迄今为止知之甚少的奇特源的X射线光谱特性。我们分析了2006年EPIC相机收集的0.5- 10 keV光谱数据。这颗射电巨响类星体的X射线光谱是典型的局部康普顿薄塞弗特2星系。它表现出强吸收（Nh~3.5 x 10^{23} cm^{-2}）和窄的中性Fe Ka发射线，等效宽度为~140+/-40 eV。我们的观察还表明，光谱的软部分的特征在于具有非常低水平的散射初级连续谱的强发射线。用双温碰撞电离等离子体发射的热发射来解释这些特征似乎是不可能的，因为估计这个分量的光度很高（L（0.5-2）~ 6 x 10^{42} erg/s）。这可能是大多数的软X射线发射起源于一个光电离等离子体，通常在模糊的，无线电安静的赛弗类活动星系核中观察到。这一X射线观测明确证实了3C 234中隐藏的类星体的存在。该源的富谱线和硬X射线连续谱（γ ~ 1.7）的陡度削弱了射电噪活动星系核中具有高激发光线的X射线发射主要来自喷注非热发射的假设。

英文摘要：

We report results on a 40 ks XMM-Newton observation of the Type 2 quasar 3C 234. Optical spectropolarimetric data have demonstrated the presence of a hidden broad-line region in this powerful (M_V <~ -24.2 after reddening and starlight correction) narrow-line FRII radio galaxy. Our analysis is aimed at investigating the X-ray spectral properties of this peculiar source which have remained poorly known so far. We analyze the 0.5--10 keV spectroscopic data collected by the EPIC cameras in 2006. The X-ray spectrum of this radio-loud quasar is typical of a local Compton-thin Seyfert 2 galaxy. It exhibits strong absorption (Nh~3.5 x 10^{23} cm^{-2}) and a narrow, neutral Fe Kalpha emission line with an equivalent width of ~140+/-40 eV. Our observation also reveals that the soft portion of the spectrum is characterized by strong emission lines with a very low level of scattered primary continuum. A possible explanation of these features in terms of thermal emission from a two-temperature collisionally ionized plasma emission seems to be unlikely due to the high luminosity estimated for this component (L(0.5-2) ~ 6 x 10^{42} erg/s). It is likely that most of the soft X-ray emission originates from a photoionized plasma as commonly observed in obscured, radio-quiet Seyfert-like AGNs. This X-ray observation has definitively confirmed the presence of a hidden quasar in 3C 234. The line-rich spectrum and the steepness of the hard X-ray continuum (Gamma ~ 1.7) found in this source weaken the hypothesis that the bulk ofthe X-ray emission in radio-loud AGNs with high excitation optical lines arises from jet non-thermal emission.

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