用XMM-牛顿法对PG 2112+059的最小状态进行长时间的研究
A long hard look at the minimum state of PG 2112+059 with XMM-Newton
摘要：
XMM-Newton在短时间的快照观测中成功探测到PG 2112+059的最小状态，并进行了长时间的跟踪观测。假设不同的排放情况下，并与档案光谱XMM-牛顿和钱德拉相比，模拟高信噪比光谱。2007年5月获得的PG 2112+059 X射线光谱允许检测到弱铁荧光线，这被解释为是由距离主要X射线发射源一定距离的中性物质反射引起的。PG 2112+059在不同通量状态下的五个不同时期拍摄的X射线光谱可以在两种不同的情况下解释。第一层由两层电离物质组成，柱密度分别为N_H ~5 x 10^22 cm^-2和N_H ~3.5 x 10^23 cm^-2。第一层是中度电离的，其电离水平遵循通量变化，而另一层是高度电离的，并没有显示出与源通量的任何相关性。光谱也可以解释为假设反射的电离吸积盘后面看到一个温暖的吸收。温暖的吸收体电离是一致的，与源的通量相关，这提供了一个额外的程度的自我一致性与整体反射为基础的模型。我们根据Miniutti和Fabian模型解释了光谱随光弯曲的变化，并将黑洞的自旋限制在a/M > 0.86.这两种情况也假设一个遥远的冷反射层是造成Fe K α发射线的原因。光弯曲为PG 2112+059的不同状态提供了一个有吸引力的解释，也可能描述其他X射线弱类星体观测到的性质的物理原因。
英文摘要：
XMM-Newton successfully detected the minimum state of PG 2112+059 during a short snapshot observation and performed a long follow-up observation. The high signal-to-noise spectra are modelled assuming different emission scenarios and compared with archival spectra taken by XMM-Newton and Chandra. The PG 2112+059 X-ray spectra acquired in May 2007 allowed the detection of a weak iron fluorescent line, which is interpreted as being caused by reflection from neutral material at some distance from the primary X-ray emitting source. The X-ray spectra of PG 2112+059 taken at five different epochs during different flux states can be interpreted within two different scenarios. The first consists of two layers of ionised material with column densities of N_H ~5 x 10^22 cm^-2 and N_H ~3.5 x 10^23 cm^-2, respectively. The first layer is moderately ionised and its ionisation levels follow the flux changes, while the other layer is highly ionised and does not show any correlation with the flux of the source. The spectra can also be interpreted assuming reflection by an ionised accretion disk seen behind a warm absorber. The warm absorber ionisation is consistent with being correlated with the flux of the source, which provides an additional degree of self-consistency with the overall reflection-based model. We explain the spectral variability with light bending according to the models of Miniutti and Fabian and constrain the black hole spin to be a/M > 0.86. Both scenarios also assume that a distant cold reflector is responsible for the Fe K αemission line. Light bending provides an attractive explanation of the different states of PG 2112+059 and may also describe the physical cause of the observed properties of other X-ray weak quasars.
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