COSMOS中的逃逸黑洞：是引力波还是弹弓反冲？
A Runaway Black Hole in COSMOS: Gravitational Wave or Slingshot Recoil?
摘要：
我们提出了一个特殊的源在COSMOS调查在z=0.359的详细研究。源CXOCJ 100043.1 +020637（CID-42）呈现嵌入在同一星系中的两个紧凑的光源。在HST/ACS图像中测量的2之间的距离是0.495”，在源的红移处，对应于2.46 kpc的投影分离。在VLT/VIMOS和Magellan/IMACS仪器的三种不同光谱中，测量了Hbeta窄分量和宽分量之间的大（~1200 km/s）速度偏移。CID-42也是唯一的X射线源，在其X射线光谱中具有强红移的宽吸收铁线和铁发射线，绘制了倒置的P-Cygni轮廓。钱德拉和XMM的数据表明，吸收线的能量在4年内变化了500 eV，并且吸收剂必须高度电离，以便不在软X射线光谱中留下签名。这些特征出现在同一个源中不太可能是巧合。我们设想了两种可能的解释：（1）引力波反冲的黑洞（BH），在合并后捕获了1- 1000万年，（2）在同一星系中的1型/2型系统，其中1型由于三重BH系统产生的弹弓效应而反冲。第一种可能性为我们提供了一个候选的引力波反冲BH与光谱和成像的签名。在第二种情况下，X射线吸收线可以解释为从前景核（2型活动星系核）到较远的活动星系核（1型活动星系核）的类似BAL-like外流，它照亮了原本无法探测到的风，这给了我们第一次机会来表明在模糊的活动星系核中存在快速风。
英文摘要：
We present a detailed study of a peculiar source in the COSMOS survey at z=0.359. Source CXOCJ100043.1+020637 (CID-42) presents two compact optical sources embedded in the same galaxy. The distance between the 2, measured in the HST/ACS image, is 0.495" that, at the redshift of the source, corresponds to a projected separation of 2.46 kpc. A large (~1200 km/s) velocity offset between the narrow and broad components of Hbeta has been measured in three different optical spectra from the VLT/VIMOS and Magellan/IMACS instruments. CID-42 is also the only X-ray source having in its X-ray spectra a strong redshifted broad absorption iron line, and an iron emission line, drawing an inverted P-Cygni profile. The Chandra and XMM data show that the absorption line is variable in energy by 500 eV over 4 years and that the absorber has to be highly ionized, in order not to leave a signature in the soft X-ray spectrum. That these features occur in the same source is unlikely to be a coincidence. We envisage two possible explanations: (1) a gravitational wave recoiling black hole (BH), caught 1-10 Myr after merging, (2) a Type 1/ Type 2 system in the same galaxy where the Type 1 is recoiling due to slingshot effect produced by a triple BH system. The first possibility gives us a candidate gravitational waves recoiling BH with both spectroscopic and imaging signatures. In the second case, the X-ray absorption line can be explained as a BAL-like outflow from the foreground nucleus (a Type 2 AGN) at the rearer one (a Type 1 AGN), which illuminates the otherwise undetectable wind, giving us the first opportunity to show that fast winds are present in obscured AGN.
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