打破规则在$z\simeq$ 0.45：叛乱案件的RBS 1055
Breaking the rules at $z\simeq$0.45: the rebel case of RBS 1055
摘要：
我们报告了2021年3月对明亮类星体RBS 1055进行的长时间（250 ks）NuSTAR观测，以及2014年7月拍摄的档案XMM-牛顿点（185 ks）。还分析了与NuSTAR观测准同时进行的Palomar天文台双摄谱仪源的光谱。我们发现，两个日冕模型，其中一个温暖的和热的日冕共存，很好地再现其宽带光谱，与温度kT $_e=0.12^{+0.08}_{-0.03}$ keV，kT $_e=30^{+40}_{-10}$ keV和汤姆逊光学深度$τ$ =30 $_{-10}^{+15}$和$τ$ =3.0 $_{-1.4}^{+1.0}$分别为前者和后者组件。我们确认了强的Fe K $α$发射线的存在（EW=55 $\pm$ 6 eV），当考虑环形模型再现康普顿反射时，发现环核反射面的康普顿薄解为N $_{\rm H}=(3.2^{+0.9}_{-0.8})\times10^{23}$ cm $^{-2}$.光谱分析揭示了我们视线相对于原子核的一种可能的特殊构型，和广泛的[O III]成分的存在，在NLR中追踪流出，速度偏移$v=$ 1500 $\pm100$ km s $^{-1}$，导致质量流出率$\dot{M}_{\rm out}=25.4\pm1.5$ M $_{\odot}$ yr $^{-1}$和流出动能$\dot{E}_{\rm kin}$ /L $_{\rm Bol}$ $\sim$ 0.33%。根据不同的BLR发射线，我们估计BH的质量在2.8 $\times$ 10 $^{8}$ -1.2 $\times$ 10 $^{9}$ M $_{\odot}$的范围内，平均值为< $M\rm_{BH}$ >=6.5 $\times$ 10 $^{8}$ M $_{\odot}$。由于Fe K $α$比从EW-L $_{2-10\ \rm keV}$关系预测的值高出3 $σ$，并且极端光源亮度为2 keV（比从光学/UV预测的亮度高10-15倍），RBS 1055被证实是X射线中的异常值，与相同光度和红移范围内的其他物体相比。
英文摘要：
We report on a long (250 ks) NuSTAR observation of the bright quasar RBS 1055 performed in March 2021, and archival XMM-Newton pointings (185 ks) taken in July 2014. An optical spectrum of the source taken with the Double Spectrograph at the Palomar Observatory, quasi-simultaneous with the NuSTAR observations, is also analyzed. We find that the two-coronae model, in which a warm and hot corona coexist, well reproduces its broad band spectrum, with temperatures kT$_e=0.12^{+0.08}_{-0.03}$ keV, kT$_e=30^{+40}_{-10}$ keV and Thomson optical depths $τ$=30$_{-10}^{+15}$ and $τ$=3.0$_{-1.4}^{+1.0}$ for the former and the latter component, respectively. We confirm the presence of an intense Fe K$α$ emission line (EW=55$\pm$6 eV) and, when a toroidal model is considered for reproducing the Compton reflection, a Compton-thin solution with N$_{\rm H}=(3.2^{+0.9}_{-0.8})\times10^{23}$ cm$^{-2}$ for the circumnuclear reflector is found. The analysis of the optical spectrum reveals a likely peculiar configuration of our line of sight with respect to the nucleus, and the presence of a broad [O III] component, tracing outflows in the NLR, with a velocity shift $v=$1500$\pm100$ km s$^{-1}$, leading to a mass outflow rate $\dot{M}_{\rm out}=25.4\pm1.5$ M$_{\odot}$ yr$^{-1}$ and outflow kinetic power $\dot{E}_{\rm kin}$/L$_{\rm Bol}$ $\sim$0.33%. We estimate the BH mass to be in the range 2.8$\times$10$^{8}$-1.2$\times$10$^{9}$ M$_{\odot}$, according to different BLR emission lines, with an average value of <$M\rm_{BH}$>=6.5$\times$10$^{8}$ M$_{\odot}$. With an Fe K$α$ which is 3$σ$ above the value predicted from the EW-L$_{2-10\ \rm keV}$ relation and an extreme source brightness at 2 keV (a factor 10-15 higher than the one expected from the optical/UV), RBS 1055 confirms to be an outlier in the X-rays, compared to other objects in the same luminosity and redshift range.
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