论文标题
以$ z \ simeq $ 0.45打破规则：RBS 1055的叛军案例
Breaking the rules at $z\simeq$0.45: the rebel case of RBS 1055
论文作者
论文摘要
我们报告了2021年3月进行的长期（250 ks）nustar观察到了明亮的准rbs 1055，以及2014年7月进行的档案XMM-Newton指数（185 ks）。在palomar观测值，Quasi-Simultane的双光谱仪与Quasimultane ustane的光谱谱相光谱中，与Noustar obustar oberestations一起分析。我们发现，两孔的模型，其中一个温暖而热的电晕并存，很好地重现了其宽带频谱，温度kt $ _e = 0.12^{+0.08} _ { - 0.03} $ kev，kt $ _e = 30^{+40^{+40^{+40} _ {-10} _ { - 10} $ kev and thomson $τ$ = 30 $ _ { - 10}^{+15} $和$τ$ = 3.0 $ _ { - 1.4}^{+1.0} $分别为前者和后一个组件。我们确认存在强烈的fe k $α$排放线（ew = 55 $ \ pm $ 6 ev），并且当考虑用于重现康普顿反思的圆环模型时，使用n $ _ {\ rm h} =（3.2^{+0.9} $ 0.8} $ {$ 0.8} $ {$ n $ _ {\ rm h} = n $ _ {\ rm h}^$ {$ n}^223^m对于环形反射器。对光谱的分析揭示了我们相对于细胞核的视线的特殊配置，并且存在广泛的[O III]组件，在NLR中追踪流出，并带有速度偏移$ v = $ 1500 $ \ pm100 $ \ pm100 $ \ pm100 $ s $ s $ s $ s $^{ - 1} $ $ nlim y; out} = 25.4 \ pm1.5 $ m $ _ {\ odot} $ yr $^{ - 1} $和流动动力$ \ dot {e} _ {\ rm kin} $/l $ _ {我们估计BH质量在2.8 $ \ times $ 10 $^{8} $ - 1.2 $ \ times $ 10 $^{9} $ m $ _ {\ odot} $，根据不同的BLR发射线，平均价值为<$ m \ m \ rm_ {bh} $ {bh} $ = 6.5 $ \ = 6.5 $ \ \ $ \ $ \ $ \ \ $ \ \ $ \ \ $ \ \ \ $ \ \ $ \ \ $ \^8} 8 m $ _ {\ odot} $。具有Fe k $α$，比EW-L $ _ {2-10 \\ rm kev} $相关的价值高3 $σ$，并且在2 keV处的极端源亮度（比光学/UV预期的10-15个要素10-15），RBS 1055证实，RBS 1055证实与x-Rays相比，与其他相同的对象相比，与其他相同的对象相比，相比之下。
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.
