论文标题
更换外观活跃的银河核MRK 590中消失的软X射线过量的起源
The origin of the vanishing soft X-ray excess in the changing-look Active Galactic Nucleus Mrk 590
论文作者
论文摘要
我们使用了\ xmm {}，\ suzaku {}，\ suzaku {}，\ swift {}和\ nustar {}的二十年多波长观测，研究了有趣的更换AGN（clagn）MRK 〜590中检测到的软X射线多余的性质和起源。鉴于在此策略中消失的软过量，我们使用广泛的UV/X射线光谱分析测试了两个模型，“温暖的组合”和“电离磁盘反射”。我们的主要发现是：（1）柔软的X射线过量发射，最后一次观察到，在2011年消失，在任何后来的观察结果中从未重新出现过，（2）我们在观察到的观察结果和最低状态（$ l _ _ pl _ pl _ pl _ plol plux and pertical-lux and pertial-uv and time l _ _ plol _ ploc}之间发现了显着的可变性（$ \ sim300 \％$ $）。 10^{43}\, erg\, s^{-1}$, in 2016) and the highest state ($L_{\rm bol} = 1.2\times 10^{44}\, erg\, s^{-1}$, in 2018), (3) the UV and power-law fluxes follow same temporal pattern, (4) the photon index showed a significant variation （$γ= 1.88^{+0.02} _ { - 0.08} $和$γ= 1.58^{+0.02} _ { - 0.02} _ { - 0.03} $在2002年和2021年分别在观察值之间），（5）在源较窄的fe $k_α中未检测到compton hump，但在狭窄的fe $k_α中均在范围内检测到6个erevers nisevions（6），所有观察者均为6 sib nisevers（6）在Power-Law Continuum（$ 92^{+55} _ { - 25} \ rm kev $和$ 60^{+10} _ { - 08} \ rm kev $）中使用最新的\ nustar {}观察值，（7）其他diskbb compoents no isskb corment of correl correl no isor correl un correl uv buck uv uv buck uv buck uv buck uv und uv buck uv und bump uv un Eddington速率和其他更换AGN中发现的软过量。我们得出的结论是，鉴于紫外/X射线的光谱变化，离子磁盘反射或温暖的构成模型可能不足以描述MRK 〜590中观察到的消失的软过量特征。
We have studied the nature and origin of the soft X-ray excess detected in the interesting changing-look AGN (CLAGN) Mrk~590 using two decades of multi-wavelength observations from \xmm{}, \suzaku{}, \swift{} and \nustar{}. In the light of vanishing soft excess in this CLAGN, we test two models, "the warm Comptonization" and "the ionized disk reflection" using extensive UV/X-ray spectral analysis. Our main findings are: (1) the soft X-ray excess emission, last observed in 2004, vanished in 2011, and never reappeared in any of the later observations, (2) we detected a significant variability ($\sim300\%$) in the observed optical-UV and power-law flux between observations with the lowest state ($L_{\rm bol} = 4.4\times 10^{43}\, erg\, s^{-1}$, in 2016) and the highest state ($L_{\rm bol} = 1.2\times 10^{44}\, erg\, s^{-1}$, in 2018), (3) the UV and power-law fluxes follow same temporal pattern, (4) the photon index showed a significant variation ($Γ=1.88^{+0.02}_{-0.08}$ and $Γ=1.58^{+0.02}_{-0.03}$ in 2002 and 2021 respectively) between observations, (5) no Compton hump was detected in the source spectra but a narrow Fe$K_α$ line is present in all observations, (6) we detected a high-energy cut-off in power-law continuum ($92^{+55}_{-25} \rm keV$ and $60^{+10}_{-08} \rm keV$) with the latest \nustar{} observations, (7) the warm Comptonization model needs an additional diskbb component to describe the source UV bump, (8) there is no correlation between the Eddington rate and the soft excess as found in other changing-look AGNs. We conclude that given the spectral variability in UV/X-rays, the ionized disk reflection or the warm Comptonization models may not be adequate to describe the vanishing soft excess feature observed in Mrk~590.
