揭示明亮裸AGN ESO 141-G55的燃烧与柔软内核：X射线宽带与SED分析
Revealing the burning and soft heart of the bright bare AGN ESO 141-G55: X-ray broadband and SED analysis
AI总结：
本研究通过XMM-Newton和NuSTAR同步观测分析裸AGN ESO 141-G55的盘-冕系统，发现暖热冕Compton化加相对论反射模型能很好拟合其SED，证实暖冕对软X射线和紫外发射有显著贡献。
摘要：
ESO 141-G55是邻近的X射线明亮BLS1，由于沿其视线方向缺乏暖吸收而被归类为裸AGN，为研究其盘-冕系统提供了无阻碍的视角。我们旨在利用2022年10月1-2日获得的首次XMM-Newton和NuSTAR同步观测来探测其盘-冕系统。我们进行X射线宽带光谱分析以确定主导过程，并进行SED分析以确定盘-冕性质。ESO 141-G55的同步宽带X射线光谱特征为存在显著的平滑软X射线过剩、宽Fe K发射线和显著的Compton隆起。RGS光谱证实AGN静止系中沿视线方向缺乏内禀暖吸收气体，确认其仍处于裸状态。然而，观测到软X射线发射线表明视线外存在大量暖气体。盘-冕系统的中等倾角约43°可能提供了从盘观测UFO的有利配置，但在2022年观测中未发现，与2007年XMM-Newton观测相反。标准盘上的相对论反射单独被X射线宽带分析排除，而暖和热冕的软硬Compton化（relagn）加上相对论反射（reflkerrd）很好地再现了其SED。热冕温度很高约140 keV，远高于约80%的AGN，而暖冕温度约0.3 keV与其他亚爱丁顿AGN的值相似。ESO 141-G55以中等爱丁顿吸积率（约10-20%）吸积。我们的分析指出光学厚暖冕对ESO 141-G55的软X射线和紫外发射有显著贡献。
英文摘要：
[Abridged] ESO 141-G55 is a nearby X-ray bright BLS1, which has been classified as a bare AGN due to the lack of warm absorption along its line-of-sight, providing an unhampered view into its disc-corona system. We aim to probe its disc-corona system thanks to the first simultaneous XMM-Newton and NuSTAR observation obtained on October 1-2, 2022. We carry out the X-ray broadband spectral analysis to determine the dominant process(es) at work, as well as the SED analysis to determine the disc-corona properties. The simultaneous broadband X-ray spectrum of ESO 141-G55 is characterised by the presence of a prominent smooth soft X-ray excess, a broad Fe K emission line and a significant Compton hump. The RGS spectra confirmed the lack of intrinsic warm-absorbing gas along our line of sight in the AGN rest frame, confirming that it is still in a bare state. However, soft X-ray emission lines are observed indicating substantial warm gas out of our line of sight. The intermediate inclination of the disc-corona system, ~43°, may offer us a favourable configuration to observe UFOs from the disc, but none is found in this 2022 observation, contrary to a previous 2007 XMM-Newton one. Relativistic reflection alone on a standard disc is ruled out from the X-ray broadband analysis, while a combination of soft and hard Comptonisation by a warm and hot corona (relagn), plus relativistic reflection (reflkerrd) reproduces its SED quite well. The hot corona temperature is very hot, ~140 keV, much higher than about 80% of the AGNs, whereas the warm corona temperature, ~0.3 keV, is similar to the values found in other sub-Eddington AGNs. ESO 141-G55 is accreting at a moderate Eddington accretion rate (~10--20%). Our analysis points to a significant contribution of an optically-thick warm corona to both the soft X-ray and UV emission in ESO 141-G55.
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