Spectroscopy of AGN-dominated ULIRGs: NGC 6240

NGC 6240 is a known ULIRG which is unique among such objects because its Xrayspectrum is very similar to those of many Seyfert 2s yet its IR spectrum showsno indication of gas excitation by a nonthermal source. Thus, there is a bigquestion regarding the major energy source with important implications to theXray background and the AGNstarburst connection. We propose 100 ks XMMobservations to reveal the nature of this source and show how a good S/N RGSspectrum containing 1015 measurable lines, combined with a stateoftheartanalysis, can probe the physical state of the soft Xray gas and supplyinformation about its excitation by a starburs, an AGN source, or both. MOS andPN observations will define the SED and resolve the complex emissionabsorption feature near 68 keV. truncated!, Please see actual data for full text [truncated!, Please see actual data for full text]

NGC 6240 是一种已知的超亮红外星系，此类星系中其独特的特性在于其X射线光谱与众多塞弗特2型星系相似，而其红外光谱却并未显示出由非热源激发的气体激发迹象。因此，关于其主要能量来源的问题引起了广泛关注，这对X射线背景以及活动星系核爆发的联系具有重要意义。我们提议进行100 ks的XMM观测，以揭示该源的本质，并展示如何通过包含1015条可测量线的优秀信噪比RGS光谱，结合最先进的分析技术，探究软X射线气体的物理状态，并为其由恒星爆发、活动星系核源或两者共同激发提供信息。MOS和PN观测将确定光谱能量分布，并解析68 keV附近的复杂发射吸收特征。具体数据请查阅实际数据[数据截断，请查阅实际数据]。