action中的活动星系核/星爆联系：NGC1365的50万秒RGS谱
AGN/starburst connection in action: the half million second RGS spectrum of NGC1365
摘要：
我们提出了一个深（~5.8天）0.3-2千电子伏的高分辨率光谱的NGC 1365，收集与反射光栅光谱仪（RGS）的XMM-牛顿。该光谱主要是由强的复合线的He和H-样的过渡从碳到硅，以及从FeXVII的L过渡。连续性很强，特别是在10到20埃的范围内。正式的配合需要两个光学薄，碰撞电离等离子体组件，温度约300和约640 eV。然而，他们留下了大部分的He-α OVII和NVI三联体的违禁成分。这些特征可以解释为由光电离气体产生。因此，NGC 1365是第一个被遮蔽的活动星系核，它的高分辨率X射线光谱需要碰撞电离和光电离。光致电离的相对弱并不源于活动星系核的内在弱性，活动星系核的X射线光度约为10^{42} erg/s。我们认为，它可能反而来自于从活动核到NLR的视线被宽线区域中的光学厚物质阻挡，同时负责观测到的大的柱密度变化遮蔽X射线活动核。或者，NGC 1365可能拥有一个与活动星系核吸积功率相比非常明亮的核恒星爆发。
英文摘要：
We present a deep (~5.8 days) 0.3-2 keV high-resolution spectrum of NGC1365, collected with the reflection grating spectrometer (RGS) on board XMM-Newton. The spectrum is dominated by strong recombination lines of He- and H-like transitions from carbon to silicon, as well as by L transitions from FeXVII. The continuum is strong, especially in the 10 to 20 Angstrom, range. Formal fits require two optically thin, collisionally ionised plasma components, with temperatures ~300 and ~640 eV. However, they leave the bulk of the forbidden components of the He-alpha OVII and NVI triplets unaccounted for. These features can be explained as being produced by photoionised gas. NGC1365 is therefore the first obscured AGN, whose high-resolution X-ray spectrum requires both collisional ionisation and photoionisation. The relative weakness of photoionisation does not stem from the intrinsic weakness of its AGN, whose X-ray luminosity is ~10^{42} erg/s. We suggest that it may instead come from the line-of-sight from the active nucleus to the NLR being blocked by optically thick matter in the broad line region, at the same time responsible for the large observed variation of the column density obscuring the X-ray active nucleus. Alternatively, NGC1365 could host a remarkably luminous nuclear starburst when compared to the AGN accretion power [abriged].
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