We have defined a sample of 63 AGN with strong forbidden high-ionisation line (FHIL) emission. These lines, with ionisation potentials >~ 100eV, respond to a portion of the spectrum that is often difficult to observe directly, thereby providing constraints on the EUV-soft X-ray continuum. The sources are selected from the Sloan Digital Sky Survey (SDSS) on the basis of their [Fe X]6374A emission, yielding one of the largest and the most homogeneous sample of FHIL-emitting galaxies. We fit a sequence of models to both FHILs ([Fe XI], [Fe X] and [Fe VII]) and lower-ionisation emission lines ([O III], [O I], H-alpha, [N II], [S II]) in the SDSS spectra. These data are combined with X-ray measurements from Rosat, which are available for half of the sample. The correlations between these parameters are discussed for both the overall sample and subsets defined by spectroscopic classifications. The primary results are evidence that: (1) the [Fe X] and [Fe XI] lines are photoionised and their strength is proportional to the continuum flux around 250 eV; (2) the FHIL-emitting clouds form a stratified outflow in which the [Fe X] and [Fe XI] source regions extend sufficiently close to the BLR that they are partially obscured in Seyfert 2s whereas the [Fe VII] source region is more extended and is unaffected by obscuration; (3) narrow-lined Seyfert 1s (NLS1s) tend to have the strongest [Fe X] flux (relative to lower-ionisation lines); and (4) the most extreme [Fe X] ratios (such as [Fe X]/[O III] or [Fe X]/[Fe VII]) are found in the NLS1s with the narrowest broad lines and appear to be an optical-band indication of objects with strong X-ray soft excesses.
Dust destruction signals shock-accelerated outflows in the nearby active galaxy NGC 1068
University of Hertfordshire（赫特福德大学）；University of Sheffield（谢菲尔德大学）；University of Cambridge（剑桥大学）；University of Edinburgh（爱丁堡大学）；Technical University of Kenya（肯尼亚科技大学）；University of Manchester（曼彻斯特大学）
Ejecta clumps revealed by study of reverse-shocked ejecta through MUSE integral field spectroscopy of SNR 0509-67.5
The University of New South Wales（新南威尔士大学）；Australian National University（澳大利亚国立大学）；Naval Research Laboratory（海军研究实验室）；The University of Manitoba（曼尼托巴大学）；RIKEN Center for Interdisciplinary Theoretical and Mathematical Sciences (iTHEMS)（理化学研究所跨学科理论与数学科学中心（iTHEMS））
Mapping the nuclear environments of extreme coronal line emitting galaxies
University of Portsmouth（朴茨茅斯大学）；American Museum of Natural History（美国自然历史博物馆）；University of Southampton（南安普顿大学）；Lawrence Berkeley National Laboratory（劳伦斯伯克利国家实验室）；Boston University（波士顿大学）；Università degli Studi di Milano（米兰大学）；INAF-Osservatorio Astronomico di Brera（INAF-布雷拉天文台）；University College London（伦敦大学学院）；Universidad Nacional Autónoma de México（墨西哥国立自治大学）
Predicting ionised gas emission in 3D with SKIRT. I. Framework and validation
Department of Physics and Astronomy, Proeftuinstraat 86 N3, B-9000 Ghent, Belgium（根特大学物理与天文学系）；Department of Physics, The University of Texas at Dallas, Richardson, Texas 75080, USA（德克萨斯大学达拉斯分校物理系）；Kavli Institute for Cosmology, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK（剑桥大学卡弗里宇宙学研究所）；Cavendish Laboratory, University of Cambridge, 19 JJ Thomson Avenue, Cambridge CB3 0HE, UK（剑桥大学卡文迪许实验室）
A Candidate Sub-Parsec Supermassive Binary Black Hole System
我们确定SDSS J153636.22+044127.0，在斯隆数字巡天发现的类星体，作为一个有前途的候选人的一个二元黑洞系统。这个类星体有两个宽线发射系统，间隔为3500公里/秒。在z=0.3889处的红系统也有一组典型的窄禁带。较蓝的系统（z=0.3727）仅显示宽的巴耳末线和UV Fe II发射，使其在缺乏窄线方面非常不寻常。第三个系统只包含未分辨的吸收线，红移z=0.3878，介于两个发射线系统之间。虽然双核黑洞的观测特征仍然不清楚，但J1536+0441在所有已知的类星体中是独一无二的，它有两个宽线区域，表明两个独立的黑洞目前正在吸积气体。将其解释为两个质量分别为10^8.9和10^7.3太阳质量的黑洞组成的束缚双星系统，得到的间隔约为0.1秒差距，轨道周期约为100年。这种分离意味着两个黑洞在一个窄线区域内运行，这与光谱的特征一致。该天体被确定为SDSS的17，500 z < 0.7类星体光谱的Karhunen-Loeve变换的极端异常值。由两个具有相似红移的类星体偶然叠加而成的光谱的概率估计为2 × 10 ^-7，因此在所研究的样本中，预期有0.003个这样的天体;然而，即使在这种情况下，低红移类星体的光谱仍然非常不寻常。
High resolution X-ray spectroscopy and imaging of Mrk573
本文详细分析了Seyfert 2星系Mrk 573的XMM-Newton RGS高分辨率X射线谱。这项分析是由钱德拉图像的研究，并比较光学（HST）和无线电（VLA）数据的补充。软X射线发射主要是由于气体光电离的活动星系核，从OVII和OVIII的辐射复合连续的检测，以及由OVII禁戒线的突出表明。这一结果证实了与自洽云光电离模型获得的最佳拟合。然而，为了再现FeXVII线，也需要碰撞激发的分量，约占15-26 A带总光度的1/3。一旦在Chandra ACIS数据中采用相同的模型，则需要另一个具有更高电离参数的光电离组分来考虑来自更高Z金属的发射。宽带ACIS光谱也证实了源的康普顿厚度性质。成像分析显示软X射线和[OIII]发射之间的密切形态对应。无线电发射看起来更紧凑，虽然明显与窄线区域对齐。软X射线发射的碰撞阶段可能是由于星暴，需要$\simeq5-9$ M $_\odot$ yr $^{-1}$的恒星形成率，但没有来自其他波长的这种活动的明确证据。另一方面，它可能与无线电喷射物有关，负责加热与流出物相互作用的等离子体，但热气体的估计压力远大于无线电喷流的压力，假设均分和合理的物理参数。
Unified Spectrospatial Forward Models: Spatially Continuous Maps of Weak Emission Lines in the Rosette Nebula with SDSS-V LVM
Monash University（莫纳什大学）；Flatiron Institute（平托研究所）；University of Washington（华盛顿大学）；Princeton University（普林斯顿大学）；The University of Texas at Austin（德克萨斯大学奥斯汀分校）；New Mexico State University（新墨西哥州立大学）；University of Toronto（多伦多大学）；Canadian Institute for Advanced Research（加拿大高级研究院）
