标题： “活动星系核参考调查”（CARS）：亚毫米波与光学活动星系核诊断图的比较 显示英文标题

标题： The Close AGN Reference Survey (CARS): A comparison between sub-mm and optical AGN diagnostic diagrams

摘要： $L_{\rm IR}-L_{\rm HCN}$关系表明致密气体与恒星形成之间存在紧密联系。 我们使用近距离活动星系核参考调查（CARS）的数据来研究宿主活动星系核（AGN）星系中的致密气体-恒星形成关系，以及将致密气体作为活动星系核（AGN）诊断工具的使用。 我们的样本包含五个类型1（无遮挡）活动星系核，它们被阿塔卡马大型毫米/亚毫米阵列（ALMA）观测，目的是检测HCN(4-3)、HCO$^+$(4-3)和CS(7-6)。 我们在5个目标中的3个中检测到了该分析所需的致密气体发射。 我们发现，尽管活动星系核可能对这些源的线流量产生影响，它们仍然遵循$L_{\rm IR}-L_{\rm HCN}$关系。 然后我们继续测试关于HCN/HCO+和HCN/CS线比率可以用作在亚毫米HCN图中分类活动星系核的工具的说法。 我们使用来自多单元光谱探测器（MUSE）的可用CARS数据生成经典电离发射线比率诊断（所谓的BPT图）。 然后我们将BPT分类与使用致密气体示踪剂进行的亚毫米分类进行比较。 在可以完成分析的地方，我们发现光学和亚毫米分类的气体激发机制之间有总体的一致性。 这表明活动星系核可以同时对温暖电离介质中的低密度气体和分子云中的高密度气体的激发做出贡献，可能是通过X射线、宇宙射线或冲击加热机制。 显示英文摘要

摘要： The $L_{\rm IR}-L_{\rm HCN}$ relation suggests that there is a tight connection between dense gas and star formation. We use data from the Close AGN Reference Survey (CARS) to investigate the dense gas - star formation relation in AGN hosting galaxies, and the use of dense gas as an active galactic nuclei (AGN) diagnostic. Our sample contains five Type-1 (unobscured) AGN that were observed with the Atacama Large Millimeter/submillimeter Array (ALMA) with the aim to detect HCN(4-3), HCO$^+$(4-3) and CS(7-6). We detect the dense gas emission required for this analysis in 3 of the 5 targets. We find that despite the potential impact from the AGN on the line fluxes of these sources, they still follow the $L_{\rm IR}-L_{\rm HCN}$ relation. We then go on to test claims that the HCN/HCO+ and HCN/CS line ratios can be used as a tool to classify AGN in the sub-mm HCN diagram. We produce the classic ionised emission-line ratio diagnostics (the so-called BPT diagrams), using available CARS data from the Multi Unit Spectroscopic Explorer (MUSE). We then compare the BPT classification with the sub-mm classification made using the dense gas tracers. Where it was possible to complete the analysis we find general agreement between optical and sub-mm classified gas excitation mechanisms. This suggests that AGN can contribute to the excitation of both the low density gas in the warm ionised medium and the high density gas in molecular clouds simultaneously, perhaps through X-ray, cosmic ray or shock heating mechanisms.