论文标题
AGN-GALAXY-HALO连接：AGN宿主光环质量到Z = 2.5的分布
The AGN-galaxy-halo connection: The distribution of AGN host halo masses to z=2.5
论文作者
论文摘要
基于观察到的活性银河核（AGN）样品的聚类测量值的聚类测量，AGN驻留在大部分宇宙时间中的类似质量宿主暗物质光环中，log $ m/m_ \ odot $ 〜12.5-13.0至z〜2.5。我们表明，这部分是由于星系中AGN的分数随着恒星质量的增加而增加，并加上加剧这种趋势的AGN观察性选择效应。在这里，我们使用AGN特异性积分速率分布函数分别根据恒星质量和红移的函数分别与最新的Galaxy-Halo连接模型相结合，以确定AGN的母体和下halo质量分布函数与各种观察限制。我们发现，尽管AGN的中值（子）光环质量，$ \ of of10^{12} m_ \ odot $，均具有亮度，特定的积聚率和红移，但完整的光晕质量分布函数却很广泛，跨越了几个数量级。我们表明，基于观察到的AGN聚类幅度基于观察到的典型的暗物质光环质量来推断典型的暗物质光环质量的方法可能导致有偏见，系统较高的宿主光晕质量。虽然AGN卫星馏分随着母晕质量的增加而上升，但我们发现中央星系通常不是AGN。我们的结果阐明了在宇宙时间内AGN宿主光晕的明显均匀性的物理原因，并强调了解释观察性AGN聚类结果时考虑AGN选择偏见的重要性。我们进一步表明，AGN聚类最容易根据与星系样品的相对偏见来解释，而不是仅凭绝对偏差测量。
It is widely reported, based on clustering measurements of observed active galactic nuclei (AGN) samples, that AGN reside in similar mass host dark matter halos across the bulk of cosmic time, with log $M/M_\odot$~12.5-13.0 to z~2.5. We show that this is due in part to the AGN fraction in galaxies rising with increasing stellar mass, combined with AGN observational selection effects that exacerbate this trend. Here, we use AGN specific accretion rate distribution functions determined as a function of stellar mass and redshift for star-forming and quiescent galaxies separately, combined with the latest galaxy-halo connection models, to determine the parent and sub-halo mass distribution function of AGN to various observational limits. We find that while the median (sub-)halo mass of AGN, $\approx10^{12}M_\odot$, is fairly constant with luminosity, specific accretion rate, and redshift, the full halo mass distribution function is broad, spanning several orders of magnitude. We show that widely used methods to infer a typical dark matter halo mass based on an observed AGN clustering amplitude can result in biased, systematically high host halo masses. While the AGN satellite fraction rises with increasing parent halo mass, we find that the central galaxy is often not an AGN. Our results elucidate the physical causes for the apparent uniformity of AGN host halos across cosmic time and underscore the importance of accounting for AGN selection biases when interpreting observational AGN clustering results. We further show that AGN clustering is most easily interpreted in terms of the relative bias to galaxy samples, not from absolute bias measurements alone.
