AI 中文总结
研究在 0.8<z<1.0 利用 PAC 方法测量类星体环境，联合建模相关函数，通过 N 体模拟等解释测量结果，得出高斯类星体占据峰值及相对卫星 hosting 参数，表明在固定晕吸积质量下类星体在中心晕和卫星子晕可能性相同，PAC 潜力大。
AI 中文摘要
类星体环境将超大质量黑洞的增长、活动星系核反馈和星系演化联系起来。小尺度类星体聚类探测单晕区域，并能检验类星体活动是否取决于中心 - 卫星状态。我们试图在 0.8<z<1.0 获得类星体环境的精确小尺度测量，并用于约束类星体 - 晕连接，特别是相同晕吸积质量的卫星子晕和中心晕 hosting 类星体的相对概率。我们将宇宙网周围的光度物体（PAC）方法应用于 DESI 数据发布 1 中的类星体和来自 DESI 遗产成像调查 DR9 的光度星系，测量类星体周围相邻星系的过剩投影表面密度，\(\bar{n}_{2}w_{\rm p}\)，在 0.1<r_{\rm p}/(h^{-1}\,\mathrm{Mpc})<15 范围内，恒星质量低至 \(M_{\ast}=10^{10.80}M_{\odot}\)。我们联合对过剩表面密度测量、类星体和亮红星系（LRG）自相关函数以及类星体 - LRG 交叉相关进行建模。我们使用 N 体模拟以及恒星到晕质量关系、明确的恒星质量不完整性模型和作为晕吸积质量函数的高斯类星体占据来解释这些测量。高斯类星体占据在 \(\log_{10}(M_{\rm acc}/h^{-1}M_{\odot})=12.88^{+0.02}_{-0.02}\) 处达到峰值，宽度 \(\sigma_{\rm q}=0.51^{+0.02}_{-0.01}\)，相对卫星 hosting 参数 \(B\)，定义为在固定晕吸积质量下卫星子晕 hosting 类星体的概率相对于中心晕的概率，为 \(B=1.01^{+0.03}_{-0.03}\)。在采用的模型框架内，在固定晕吸积质量下，类星体同样有可能位于中心晕和卫星子晕中。PAC 有很强的潜力提供类星体环境的精确小尺度测量。
英文摘要
Quasar environments connect the growth of supermassive black holes, active galactic nucleus feedback, and galaxy evolution. Small-scale quasar clustering probes the one-halo regime and can test whether quasar activity depends on central--satellite status. We seek to obtain precise small-scale measurements of quasar environments at $0.8<z<1.0$ and use them to constrain the quasar--halo connection, particularly the relative probability for satellite subhalos and central halos of the same halo accretion mass to host a quasar. We apply the Photometric Objects Around Cosmic Webs (PAC) method to DESI Data Release~1 quasars and photometric galaxies from the DESI Legacy Imaging Surveys DR9, measuring the excess projected surface density of neighbouring galaxies around quasars, $\bar{n}_{2}w_{\rm p}$, down to a stellar mass of $M_{\ast}=10^{10.80}M_{\odot}$ over $0.1<r_{\rm p}/(h^{-1}\,\mathrm{Mpc})<15$. we jointly model the excess surface-density measurements, the quasar and luminous red galaxy (LRG) autocorrelation functions, and the quasar--LRG cross-correlation. We interpret these measurements using an N-body simulation together with a stellar-to-halo mass relation, an explicit stellar-mass-incompleteness model, and a Gaussian quasar occupation as a function of halo accretion mass. The Gaussian quasar occupation peaks at $\log_{10}(M_{\rm acc}/h^{-1}M_{\odot})=12.88^{+0.02}_{-0.02}$ with width $σ_{\rm q}=0.51^{+0.02}_{-0.01}$, and the relative satellite-hosting parameter, $B$, defined as the quasar-hosting probability of a satellite subhalo relative to that of a central halo at fixed halo accretion mass, is $B=1.01^{+0.03}_{-0.03}$. Within the adopted model framework, quasars are consistent with being equally likely to reside in central halos and satellite subhalos at fixed halo accretion mass. PAC has strong potential to deliver precise small-scale measurements of quasar environments.
Comments10 pages, 10 figures, 1 table. Submitted to A&A
