宇宙网周围的测光天体（PAC）。VI. 类星体的高卫星占比
Photometric Objects Around Cosmic Webs (PAC). VI. High Satellite Fraction of Quasars
AI总结：
本研究利用PAC方法结合SDSS-IV eBOSS与DESI遗产巡天数据，测量红移0.8-1.0的类星体周围近邻星系面密度超量，通过子晕丰度匹配建模得出类星体的卫星占比达0.29，揭示子晕与同质量主晕承载类星体的概率相近、大尺度环境对类星体活动影响可忽略。
摘要：
Xu等人（2022b）提出的Photometric objects Around Cosmic webs（PAC，宇宙网周围测光天体）方法具有充分利用光谱巡天与更深层测光巡天数据的优势。借助PAC方法的特性，结合Sloan Digital Sky Survey IV（SDSS-IV，斯隆数字巡天IV）extended Baryon Oscillation Spectroscopic Survey（eBOSS，扩展重子振荡光谱巡天）以及Dark Energy Spectroscopic Instrument（DESI，暗能量光谱仪）Legacy Imaging Surveys（遗产成像巡天）的数据，我们可以测量红移0.8<z_s<1.0的类星体周围、恒星质量低至10^10.80 M⊙的近邻星系的面密度超量$\bar{n}_2w_{\rm{p}}$。研究发现，$\bar{n}_2w_{\rm{p}}$通常随间距减小而急剧上升。利用子晕丰度匹配方法，我们可以在小尺度和大尺度上准确拟合$\bar{n}_2w_{\rm{p}}$的分布。结果表明，$\bar{n}_2w_{\rm{p}}$向类星体方向的陡峭上升要求大质量晕中相当比例的类星体为卫星天体，该占比$f_{\rm{sate}}=0.29_{-0.06}^{+0.05}$，且这一占比测量结果对我们的建模假设不敏感。如此高的卫星占比说明，对于相同的（下落）晕质量，子晕承载类星体的概率与主晕几乎一致，且大尺度环境对类星体活动的影响可忽略不计。我们还发现，尽管卫星占比很高，但由于类星体的稀疏性，平均每个大质量晕承载的卫星类星体数量不超过1个。
英文摘要：
The Photometric objects Around Cosmic webs (PAC) approach developed in Xu et al. (2022b) has the advantage of making full use of spectroscopic and deeper photometric surveys. With the merits of PAC, the excess surface density $\bar{n}_2w_{\rm{p}}$ of neighboring galaxies can be measured down to stellar mass $10^{10.80}\,M_{\odot}$ around quasars at redshift $0.8<z_{\rm{s}}<1.0$, with the data from the Sloan Digital Sky Survey IV (SDSS-IV) extended Baryon Oscillation Spectroscopic Survey (eBOSS) and the Dark Energy Spectroscopic Instrument (DESI) Legacy Imaging Surveys. We find that $\bar{n}_2w_{\rm{p}}$ generally increases quite steeply with the decrease of the separation. Using subhalo abundance matching method, we can accurately model the $\bar{n}_2w_{\rm{p}}$ both on small and large scales. We show that the steep increase of the $\bar{n}_2w_{\rm{p}}$ towards the quasars requires that a large fraction $f_{\mathrm{sate}}=0.29_{-0.06}^{+0.05}$ of quasars should be satellites in massive halos, and find that this fraction measurement is insensitive to the assumptions of our modeling. This high satellite fraction indicates that the subhalos have nearly the same probability to host quasars as the halos for the same (infall) halo mass, and the large scale environment has negligible effect on the quasar activity. We show that even with this high satellite fraction, each massive halo on average does not host more than one satellite quasar due to the sparsity of quasars.
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