Title: The cosmic web of X-ray active galactic nuclei seen through the eROSITA Final Equatorial Depth Survey (eFEDS) Show Chinese title

Title: 通过eROSITA最终赤道深度调查（eFEDS）看到的X射线活动星系核的宇宙网

Abstract: Which galaxies in the general population turn into active galactic nuclei (AGNs) is a keystone of galaxy formation and evolution. Thanks to SRG/eROSITA's contiguous 140 square degree pilot survey field, we constructed a large, complete, and unbiased soft X-ray flux-limited ($F_X>6.5\times 10^{-15}$ erg s$^{-1}$ cm$^{-2}$) AGN sample at low redshift, $0.05<z<0.55$. Two summary statistics, the clustering using spectra from SDSS-V and galaxy-galaxy lensing with imaging from HSC, are measured and interpreted with halo occupation distribution and abundance matching models. Both models successfully account for the observations. We obtain an exceptionally complete view of the AGN halo occupation distribution. The population of AGNs is broadly distributed among halos with a mean mass of $3.9 _{- 2.4 }^{+ 2.0 }\times10^{12}M_\odot$. This corresponds to a large-scale halo bias of $b(z=0.34)= 0.99 ^{+0.08}_{-0.10}$. The central occupation has a large transition parameter, $\sigma_{\log_{10}(M)}=1.28\pm0.2$. The satellite occupation distribution is characterized by a shallow slope, $\alpha_{{\rm sat}}=0.73\pm0.38$. We find that AGNs in satellites are rare, with $f_{{\rm sat}}<20\%$. Most soft X-ray-selected AGNs are hosted by central galaxies in their dark matter halo. A weak correlation between soft X-ray luminosity and large-scale halo bias is confirmed (3.3$\sigma$). We discuss the implications of environmental-dependent AGN triggering. This study paves the way toward fully charting, in the coming decade, the coevolution of X-ray AGNs, their host galaxies, and dark matter halos by combining eROSITA with SDSS-V, 4MOST, DESI, LSST, and \textit{Euclid} data. Show Chinese abstract

Abstract: 哪些星系会成为活动星系核(AGNs)是星系形成和演化的一个关键问题。得益于SRG/eROSITA的连续140平方度试点调查区域，我们在低红移处构建了一个大、完整且无偏的软X射线通量限制($F_X>6.5\times 10^{-15}$ erg s$^{-1}$ cm$^{-2}$) AGN样本，$0.05<z<0.55$。两种总结统计量，使用SDSS-V的光谱进行的聚类和利用HSC成像进行的星系-星系引力透镜效应，被测量并用晕占有率分布和丰度匹配模型进行解释。这两种模型都成功地解释了观测结果。我们获得了对AGN晕占有率分布的极其完整的视图。AGN群体广泛分布在不同质量的晕中，平均质量为$3.9 _{- 2.4 }^{+ 2.0 }\times10^{12}M_\odot$。这对应于大尺度的晕偏差为$b(z=0.34)= 0.99 ^{+0.08}_{-0.10}$。中心占有率有一个大的过渡参数，$\sigma_{\log_{10}(M)}=1.28\pm0.2$。 卫星占用分布的特点是斜率较缓，$\alpha_{{\rm sat}}=0.73\pm0.38$。 我们发现卫星中的AGN很少，具有$f_{{\rm sat}}<20\%$。 大多数软X射线选择的AGN由其暗物质晕中的中心星系宿主。 确认了软X射线光度与大尺度晕偏置之间的弱相关性（3.3$\sigma$）。 我们讨论了环境依赖的AGN触发的影响。 这项研究为在接下来的十年中，通过结合eROSITA与SDSS-V、4MOST、DESI、LSST和\textit{欧几里得}数据，全面绘制X射线AGN、其宿主星系和暗物质晕的共同演化铺平了道路。