论文标题
由Ly $α$森林吸收所追踪的银河特性的环境依赖性：星系种群的多样性
Environmental Dependence of Galactic Properties Traced by Ly$α$ Forest Absorption: Diversity among Galaxy Populations
论文作者
论文摘要
为了阐明银河系特性如何依赖于ly $α$森林所追踪的Galactic介质（IGM）环境，我们使用公开可用的3D IGM层析成像数据（Clamato）和宇宙场中的几个星系目录在观察中研究了IGM-Galaxy连接。我们以$ 570 $的星系为$ z $测量值的$ 570 $星系测量互相关功能（CCF），并检测IGM的相关性高达$ 50 $ $ $ $ h^{ - 1} $ commoving mpc。我们表明，恒星质量的星系为$ 10^9-10^{10} $ m $ _ \ odot $是总CCF信号的主要贡献者。我们还研究了几个星系种群的CCF：Ly $α$发射器（LAES），H $α$ emitters（HAES），[OIII]发射器（O3ES），Active Galactic nuclei（AGNS）和亚略列表（SMGS），我们检测到Agns和Smgs的最高信号（我们） $ h^{ - 1} $ mpc），但在laes中，小尺度（$ r <5 $ $ h^{ - 1} $ mpc）。我们发现它们生活在各种IGM环境中 - HAE以与连续式星系相似的方式追踪IGM，但是LAES和O3ES倾向于驻留在更高密度的区域。此外，Laes'CCF最多可容纳$ r \ sim3 $ $ h^{ - 1} $ MPC，表明它们倾向于避免最高密度的区域。对于AGN和SMG，CCF峰值为$ r = 5-6 $ $ h^{ - 1} $ MPC意味着它们往往位于局部较低的密度区域。我们怀疑这是由于AGN的IGM HI的光电离，即接近效应。
In order to shed light on how galactic properties depend on the intergalactic medium (IGM) environment traced by the Ly$α$ forest, we observationally investigate the IGM-galaxy connection using the publicly available 3D IGM tomography data (CLAMATO) and several galaxy catalogs in the COSMOS field. We measure the cross-correlation function (CCF) for $570$ galaxies with spec-$z$ measurements and detect a correlation with the IGM up to $50$ $h^{-1}$ comoving Mpc. We show that galaxies with stellar masses of $10^9-10^{10}$ M$_\odot$ are the dominant contributor to the total CCF signal. We also investigate CCFs for several galaxy populations: Ly$α$ emitters (LAEs), H$α$ emitters (HAEs), [OIII] emitters (O3Es), active galactic nuclei (AGNs), and submillimeter galaxies (SMGs), and we detect the highest signal in AGNs and SMGs at large scales ($r\geq5$ $h^{-1}$ Mpc), but in LAEs at small scales ($r<5$ $h^{-1}$ Mpc). We find that they live in various IGM environments -- HAEs trace the IGM in a similar manner to the continuum-selected galaxies, but LAEs and O3Es tend to reside in higher-density regions. Additionally, LAEs' CCF is flat up to $r\sim3$ $h^{-1}$ Mpc, indicating that they tend to avoid the highest-density regions. For AGNs and SMGs, the CCF peak at $r=5-6$ $h^{-1}$ Mpc implies that they tend to be in locally lower-density regions. We suspect that it is due to the photoionization of IGM HI by AGNs, i.e., the proximity effect.
