论文标题
使用$ z \ sim $ 0的大型光谱调查对流出的多相性质的观察性约束
Observational Constraints on the Multiphase Nature of Outflows Using Large Spectroscopic Surveys at $z\sim$0
论文作者
论文摘要
质量流出率和负载因子通常用于推断银河级流出的淬火潜力。但是，这些通常依赖于单个气相的观察结果，这些气相可能严重低估了总弹性气体质量。要解决这个问题，我们使用高质量的观察（$ \ geqslant $ 10 $^{10} $ m $ _ {\ odot} $），正常的星形星系，$ z \ sim $ 0，来自漫画，xcold gass，xccold gass，xgass，xgass and xgass and alfalfa unveys us a $ nad $ $ $ $ $ $ $ nad，and $ nad $ na将约束放在平均值，总质量流出率和负载因子上。我们发现中性和电离气体示踪剂中流出的检测，在分子或原子气排放的堆叠中没有检测。流出组件的建模揭示了$ | $ v $ _ {\ text {nad}} | $ = 131 km s $^{ - 1} $和$ | $ | $ v $ _ {\ text { $ \ dot {m} _ {\ text {nad}} $ = 7.55 m $ $ _ {\ odot} $ yr $^{ - 1} $和$ \ dot {M} _ {\ text {\ text { 分别。假设有200 km s $^{ - 1} $的分子/原子流出速度，我们得出了$ \ dot {m} _ {\ text {co}} <$ 19.43 m $ _ $ _ $ _ {\ odot} $ yr $ yr $ yr $^{ - yr $^{ - yr $^{ - yr $^{ - yr $^{-1} $ $ \ dot {m} _ {\ text {hi}} <$ 26.72 m $ _ {\ odot} $ yr $^{ - 1} $分别用于分子和原子气。结合检测和上限，我们发现平均总流出率为$ \ dot {m} _ {\ text {tox {tot}} \ Lessim $ 27 m $ $ _ {\ odot} $ yr $^{ - yr $^{ - 1} $，以及$η__ {\ fordect of togut poss posss posss posss possssssssssssssssssssssssssssssssssssssssssssssssssssssssssssssssssssssssssssssssssssss 6. \ 6. \ 6. \ 6. \ 6. \ 6. \ 6. \ 6. \ 66 $ \ Lessim $ 72％的总质量流出率，中性和电离气体分别贡献了$ \ sim $ 28％和$ <$ 1％。我们的结果表明，在一阶中，即使在没有AGN的情况下，即使在考虑所有气相，也可能会在正常星系中通过排出的反馈进行一定程度的淬火。
Mass outflow rates and loading factors are typically used to infer the quenching potential of galactic-scale outflows. However, these generally rely on observations of a single gas phase which can severely underestimate the total ejected gas mass. To address this, we use observations of high mass ($\geqslant$10$^{10}$ M$_{\odot}$), normal star-forming galaxies at $z\sim$0 from the MaNGA, xCOLD GASS, xGASS and ALFALFA surveys and a stacking of NaD, H$α$, CO(1-0) and HI 21cm tracers with the aim of placing constraints on an average, total mass outflow rate and loading factor. We find detections of outflows in both neutral and ionised gas tracers, with no detections in stacks of molecular or atomic gas emission. Modelling of the outflow components reveals velocities of $|$v$_{\text{NaD}}|$=131 km s$^{-1}$ and $|$v$_{\text{H}α}|$=439 km s$^{-1}$ and outflow rates of $\dot{M}_{\text{NaD}}$=7.55 M$_{\odot}$yr$^{-1}$ and $\dot{M}_{\text{H}α}$=0.10 M$_{\odot}$yr$^{-1}$ for neutral and ionised gas, respectively. Assuming a molecular/atomic outflow velocity of 200 km s$^{-1}$, we derive upper limits of $\dot{M}_{\text{CO}}<$19.43 M$_{\odot}$yr$^{-1}$ and $\dot{M}_{\text{HI}}<$26.72 M$_{\odot}$yr$^{-1}$ for the molecular and atomic gas, respectively. Combining the detections and upper limits, we find average total outflow rates of $\dot{M}_{\text{tot}}\lesssim$27 M$_{\odot}$yr$^{-1}$ and a loading factor of $η_{\text{tot}}\lesssim$6.39, with molecular gas likely contributing $\lesssim$72% of the total mass outflow rate, and neutral and ionised gas contributing $\sim$28% and $<$1%, respectively. Our results suggest that, to first order, a degree of quenching via ejective feedback could occur in normal galaxies when considering all gas phases, even in the absence of an AGN.
