AI 中文总结
该研究利用MaNGA巡天数据，通过空间分辨光谱研究附近恒星形成星系中电离气体外流性质。发现外流电子密度等与发射区域及星系整体性质有关，给出相关相关性及密度对比，为反馈模型提供新约束，强调相关观测和诊断需求。
AI 中文摘要
我们利用阿帕奇点天文台附近星系绘图（MaNGA）巡天的最终数据发布，研究了附近恒星形成星系中电离气体外流的性质。通过空间分辨光谱，我们在符合物理条件的外流孔径内寻找电离外流的特征。我们在115个星系中发现了显著证据，表明存在额外的宽Hα、[N II]λλ6550,6584和[S II]λλ6718,6733发射线成分，约占恒星形成的MaNGA星系的3%。我们的分析表明，外流电子密度（$n_{\text{e, out}}$）、质量损失率和质量加载因子与发射区域的性质和星系整体性质都有关。特别是，我们发现$n_{\text{e, out}}$与封闭（-3.4$\sigma$）和整体（-2.4$\sigma$）恒星形成率表面密度之间存在相关性，即表面密度较低的区域往往驱动密度更高的电离气体外流。我们利用单个$n_{\text{e, out}}$估计值发现质量加载因子与星系性质之间有几个>2$\sigma$的相关性，而当$n_{\text{e, out}}$固定为样本的中值时，更显著的相关性（>3$\sigma$）才会出现。结合文献中z~1.9范围内的$n_{\text{e, out}}$测量值，$n_{\text{e, out}}$没有显著的红移演化，这与星际介质（ISM）气体电子密度观察到的强烈演化形成对比。在z~0时，电离外流的密度比ISM高约8.5倍，在z~1.9时约高1.6倍。这些结果为反馈模型提供了新的约束，并强调了需要高分辨率积分场单元观测和模拟的合成线诊断来研究外流性质与局部ISM条件之间的联系。
英文摘要
We investigate the properties of ionized gas outflows in nearby star-forming galaxies from the final Data Release of the Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) Survey. Using spatially resolved spectroscopy, we search for signatures of ionized outflows within physically motivated outflow apertures. We find significant evidence for additional broad H$α$, [N II]$λλ$6550,6584, and [S II]$λλ$6718,6733 emission-line components in 115 galaxies, $\sim$3% of star-forming MaNGA galaxies. Our analysis suggests that outflow electron densities ($n_{\text{e, out}}$), mass-loss rates, and mass-loading factors are related to both the properties of the regions that launch and global galactic properties. In particular, we find correlations between $n_{\text{e, out}}$ and both the enclosed ($-$3.4$σ$) and global ($-$2.4$σ$) star-formation-rate surface densities, such that lower surface density regions tend to drive denser ionized gas outflows. We find several $>$$2σ$ correlations between the mass-loading factor and galactic properties using individual $n_{\text{e, out}}$ estimates, while more significant correlations ($>$$3σ$) only emerge when $n_{\text{e, out}}$ is fixed to the median value of the sample. Combining with literature $n_{\text{e, out}}$ measurements out to $z \sim 1.9$, $n_{\text{e, out}}$ exhibits no significant redshift evolution, in contrast to the strong evolution observed for gas electron densities of the interstellar medium (ISM). Ionized outflows remain denser than the ISM by a factor of $\sim$8.5 at $z \sim 0$ and $\sim$1.6 at $z \sim 1.9$. These results provide new constraints for feedback models and highlight the need for high-resolution IFU observations and synthetic line diagnostics from simulations to investigate the connection between outflow properties and local ISM conditions.
Comments27 pages, 9 figures, 4 tables. Accepted to ApJ
