论文标题
观察星系相互作用对卷乳介质的影响
Observing the Effects of Galaxy Interactions on the Circumgalactic Medium
论文作者
论文摘要
我们继续对发射线通量的实证研究起源于凉爽（$ t \ sim10^4 $ k）气体，该气体填充了星系及其环境的光晕。具体而言，我们介绍了与一系列预计分离的星系对样本获得的结果，{\ bf $ 10 <{s_p/\ rm kpc} <200 $} <200 $}，质量比$ <$ <$ <$ <$ <$ 1：5，由5,443个SDSS在10至50 kpc的预测radii sds sds sds sds sds sds sds sds。我们发现h $α$排放的显着增强和低质量对的[n {\ small ii}] 6583排放（平均每个星系平均恒星质量，$ \ overline {。这种增强的H $α$排放几乎完全来自位于星系之间的视线，与短期，相互作用驱动的起源相一致。我们发现H $α$排放尚未增强，但是[n {\ small ii}] 6583发射高质量（$ \ overline {\ rm m} _*> 10^{10.4} {\ rm m m} _ \ odot $）。此外，我们发现发射线特性对星系对质量比的依赖性，使得质量比低于1：2.5的质量比具有增强的[N {\ Small II}] 6583，而质量比在1：2.5和1：5之间的质量比则增强了。在所有情况下，仅检测到与控制样本的偏离（$ s_p <$ 100 kpc）。将高架的[n {\ small ii}] 6583/h $α$比率归因于冲击，我们推断出冲击在确定较大较大且具有接近1：1的较大质量比的CGM属性方面发挥了作用。
We continue our empirical study of the emission line flux originating in the cool ($T\sim10^4$ K) gas that populates the halos of galaxies and their environments. Specifically, we present results obtained for a sample of galaxy pairs with a range of projected separations, {\bf $10 < {S_p/\rm kpc} < 200$}, and mass ratios $<$ 1:5, intersected by 5,443 SDSS lines of sight at projected radii of 10 to 50 kpc from either or both of the two galaxies. We find significant enhancement in H$α$ emission and a moderate enhancement in [N {\small II}]6583 emission for low mass pairs (mean stellar mass per galaxy, $\overline{\rm M}_*, <10^{10.4} {\rm M}_\odot$) relative to the results from a control sample. This enhanced H$α$ emission comes almost entirely from sight lines located between the galaxies, consistent with a short-term, interaction-driven origin for the enhancement. We find no enhancement in H$α$ emission, but significant enhancement in [N {\small II}]6583 emission for high mass ($\overline{\rm M}_* >10^{10.4}{\rm M}_\odot$) pairs. Furthermore, we find a dependence of the emission line properties on the galaxy pair mass ratio such that those with a mass ratio below 1:2.5 have enhanced [N {\small II}]6583 and those with a mass ratio between 1:2.5 and 1:5 do not. In all cases, departures from the control sample are only detected for close pairs ($S_p <$ 100 kpc). Attributing an elevated [N {\small II}]6583/H$α$ ratio to shocks, we infer that shocks play a role in determining the CGM properties for close pairs that are among the more massive and have mass ratios closer to 1:1.
