论文标题
关于漫画主要合并对的HI内容
On the HI Content of MaNGA Major Merger Pairs
论文作者
论文摘要
HI内容在星系相互作用中的作用仍在争论中。为了在不同的合并阶段研究星系对的HI含量，我们从SDSS-IV漫画IFU调查中编辑了66个主要合并星系对和433个对照星系的样本。在这项研究中，我们采用运动学不对称性作为一种新的有效指标来描述星系对的合并阶段。借助Hi-Manga调查的档案数据以及来自五百米的光圈射线射电望远镜（FAST）的新观察结果，我们研究了HI气体分数的差异（$ f _ {\ text {hi}} $），星形形成率（SFR），hi star构建效率（$ \ rm sefecte（$ \ rm rm semeple）我们的结果表明，相对于孤立的星系，大合并对的HI气体比例平均减少了$ \ sim 15 \％$，这意味着在星系相互作用期间，轻度的HI耗竭。与孤立的星系相比，预足够的配对星系具有相似的$ f _ {\ text {hi}} $，sfr和$ \ rm sfe _ {\ text {hi}} $，而周围通道期间的成对却弱减少了$ f _ {$ f _ {$ fext { sfr（$ 0.42 \ pm0.11 $ dex）和$ \ rm sfe _ {\ text {hi}} $（$ 0.48 \ pm0.12 $ dex）。接近启示剂时，配对的星系显示出略降低$ f _ {\ text {hi}} $（$ -0.05 \ pm0.04 $ dex），可比较的sfr（$ 0.04 \ pm0.06 $ dex）和$ \ sfe _ sfe _ {我们提出，略有检测到的HI耗竭可能源于气体消耗，从而加油了Galaxy Pairs的增强$ \ rm H_2 $储层。此外，新的快速观察还揭示了一个HI吸收器（$ n _ {\ text {hi}} \ sim 4.7 \ times 10^{21} \ text {cm}^{ - 2} $），这可能暗示气体输入和触发AGN活动的触发。
The role of HI content in galaxy interactions is still under debate. To study the HI content of galaxy pairs at different merging stages, we compile a sample of 66 major-merger galaxy pairs and 433 control galaxies from the SDSS-IV MaNGA IFU survey. In this study, we adopt kinematic asymmetry as a new effective indicator to describe the merging stage of galaxy pairs. With archival data from the HI-MaNGA survey and new observations from the Five-hundred-meter Aperture Spherical Radio Telescope (FAST), we investigate the differences in HI gas fraction ($f_{\text{HI}}$), star formation rate (SFR), and HI star formation efficiency ($\rm SFE_{\text{HI}}$) between the pair and control samples. Our results suggest that the HI gas fraction of major-merger pairs on average is marginally decreased by $\sim 15\%$ relative to isolated galaxies, implying mild HI depletion during galaxy interactions. Compared to isolated galaxies, pre-passage paired galaxies have similar $f_{\text{HI}}$, SFR and $\rm SFE_{\text{HI}}$, while pairs during pericentric passage have weakly decreased $f_{\text{HI}}$ ($-0.10\pm0.05$ dex), significantly enhanced SFR ($0.42\pm0.11$ dex) and $\rm SFE_{\text{HI}}$ ($0.48\pm0.12$ dex). When approaching the apocenter, paired galaxies show marginally decreased $f_{\text{HI}}$ ($-0.05\pm0.04$ dex), comparable SFR ($0.04\pm0.06$ dex) and $\rm SFE_{\text{HI}}$ ($0.08\pm0.08$ dex). We propose the marginally detected HI depletion may originate from the gas consumption in fuelling the enhanced $\rm H_2$ reservoir of galaxy pairs. In addition, new FAST observations also reveal an HI absorber ($N_{\text{HI}}\sim 4.7 \times 10^{21} \text{ cm}^{-2}$), which may suggest gas infalling and the triggering of AGN activity.
