Title: Multi-phase gas interactions on subarcsec scales in the shocked IGM of Stephan's Quintet with JWST and ALMA Show Chinese title

Title: 斯蒂芬五重星系激震星际介质中亚角秒尺度的多相气体相互作用与詹姆斯·韦布空间望远镜和阿塔卡马大型毫米波天线阵的观测

Abstract: We combine JWST and HST imaging with ALMA~CO(2-1) spectroscopy to study the highly turbulent multi-phase intergalactic medium (IGM) in Stephan's Quintet on 25-150 pc scales. Previous Spitzer observations revealed luminous H$_2$ line cooling across a 45 kpc-long filament, created by a giant shock-wave, following the collision with an intruder galaxy NGC~7318b. We demonstrate that the MIRI/F1000W/F770W filters are dominated by 0-0~S(3)~H$_2$ and a combination of PAH and 0-0~S(5)~H$_2$ emission. They reveal the dissipation of kinetic energy as massive clouds experience collisions, interactions and likely destruction/re-cycling within different phases of the IGM. In one kpc-scaled structure, warm H$_2$ formed a triangular-shaped head and tail of compressed and stripped gas behind a narrow shell of cold H$_2$. In another region, two cold molecular clumps with very different velocities are connected by an arrow-shaped stream of warm, probably shocked, H$_2$ suggesting a cloud-cloud collision is occurring. In both regions, a high warm-to-cold molecular gas fraction indicates that the cold clouds are being disrupted and converted into warm gas. We also map gas associated with an apparently forming dwarf galaxy. We suggest that the primary mechanism for exciting strong mid-IR H$_2$ lines throughout Stephan's Quintet is through a fog of warm gas created by the shattering of denser cold molecular clouds and mixing/recycling in the post-shocked gas. A full picture of the diverse kinematics and excitation of the warm H$_2$ will require future JWST mid-IR spectroscopy. The current observations reveal the rich variety of ways that different gas phases can interact with one another. Show Chinese abstract

Abstract: 我们结合JWST和HST成像与ALMA~CO(2-1)光谱学研究Stephan's Quintet中高度湍流的多相星系际介质（IGM），在25-150 pc尺度上。 之前的Spitzer观测揭示了在45 kpc长的丝状结构中，由与入侵星系NGC~7318b碰撞产生的巨大激波形成的明亮H$_2$线冷却。 我们证明MIRI/F1000W/F770W滤镜主要由0-0~S(3)~H$_2$和PAH以及0-0~S(5)~H$_2$发射组成。 它们揭示了大云团经历碰撞、相互作用以及可能在IGM不同相中的破坏/再循环过程中动能的耗散。 在一个kpc尺度的结构中，温暖的H$_2$形成了一个三角形的头部和尾部，压缩和剥离的气体位于冷H$_2$的狭窄壳层之后。 在另一个区域，两个速度截然不同的冷分子云团通过箭头形状的温暖、可能是被冲击的H$_2$流连接，表明正在发生云-云碰撞。 在这两个区域，高比例的温暖分子气体与冷分子气体表明冷云正在被破坏并转化为温暖气体。 我们还绘制了一个似乎正在形成的矮星系相关的气体。 我们认为，激发Stephan's Quintet中强中红外H$_2$线的主要机制是通过致密冷分子云的破碎形成的温暖气体雾，以及冲击后气体的混合/再循环。 温暖的H$_2$的多样运动学和激发的完整图景将需要未来的JWST中红外光谱学。 当前的观测揭示了不同气体相之间相互作用的丰富多样性。