解密M16中HH 216与柱体IV的隐藏结构：来自JWST与HST的结果
Deciphering the Hidden Structures of HH 216 and Pillar IV in M16: Results from JWST and HST
AI总结：
本文利用JWST和HST高分辨率观测鹰状星云柱体IV及其外流激波HH 216，揭示了原恒星的孤立性、电离结构、新H₂结和喷流，并结合CO谱线证据提出云-云碰撞可能触发了该区域的恒星形成。
摘要：
为探究恒星形成过程，我们对鹰状星云（M16）中的柱体IV和电离结HH 216进行了观测研究。已知柱体IV内存在一颗驱动双极外流的I类原恒星。该外流产生了弓形激波HH 216，它与红移外流瓣相关联。詹姆斯·韦布空间望远镜的近红外和中红外图像（分辨率约0.07角秒至0.7角秒）显示该原恒星是一个单一、孤立的天体（尺度小于1000 AU）。柱体IV的外边界由3.3 μm多环芳烃（PAH）发射描绘。HH 216通过4.05 μm Brα和射电连续谱发射被追踪到，但在4.693 μm H₂发射中未被探测到。HH 216似乎同时与热和非热射电发射相关。高分辨率图像揭示了HH 216中纠缠的电离结构（尺度小于3000 AU），这些结构似乎位于终止激波处。在4.693 μm H₂发射中探测到新的结，主要分布在柱体IV的北侧。这一结果支持了此前提出的HH 216供能源中存在间歇性吸积的观点。在驱动源的南侧发现了一段电离喷流（延伸约0.16 pc）。利用¹²CO(J = 1-0)、¹²CO(J = 3-2)和¹³CO(J = 1-0)发射，研究了指向柱体IV的云-云碰撞（或相互作用云）的观测标志。总体而言，我们的结果表明，约23和26 km s⁻¹处分子云成分的相互作用可能影响了柱体IV中的恒星形成活动。
英文摘要：
To probe the star formation process, we present an observational investigation of the Pillar IV and an ionized knot HH 216 in the Eagle Nebula (M16). Pillar IV is known to host a Class I protostar that drives a bipolar outflow. The outflow has produced the bow shock, HH 216, which is associated with the red-shifted outflow lobe. The James Webb Space Telescope's near- and mid-infrared images (resolution $\sim$0.07 arcsec - 0.7 arcsec) reveal the protostar as a single, isolated object (below 1000 AU). The outer boundary of Pillar IV is depicted with the 3.3 $μ$m Polycyclic aromatic hydrocarbon (PAH) emission. HH 216 is traced with the 4.05 $μ$m Br$α$ and the radio continuum emission, however it is undetected with 4.693 $μ$m H$_{2}$ emission. HH 216 seems to be associated with both thermal and non-thermal radio emissions. High-resolution images reveal entangled ionized structures (below 3000 AU) of HH 216, which appear to be located toward termination shocks. New knots in 4.693 $μ$m H$_{2}$ emission are detected, and are mainly found on Pillar IV's northern side. This particular result supports the previously proposed episodic accretion in the powering source of HH 216. One part of the ionized jet (extent $\sim$0.16 pc) is discovered on the southern side of the driving source. Using the $^{12}$CO($J$ = 1-0), $^{12}$CO($J$ = 3-2), and $^{13}$CO($J$ = 1-0) emission, observational signposts of Cloud-Cloud Collision (or interacting clouds) toward Pillar IV are investigated. Overall, our results suggest that the interaction of molecular cloud components around 23 and 26 km s$^{-1}$ might have influenced star formation activity in Pillar IV.
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