贫金属星暴 Mrk 71 的星云 C IV 1550 成像：灾难性冷却的直接证据
Nebular C IV 1550 Imaging of the Metal-Poor Starburst Mrk 71: Direct Evidence of Catastrophic Cooling
AI总结：
本研究利用哈勃望远镜首次获得贫金属星暴 Mrk 71 的 C IV 星云成像，发现 Knot A 的反馈由灾难性辐射冷却主导，而 Knot B 表现为绝热超新星驱动反馈，为星暴机械反馈机制提供了直接观测证据。
摘要：
我们使用哈勃太空望远镜 ACS 相机，利用 F150LP 和 F165LP 滤镜，首次获得了 C IV 1548,1551 波段的空间分辨星云成像。对 NGC 2366 中本地星暴 Mrk 71 的观测显示，发射显然源自主导超星团（SSC）Knot A 周围内部空腔内。结合 He II 4686 成像和辅助的 STIS FUV 光谱，C IV 星云表面亮度的形态和强度以及 C IV / He II 比值图提供了直接证据，表明机械反馈可能由灾难性辐射冷却主导，这强烈破坏了绝热超气泡演化。所暗示的极端质量加载和星团风的低动能效率与风能预算合理一致，该预算可能因辐射压而增强。相反，Knot B SSC 位于一个轮廓清晰的超气泡内，伴随软 X 射线和 He II 1640 发射，这些是超新星驱动外流的绝热、能量驱动反馈的标志。正如该模型预期，该系统缺乏来自边缘增亮壳层的明显 C IV 证据，但观测可能不够深以确认其存在。我们还探测到一个发射 C IV 的小天体，可能是一个嵌入的致密 H II 区。其 C IV 发射可能表明存在超大质量恒星（> 100 M_sun）或强压力约束的恒星反馈。
英文摘要：
We use the Hubble Space Telescope ACS camera to obtain the first spatially resolved, nebular imaging in the light of C IV 1548,1551 by using the F150LP and F165LP filters. These observations of the local starburst Mrk 71 in NGC 2366 show emission apparently originating within the interior cavity around the dominant super star cluster (SSC), Knot A. Together with imaging in He II 4686 and supporting STIS FUV spectroscopy, the morphology and intensity of the C IV nebular surface brightness and the C IV / He II ratio map provide direct evidence that the mechanical feedback is likely dominated by catastrophic radiative cooling, which strongly disrupts adiabatic superbubble evolution. The implied extreme mass loading and low kinetic efficiency of the cluster wind are reasonably consistent with the wind energy budget, which is probably enhanced by radiation pressure. In contrast, the Knot B SSC lies within a well-defined superbubble with associated soft X-rays and He II 1640 emission, which are signatures of adiabatic, energy-driven feedback from a supernova-driven outflow. This system lacks clear evidence of C IV from the limb-brightened shell, as expected for this model, but the observations may not be deep enough to confirm its presence. We also detect a small C IV-emitting object that is likely an embedded compact H II region. Its C IV emission may indicate the presence of very massive stars (> 100 M_sun) or strongly pressure-confined stellar feedback.
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