论文标题
索非亚反馈遗产调查：双相HII区域RCW 36
The SOFIA FEEDBACK Legacy Survey: Dynamics and mass ejection in the bipolar HII region RCW 36
论文作者
论文摘要
我们提出[CII] 158 $μ$ m和[OI] 63 $ $ m m对vela c分子云中双极HII区域RCW 36观察，在Sofia Legacy Project反馈中获得，该反馈与Apex $^{12/13} $ CO（3-2）$ CO（3-2）和Chandra x-ray（0.5--7-7-7-7-7-7-7-7-7-7）这表明，形成双极星云的腰部的分子环的速度为1-1.9 km s $^{ - 1} $。我们还观察到环宽的增加，表明湍流是由恒星反馈的能量注入驱动的。双极腔的蓝移膨胀[CII]壳为5.2 $ \ pm $ 0.5 $ \ pm $ \ $ 0.5 km s $ s $^{ - 1} $（统计和系统的不确定性），这表明从密集气体中扩张不均匀，而观察到的双极相对阶段可能会相对短（$ 0.2 Myr）。 X射线观测结果显示，弥漫性发射，可追踪RCW 36和RCW 36周围恒星风创建的热等离子体。在RCW 36中，至少50％的恒星风能中缺少恒星风能。这可能是由于泄漏所致，这可能清除了在双极RCW 36区域周围更大的腔。最后，[CII]中的腔体托管高速翼，表示相对较高的质量排放率（$ \ sim $ 5 $ \ times $ 10 $^{ - 4} $ M $ _ {\ odot} $ yr $^{ - 1} $）。这可能是由恒星风和/或辐射压力驱动的，但仍然很难约束。这种局部质量喷射可以消除RCW 36 in 1-2 MYR的1 pc中的所有质量，并且对Vela C云中环境气体的大规模清除表明，恒星反馈在抑制恒星形成效率（SFE）中起着重要作用。
We present [CII] 158 $μ$m and [OI] 63 $μ$m observations of the bipolar HII region RCW 36 in the Vela C molecular cloud, obtained within the SOFIA legacy project FEEDBACK, which is complemented with APEX $^{12/13}$CO(3-2) and Chandra X-ray (0.5-7 keV) data. This shows that the molecular ring, forming the waist of the bipolar nebula, expands with a velocity of 1 - 1.9 km s$^{-1}$. We also observe an increased linewidth in the ring indicating that turbulence is driven by energy injection from the stellar feedback. The bipolar cavity hosts blue-shifted expanding [CII] shells at 5.2$\pm$0.5$\pm$0.5 km s$^{-1}$ (statistical and systematic uncertainty) which indicates that expansion out of the dense gas happens non-uniformly and that the observed bipolar phase might be relatively short ($\sim$0.2 Myr). The X-ray observations show diffuse emission that traces a hot plasma, created by stellar winds, in and around RCW 36. At least 50 \% of the stellar wind energy is missing in RCW 36. This is likely due to leakage which is clearing even larger cavities around the bipolar RCW 36 region. Lastly, the cavities host high-velocity wings in [CII] which indicates relatively high mass ejection rates ($\sim$5$\times$10$^{-4}$ M$_{\odot}$ yr$^{-1}$). This could be driven by stellar winds and/or radiation pressure, but remains difficult to constrain. This local mass ejection, which can remove all mass within 1 pc of RCW 36 in 1-2 Myr, and the large-scale clearing of ambient gas in the Vela C cloud indicates that stellar feedback plays a significant role in suppressing the star formation efficiency (SFE).
