IRAS 04239+2436（HH 300）的幕式旋进巨分子外流
The Episodic, Precessing Giant Molecular Outflow from IRAS 04239+2436 (HH 300)
摘要：
我们提出了第一套详细的分子线地图的区域与巨大的赫比格-哈罗流HH 300，从年轻的恒星IRAS 04239+2436。我们的研究结果表明，HH 300气流的红色叶在其宿主乌云的显著体积上沉积了相当数量的动量和动能。这使得HH 300成为其母云发展和命运的关键参与者。HH 300的红移分子流出叶长1.1 pc，宽0.3 pc，具有非常密集的结构。在流出的密度，速度和动量分布表明，所观察到的团块产生的环境气体的迅速夹带。弓形激波形状的结构与团块，我们假设的冲击是由不同的质量喷射事件。从IRAS 04239+2436到这些团块的线在天空平面上有不同的方向，我们得出结论，HH 300是一个旋进和幕式外流。观测结果包括12 CO（2-1）线上的红色瓣图，光束尺寸为27“，以及12 CO（1-0）和13 CO（1-0）线上流出区的更扩展图，光束尺寸分别为45”和47“。我们得到一个陡峭的幂律质谱HH 300，我们认为这是最好的解释流出质量运动学的演变。此外，我们的13 CO观测结果表明，HH 300流已经能够重新分配（在空间和速度）相当数量的周围中密度气体。
英文摘要：
We present the first set of detailed molecular line maps of the region associated with the giant Herbig-Haro flow HH 300, from the young star IRAS 04239+2436. Our results indicate that the red lobe of the HH 300 flow is depositing a fair amount of momentum and kinetic energy over a notable volume of its host dark cloud. This makes HH 300 a key player in the evolution and fate of its parent cloud. The redshifted molecular outflow lobe of HH 300 is 1.1 pc long and 0.3 pc wide, and has a very clumpy structure. The density, velocity, and momentum distributions in the outflow indicate that the observed clumps arise from the prompt entrainment of ambient gas. Bow shock-shaped structures are associated with the clumps, and we hypothesize that the shocks are produced by different mass ejection episodes. Lines drawn from IRAS 04239+2436 to each of these clumps have different orientations on the plane of the sky, and we conclude that HH 300 is a precessing and episodic outflow. The observations include a map of the red lobe in the 12CO(2-1) line, with a beam size of 27'', and more extended maps of the outflow region in the 12CO(1-0) and 13CO(1-0) lines, with 45'' and 47'' beam sizes, respectively. We obtain a steep power-law mass spectrum for HH 300, which we believe is best explained by the evolution of the outflow mass kinematics. In addition, our 13CO observations show that the HH 300 flow has been able to redistribute (in space and velocity) considerable amounts of its surrounding medium-density gas.
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