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首页> 外文期刊>The Astrophysical journal >NEAR-INFRARED H_2 AND [Fe Ⅱ] IMAGING AND SPECTROSCOPY OF NEW JETS IN THE VELA MOLECULAR CLOUDS
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NEAR-INFRARED H_2 AND [Fe Ⅱ] IMAGING AND SPECTROSCOPY OF NEW JETS IN THE VELA MOLECULAR CLOUDS

机译：绒毛分子团中新芽的近红外H_2和[FeⅡ]成像和光谱学

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摘要

We present narrowband imaging in the 2.122 μm transition of H_2 and in the 1.644 μm transition of [Fe Ⅱ] of a sample of 12 protostellar candidates and three Herbig-Haro (HH) objects belonging to the Vela molecular ridge (VMR). Out of the 15 investigated fields, we detected H_2 emission in IRS 63, 17, 19, 21, and 8 (according to our catalog), while [Fe Ⅱ] was observed toward only one source (IRS 8), where a counterjet has been identified for the first time. H_2 and [Fe Ⅱ] images have been combined to trace the different shock conditions along this jet. In addition, a new pure molecular H_2 jet was discovered in IRS 17, which results in about 20 knots of emission extending up to 0.3 pc from the central driving source. IR spectroscopy (1.55-2.55 μm) at a resolution of ≈600 of the most prominent knots has revealed a large number of H_2 emission lines, which were used to evaluate both the extinction and the excitation temperature along the flow. The observed increase of the excitation temperature with the distance from the central source was interpreted as being due to a decrease of the flow velocity with time or, alternatively, to the fact that internal knots travel in a medium already put into motion by previous shock events. Comparisons with model predictions indicate nondissociative C-shocks as the most likely mechanism for line excitation. Finally, the presence of a common alignment of the detected flows with the Galactic plane indicates that the Galactic B field affects the star formation on large scales in VMR.
机译：我们在12个原恒星候选物和属于Vela分子脊（VMR）的三个Herbig-Haro（HH）对象的样本中，在H_2的2.122μm跃迁和[FeⅡ]的1.644μm跃迁中呈现窄带成像。在15个调查场中，我们在IRS 63、17、19、21和8中（根据我们的目录）检测到了H_2的排放，而[FeⅡ]仅向一个源（IRS 8）观察到，其中对冲具有首次被确定。将H_2和[FeⅡ]图像组合起来，以追踪沿该射流的不同冲击条件。此外，在IRS 17中发现了一种新的纯分子H_2射流，导致从中央驱动源发出的大约20节的排放物延伸到0.3 pc。红外光谱（1.55-2.55μm）分辨率约为最显着的结节的≈600，显示出大量的H_2发射谱线，这些谱线用于评估流的消光和激发温度。所观察到的激发温度随距中心源距离的增加而升高，被认为是由于流速随时间的推移而降低，或者是由于内部结在先前的冲击事件已经作用的介质中传播这一事实。 。与模型预测的比较表明，非解离性C震荡是最可能的线路激励机制。最后，检测到的流与银河平面的共同对准的存在表明，银河B场会影响VMR中大规模的恒星形成。

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