SPITZER SPECTRAL LINE MAPPING OF PROTOSTELLAR OUTFLOWS. I. BASIC DATA AND OUTFLOW ENERGETICS
SPITZER SPECTRAL LINE MAPPING OF PROTOSTELLAR OUTFLOWS. I. BASIC DATA AND OUTFLOW ENERGETICS
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原恒星流出的斯皮策光谱线图。
DOI：
10.1088/0004-637x/706/1/170
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发表时间：
2009
期刊：
影响因子：
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通讯作者：
M. Kaufman
中科院分区：
文献类型：
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作者：
D. Neufeld;B. Nisini;T. Giannini;G. Melnick;E. Bergin;Yuan Yuan;S. Maret;V. Tolls;R. Guesten;M. Kaufman
我们报告了利用斯皮策太空望远镜的红外光谱仪（IRS）对BHR71、L1157、L1448、NGC 2071和VLA 1623分子区域的原恒星流出物进行光谱测绘观测的结果。这些观测覆盖了5.2-37 μm光谱区域，提供了分子氢的8条最低纯旋转谱线以及[S i] 25.25 μm和[Fe ii] 26.0 μm精细结构谱线的详细图谱。分子氢谱线被认为是由非解离激波加热的温暖分子气体辐射冷却的主要原因，它使流出的能量学得以阐明。在朝向这五个流出源的区域内，从8个最低纯旋转跃迁的总和推断出H2的总光度从0.02到0.75 L☉。相比之下，弱得多的[Fe ii] 26.0 μm细结构转变记录了更快的解离冲击；在这里，只有一小部分快速激波亮度以线辐射的形式出现，可以被斯皮策/IRS探测到。
We report the results of spectroscopic mapping observations carried out toward protostellar outflows in the BHR71, L1157, L1448, NGC 2071, and VLA 1623 molecular regions using the Infrared Spectrograph (IRS) of the Spitzer Space Telescope. These observations, covering the 5.2–37 μm spectral region, provide detailed maps of the eight lowest pure rotational lines of molecular hydrogen and of the [S i] 25.25 μm and [Fe ii] 26.0 μm fine-structure lines. The molecular hydrogen lines, believed to account for a large fraction of the radiative cooling from warm molecular gas that has been heated by a non-dissociative shock, allow the energetics of the outflows to be elucidated. Within the regions mapped toward these five outflow sources, total H2 luminosities ranging from 0.02 to 0.75 L☉ were inferred for the sum of the eight lowest pure rotational transitions. By contrast, the much weaker [Fe ii] 26.0 μm fine-structure transition traces faster, dissociative shocks; here, only a small fraction of the fast shock luminosity emerges as line radiation that can be detected with Spitzer/IRS.