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首页> 外文期刊>PASJ: Publications of the Astronomical Society of Japan >N2H+ and HC3N observations of the Orion A cloud
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N2H+ and HC3N observations of the Orion A cloud

机译：猎户座A云的N2H +和HC3N观测

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The "integral-shaped filament" of the Orion A giant molecular cloud was mapped in N2H+, and its nor-them end, the OMC-2/3 region, was also observed in HC3N and CCS. The results were compared with maps of other molecular lines and the dust continuum emission. The N2H+ distribution is similar to the dust continuum distribution, except for the central part of the Orion Nebula. The distribution of (HCO+)-C-13 holds a resemblance to that of the dust continuum, but the N2H+ distribution looks more similar to the dust continuum distribution. The N-bearing molecules, N2H+ and NH3, seem to be more intense in OMC-2, compared with the, (HCO+)-C-13 and CS distribution. This suggests that OMC-2 has a higher abundance of N-bearing molecules, or a higher filling factor of the quiescent gas. We identified 34 cloud cores from N2H+ data. Over the Orion Nebula region, the N2H+ linewidth is large (1.1-2.1 km s(-1)). In the OMC-2/3 region, it becomes moderate (0.5-1.3 km s(-1)), and it is smaller (0.3-1.1 km s(-1)) in the south of the Orion Nebula. On the other hand, the gas kinetic temperature of the quiescent cores observed in N2H+ is rather constant (similar to 20 K) over the integral-shaped filament. We detected no CCS emission in the OMC-2/3 region. In general, the N2H+ and HC3N distribution is quite similar in the OMC-2/3 region, but we observed a displacement between N2H+ and HC3N over a 2' scale in OMC-3, which has a chain of Class 0-I protostars (candidates).
机译：Orion A巨型分子云的“整体形细丝”被绘制在N2H +中，并且在HC3N和CCS中也观察到其正态末端OMC-2 / 3区域。将结果与其他分子线图和粉尘连续体发射图进行了比较。 N2H +分布类似于粉尘连续体分布，除了猎户星云的中心部分。 （HCO +）-C-13的分布与粉尘连续体的分布相似，但N2H +分布看起来更类似于粉尘连续体的分布。与（HCO +）-C-13和CS分布相比，OMC-2中的含N分子N2H +和NH3似乎更强烈。这表明OMC-2具有更高的含氮分子丰度，或者具有更高的静态气体填充因子。我们从N2H +数据中识别出34个云核心。在猎户星云区域，N2H +的线宽很大（1.1-2.1 km s（-1））。在OMC-2 / 3区域，它变温和（0.5-1.3 km s（-1）），在猎户座星云的南部变小（0.3-1.1 km s（-1））。另一方面，在N2H +中观察到的静态纤芯的气体动力学温度在整体形灯丝上相当恒定（类似于20 K）。我们在OMC-2 / 3区域未检测到CCS排放。通常，在OMC-2 / 3区域中N2H +和HC3N的分布非常相似，但是我们在OMC-3中观察到N2H +和HC3N之间的位移超过2'，该链具有0-I类原恒星（考生）。

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