Far-Infrared Spectroscopic Survey of Near-by Interstellar Clouds

近邻星际云的远红外光谱巡天

• 批准号: 05452022
• 负责人: NAKAGAWA Takao
• 金额: $ 4.74万
• 依托单位: The Institute of Space & Astronautical Science
• 依托单位国家: 日本
• 项目类别: Grant-in-Aid for General Scientific Research (B)
• 财政年份: 1993
• 资助国家: 日本
• 起止时间: 1993 至 1994
• 项目状态: 已结题
• 来源: https://kaken.nii.ac.jp/en/grant/KAKENHI-PROJECT-05452022/
• 关键词: Interstellar Gas; Far-Infrared Spectroscopy; [CII] Spectral Line; Star-Forming Regions; Photo-Dissociation Regions; Survey Observation

The far-infrared [C II] spectral line (^2P_<3/2>-^2P_<1/2>,157.7409 mum), which is emitted by singly ionized carbon (C^+), is the dominant coolant of neutral interstellar clouds. Hence observations of the line is crucial to reveal the physical states, especially the energy budget, of interstellar clouds.We have been successfully making survey observations of the [C II] line using a dedicated observing instrument BICE.The observational results are very important for interstellar physics. However, since there are various components in a line sight toward the Galactic plane, the observational results are rather complicated.Hence the [C II] observations of indivudual clouds which have a single component in a line sight are very important to understand the physical properties of the [C II] emitting regions. To make templates of [C II] emitting regions, we observed the Orion regions, which is the most representative massive-star-forming regions. The observation was carried out on September 3,1994, from the Sanriku Balloon Center, using the BICE.The observation revelaed that there are several groups of [C II] emitting regions with different physical parameters in the Orion regions. Using the results, we reinvestigated our previous [C II] observations of the Galactic plane.

远红外[C II]光谱线（^2p_ <3/2> - ^2p_ <1/2>，157.7409 MUM）是由单个离子化的碳（C^+）发射的，是中性星际云的主要冷却剂。因此，观察这条线对于揭示星际云的物理状态，尤其是能量预算至关重要。我们已经成功地使用专用观察仪器泡沫对[C II]线进行了调查观察。观察结果对星际物理学非常重要。但是，由于一条线瞄准器朝向银河平面上有各种组件，因此观察结果相当复杂。因此，在线路视觉中具有单个组分的独立云的[C II]观察结果对于理解[C II]发射区域的物理特性非常重要。为了制作[C II]发射区域的模板，我们观察到猎户座区域，这是最具代表性的大型巨大形成区域。该观察结果是在1994年9月3日从Sanriku气球中心进行的。观察结果是，在猎户座地区，有几组[C II]发射区域具有不同的物理参数。使用结果，我们对银河平面的先前[C II]观察进行了重新研究。

项目成果

Okuda,et al.: "Large Scale [CII] Line Emission in the Galaxy Observed by Stratospheric Balloons" Infrared Physics. 35. 391-405 (1994)

Okuda 等人：“平流层气球观测到的星系中的大规模 [CII] 线发射”红外物理学。

Yui, et al.: "A [CII] 158 micron Map of the rho-Ophiuchi Cloud" Astrophysical Journal Letters. 419. L37-L40 (1993)

Yui 等人：“一张 [CII] 158 微米 rho-Ophiuchi 云图”《天体物理学杂志快报》。

Nakagawa,et al.: "Deficit of Far-Infrared [CII] Line Emission toward the Galactic Center" Astrophys. J.Letters. 455(印刷中). (1995)

Nakakawa 等人：“向银河系中心发射的远红外 [CII] 线的缺陷”，J.Letters 455（出版中）。

Y.Doi,et al.: "Clumpy Structure of Interstellar Clouds in the Cygnus-X Region" AIP Conf.Proceedings "Back to the Galaxy". 278. 307-310 (1993)

Y.Doi 等人：“Cygnus-X 区域星际云的块状结构”AIP Conf.Proceedings“回到银河系”。

K.Mizutani et al.: "[CII]158 Micron and [OI] 63 Micron Observztions of the Galactic Center Region)" Astrophysical Journal Supplement. 91. 613-624 (1994)

K.Mizutani 等人：“银河系中心区域的[CII]158 微米和[OI]63 微米观测）”天体物理学杂志增刊。