A Research of the Galactic Structure through the [CII] 158 Micron Line

通过[CII]158微米线研究银河系结构

• 批准号: 02402002
• 负责人: OKUDA Haruyuki
• 金额: $ 19.26万
• 依托单位: The Institute of Space and Astronautical Science
• 依托单位国家: 日本
• 项目类别: Grant-in-Aid for General Scientific Research (A)
• 财政年份: 1990
• 资助国家: 日本
• 起止时间: 1990 至 1993
• 项目状态: 已结题
• 来源: https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-02402002/
• 关键词: Interstellar Physics; Far-Infrared Spectroscopy; [CII] Spectral Line; The Galaxy; Fabry-Perot Spectrometer; 〔CII〕スペクトル線; 大マゼラン雲; ファーブルペロー分光器; 銀河構造

By using a balloon borne telescope, an extensive survey of the [CII] line emission of the Galaxy has been undertaken. To minimize the instrumental emission, an off-axis telescope with a Newtonian-Nasmyth focus was used in conjunction with a liquid helium cooled Fabry-Perot spectrometer. The beam size of the telescope was 12' in diameter and the spectral resolution of the spectrometer was 175 km/s in velocity scale.The balloon flights were made from Palestine, TX in 1991 and from Alice Springs, Australia in 1992. By both obsevations, the major part of the galactic plane in the northern sky and the southern sky has been scanned. As a result, a complete map of the [CII] line intensity distribution has been constructed for the region from - 100ﾟ to 80ﾟ in galactic longitude and within (]SY.+-。[) 4ﾟ in galactic latitude. In addition to the general scan of the galactic plane, the observations were extended to some individual sources, such as Cyg-X region, p-Oph dark cloud and Large Magellanic Cloud.The observed maps reveal strong [CII] line emission extensively distributed in the galactic plane, as well as many discrete sources associated with HII regions and/or molecular clouds. The distribution is more or less correlated with far infrared continuum and CO line intensity distributions. However, detailed comparisons show interesting differences between the three components.

利用球载望远镜对银河系的[CII]线辐射进行了广泛的观测。为了尽量减少仪器发射，一个离轴望远镜与牛顿-纳斯迈斯焦点与液氦冷却法布里-珀罗光谱仪一起使用。望远镜的光束直径为12“，光谱仪的速度分辨率为175 km/s。气球飞行于1991年从德克萨斯州的巴勒斯坦和1992年从澳大利亚的爱丽丝泉进行。通过这两次观测，对银道面在北方和南方的主要部分进行了扫描。结果，在银经-100 ° C ~ 80 ° C范围内，（）SY ±-内，绘制了一幅完整的[CII]线强度分布图。[）银河纬度4度。除了对银道面的一般性扫描外，还对Cyg-X区、p-Oph暗云和大麦哲伦云等单个源进行了观测，观测到的图显示了在银道面广泛分布的强[CII]线辐射，以及许多与HII区和/或分子云有关的离散源。该分布与远红外连续谱和CO谱线强度分布有一定的相关性。然而，详细的比较显示了这三个组成部分之间有趣的差异。

项目成果

Okuda, H.: "Balloon Observations of Diffuse Infrared Emission in the Galaxy" IR Phys.32. 365 (1991)

Okuda, H.：“银河系中漫射红外发射的气球观测”IR Phys.32。

Nakagawa, T.: "Balloon-borne Far-Infrared Spectroscopy" ASP Conf.Ser. "Astronomical Infrared Spectroscopy : Future Observational Directions. 373-381 (1993)

Nakakawa, T.：“气球载远红外光谱”ASP Conf.Ser。

Mizutani,K,et al.: "〔CII〕 158μm and 〔OI〕 63μm Observations of the Galactic Center Region" Astrophys.J.

Mizutani,K,et al.：“银河系中心区域的[CII] 158μm 和[OI] 63μm 观测” Astrophys.J。

Mochizuki, K., Nakagawa, T., Doi, Y., Yui, Y.Y., Okuda, H., Yui, M., Shibai, H., Nishimura, T., Low, F.J.: "A Survey of the Large Magellanic Cloud in the [CII] 158 Micron Line" Astrophysical Journal. 430. L37-L40 (1994)

Mochizuki, K.、Nakakawa, T.、Doi, Y.、Yui, Y.Y.、Okuda, H.、Yui, M.、Shibai, H.、Nishimura, T.、Low, F.J.：“大麦哲伦星系的调查

Okyda,H.: "Large Scale Distribution of the[CII]Fine Structure Line in the Galaxy" Adv.Space Res.(1993)

Okyda, H.：“银河系中[CII]精细结构线的大尺度分布”Adv.Space Res.(1993)