Multi-Line Survey Observation of the Galactic Plane by Balloon-Borne Telescopes

气球望远镜对银道面的多线巡天观测

• 批准号: 06402004
• 负责人: OKUDA Haruyuki
• 金额: $ 20.61万
• 依托单位: The Institute of Space and Astronautical Science (ISAS)
• 依托单位国家: 日本
• 项目类别: Grant-in-Aid for Scientific Research (A)
• 财政年份: 1994
• 资助国家: 日本
• 起止时间: 1994 至 1996
• 项目状态: 已结题
• 来源: https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-06402004/
• 关键词: Infrared Radiation; The Galaxy; Interstellar Matter; Interstellar Gas; Balloon-Borne Telescope; Far-Infrared Radiation; Spectroscopy; Star Fromation; 気球観測

It has widely been demonstrated that there exist various stages of gas, such as atoms, ions, and molecules in the interstellar space of the Galaxy. Among them, hydrogen 21 cm line and CO 2.6 mm line have been playing important roles in investigations of the galactic structure and physical and chemical stage of the Galaxy through the neutral hydrogen atomic gas and molecular gas, respectively. However, the previous result of our study by a [CII] far-Infrared line survey showed that there exists a new interstellar gas phase, "diffuse photodissociation region" . Photodissociation regions in the enterface region between the CO molecular gas and the hydrogen atomic gas, and are the dominant coolant by conversion of UV and optical radiation from luminous stars into the far-infrared radiation.Therefore, the far-Infrared spectral lines are key for understanding the galactic interstellar space/matter, and are a tool for measuring the interstellar heavy element abundance. We have carried out a wide sky survey of [CII] 158 micron by a space infrared telescope ( IRTS ) and by a balloon-borne telescope ( BICE ), and [OI] 63 micron, [OIII] 52,88 micron, [CII] 158 micron, [NII] 122 micron, and [NIII] 57 micron lines by a European Infrared space observatory ( ISO ). From these data, we have shown diffuse photodissociation regions and diffuse ionization regions are important gas phases in the Galactic Interstellar space.

人们广泛地证明，在银河系的星际空间中存在着不同阶段的气体，如原子、离子和分子。其中，氢21 cm线和CO 2.6 mm线分别通过中性氢原子气体和分子气体在银河系结构和物理化学阶段的研究中发挥了重要作用。然而，我们先前的[CII]远红外线测量结果表明，存在一个新的星际气体相--“扩散光解离区”。光解离区位于CO分子气体和氢原子气体之间的入口区，是从发光星发出的紫外光和光辐射转化为远红外辐射的主要冷却剂，因此，远红外光谱线是理解银河系星际空间/物质的关键，也是测量星际重元素丰度的工具。我们用空间红外望远镜(IRTS)和气球载望远镜(BICE)进行了[CII]158微米的宽天测量，以及欧洲红外空间天文台(ISO)的[OI]63微米、[OIII]52，88微米、[CII]158微米、[NII]122微米和[NII]57微米的测量。从这些数据可以看出，扩散光解离区和扩散电离区是银河系星际空间中重要的气相。

项目成果

T.Nakagawa, Y.Y.Yui, Y.Doi, H.Okuda, H.Shibai, K.Mochizuki, T.Nishimura, and F.J.Low.: ""Far-Infrared [CII] Line Survey Observations of the Galactic Plane"" Astrophys.J.Suppl.115(in press). (1998)

T.Nakakawa、Y.Y.Yui、Y.Doi、H.Okuda、H.Shibai、K.Mochizuki、T.Nishimura 和 F.J.Low.：“银河平面的远红外 [CII] 线巡天观测”天体物理学

H.Shibai et al.: ""Fight Performance of the Far-Infrared Line Mapper (FILM)." Proc.of SPIE 2817,"Infrared Spacebone Remote Sensing IV". 267-275 (1996)

H.Shibai 等人：“远红外测线仪 (FILM) 的战斗性能。”Proc.of SPIE 2817，“红外太空骨遥感 IV”。267-275 (1996)

K.Mochizuki et al.: "A Survey of the Large Magellanic Cloud in the [CII] 158 Micron Line" Astrophysical Journal (Letters). 430. L37-L40 (1994)

K.Mochizuki 等人：“[CII] 158 微米线中大麦哲伦云的调查”天体物理学杂志（快报）。

N.Hiromoto et al.: "Ge : Ga Far-Infrared Photoconductors for Space Applications" Jpn.J.Appl.Phys. 35. 1676-1680 (1996)

N.Hiromoto 等人：“Ge : Ga 远红外光电导体用于空间应用”Jpn.J.Appl.Phys。

S.Makiuti, H.Shibai, H.Okuda, T.Nakagawa, H.Matsuhara, N.Hiromoto, and K.Okumura: ""Far-Infrared [CII] Line Observation of the Galactic Plane by the IRTS "" Publ.Astron.Soc.Jp.48. L71-L75 (1996)

S.Makiuti、H.Shibai、H.Okuda、T.Nakakawa、H.Matsuhara、N.Hiromoto 和 K.Okumura：“IRTS 对银河平面的远红外 [CII] 线观测”出版。