Portable Submillmeter-wave SIS Receiver

便携式亚毫米波 SIS 接收器

• 批准号: 10554004
• 负责人: SEKIMOTO Yutaro
• 金额: $ 8.13万
• 依托单位: NATIONAL ASTRONOMICAL OBSERVATORY OF JAPAN (1999-2000)The University of Tokyo (1998)
• 依托单位国家: 日本
• 项目类别: Grant-in-Aid for Scientific Research (B).
• 财政年份: 1998
• 资助国家: 日本
• 起止时间: 1998 至 2000
• 项目状态: 已结题
• 来源: https://kaken.nii.ac.jp/en/grant/KAKENHI-PROJECT-10554004/
• 关键词: Submillimeter-wave Receiver; G-M cryocooler; Superconductor application; Submillimeter-wave Astronomy; Environmental Research; Molecular Sepctroscopy; 超伝導; 地球環境; 分子分光

We have developed a portable submillmeter-wave receiver with a low-power consumption cryocooler. Because of lightweight(30kg), it is easy to transport the SIS receiver to high altitude sites such as Pampa la Bola in northern Chile. A careful thernal design include a new 250 K shield gives an operational temperature 3.5 K at the 2^<nd> stage. A simple optical design allows high aperture efficiency in submillimeter-wave frequencies above 400 GHz. With a new low noise SIS receiver, we have surveyed a giant molecular cloud, M17 in the neutral carbon atom(CI : 492GHz) and CO J=3-2(345 GHz)lines. The integrated intensity ratio of CI to CO J=3-2([CI]/[CO(3-2)])in M17 shows a spatial gradient that it continuously increases from 0.2 in the NE part(M17A)near OB clusters to 0.8 in the SW part(M17D). The [CI]/[CO(3-2)]of 0.5 in total is close to the Galactic value of 0.57 obtaied by COBE FIRAS.Thus, the giant molecular clouds without strong UV sources such as M17D largely contribute to the CI emission in the Galactic plane. Our developments on the small, low-power consumption and low-noise SIS receiver are useful for molecular spectroscopy and atmospheric research as well we the Atacama Large Millimeter Submillimeter Array(ALMA).

研制了一种低功耗制冷机的便携式亚毫米波接收机。由于重量轻（30公斤），很容易将SIS接收机运输到高海拔地区，如智利北方的Pampa la Bola。一个精心的热设计，包括一个新的250 K的屏蔽提供了一个工作温度为3.5 K的第2<nd>阶段。一个简单的光学设计允许在400 GHz以上的亚毫米波频率的高孔径效率。用一种新的低噪声SIS接收机观测了一个巨大的分子云M17的中性碳原子（CI：492 GHz）和CO J=3-2（345 GHz）谱线。M17中CI与CO的积分强度比J=3-2（[CI]/[CO（3-2）]）显示了一个空间梯度，它从靠近OB团的NE部分（M17 A）的0.2连续增加到SW部分（M17 D）的0.8。[CI]/[CO（3-2）]为0.5，接近COBE FIRAS的银河系数值0.57，因此，没有强紫外源的巨大分子云（如M17 D）对银河系面CI辐射贡献很大。我们研制的小型、低功耗、低噪声的SIS接收机对分子光谱学和大气研究以及阿塔卡马大型毫米波亚毫米波阵列（阿尔马）都有重要意义。

项目成果

Y.Sekimoto,T.Sakai et al.: "A Plan of Receiver developments for ASTE/LMSA"ALMA memo. 315. 1-17 (2000)

Y.Sekimoto、T.Sakai 等人：“ASTE/LMSA 接收器开发计划”ALMA 备忘录。

Yamamoto, Satoshi ; Maezawa, Hiroyuki ; Ikeda, Masafumi ; Ito, Tetsuya ; Oka, Tomoharu ; Saito, Gaku ; Iwata, Mitsuhiro ; Kamegai, Kazuhisa ; Sakai, Takeshi ; Sekimoto, Yutaro ; Tatematsu, Ken'ichi ; Noguchi, Takeshi ; Shi, Sheng-Cai ; Arikawa, Yuji ; Aso

山本聪；

M.Ikeda,H.Maezawa, et al.: "Large-scale mapping observations of the CI 3P1-3P0 line toward the Orion A molecular Cloud"Astrophys.J.. 527. L59-L62 (2000)

M.Ikeda、H.Maezawa 等人：“CI 3P1-3P0 线朝向猎户座 A 分子云的大规模测绘观测”Astrophys.J.. 527. L59-L62 (2000)

Y.Sekimoto, S.Yamamoto, T.Oka, M.Ikeda, H.Maezawa, T.Ito, G.Saito, M.Iwata, K.Kamegai, T.Sakai, K.Tatematsu, Y.Arikawa. Y.Aso, T.Noguchi, S.C.Shi, K.Miyazawa, S.Saito, H.Ozeki, H.Fujiwara, M.Ohishi, J.Inatani, K.Noda, and Y.Togashi: "The Mt. Fuji subumill

Y.Sekimoto、S.Yamamoto、T.Oka、M.Ikeda、H.Maezawa、T.Ito、G.Saito、M.Iwata、K.Kamegai、T.Sakai、K.Tatematsu、Y.Arikawa。

K. Matsuzaki, et al.: "Hard X-ray emission from giant molecular cloud NGC6334 and M17"Japanese-German Workshop on High Energy Astrophysics. 56-59 (1998)

K. Matsuzaki 等人：“巨型分子云 NGC6334 和 M17 的硬 X 射线发射”日德高能天体物理学研讨会。