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テラヘルツ受信機のASTE望遠鏡への搭載実験と 実験室における分子分光実験
渡邉, 祥正;酒井, 剛;坂井, 南美
Permalink : http://hdl.handle.net/2115/77788
JaLCDOI : 10.14943/lowtemsci.78.241
KEYWORDS : テラヘルツ;受信機開発;星間分子;分子分光;Terahertz;Receiver development;Interstellar molecule;Spectroscopy
Abstract
天文学では観測のための装置開発も重要な研究テーマである．これまであまり観測されていない電 磁波の波長帯の観測装置や，より高い感度の検出器を開発することで，今まで見えなかった新しい宇 宙の姿を明らかにできる．電波と赤外線の中間の波長領域であるテラヘルツ帯も発展途上の波長帯の ひとつである．本稿では，テラヘルツ帯の天体観測を目指して，受信機を開発し南米チリのアタカマ 高原のASTE望遠鏡に搭載実験をしたので紹介する．また，天体観測用の装置は非常に性能が高く， 実験室における様々な測定でも性能を十分に発揮する．本稿の後半では，電波天文学で使われる受信 機やデジタル分光計を使った，分子分光の実験を紹介する．
The terahertz band,which corresponds to a frequency range of 1-10 THz,remains relatively unexplored in both astronomy and technology.In order to observe astronomical objects from the ground in the terahertz band,we developed low-noise hot electron bolometer(HEB)mixers and built a cartridge-type heterodyne receiver using the HEB mixers. The cartridge-type receiver was installed on the ASTE 10 m radio telescope in Chile to detect molecular spectral lines from star-forming regions. In addition,we developed a molecular spectrometer in a laboratory using low- noise ALMA-type radio receivers and wide-band digital spectrometers. Accurate frequency of spectral lines of known complex organic species will be measured by the spectrometer,to interpret the results from radio astronomical observations.
The terahertz band,which corresponds to a frequency range of 1-10 THz,remains relatively unexplored in both astronomy and technology.In order to observe astronomical objects from the ground in the terahertz band,we developed low-noise hot electron bolometer(HEB)mixers and built a cartridge-type heterodyne receiver using the HEB mixers. The cartridge-type receiver was installed on the ASTE 10 m radio telescope in Chile to detect molecular spectral lines from star-forming regions. In addition,we developed a molecular spectrometer in a laboratory using low- noise ALMA-type radio receivers and wide-band digital spectrometers. Accurate frequency of spectral lines of known complex organic species will be measured by the spectrometer,to interpret the results from radio astronomical observations.
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