TY - GEN
T1 - Current status and future plan of Osaka Prefecture University 1.85-m mm-submm telescope project
AU - Nishimura, Atsushi
AU - Tokuda, Kazuki
AU - Harada, Ryohei
AU - Hasegawa, Yutaka
AU - Ueda, Shota
AU - Masui, Sho
AU - Konishi, Ryotaro
AU - Yamasaki, Yasumasa
AU - Kondo, Hiroshi
AU - Yokoyama, Koki
AU - Matsumoto, Takeru
AU - Minami, Taisei
AU - Okawa, Masanari
AU - Fujita, Shinji
AU - Konishi, Ayu
AU - Nakao, Yuka
AU - Nishimoto, Shimpei
AU - Kawashita, Sana
AU - Yoneyama, Sho
AU - Takashima, Tatsuyuki
AU - Goto, Kenta
AU - Okada, Nozomi
AU - Kimura, Kimihiro
AU - Abe, Yasuhiro
AU - Muraoka, Kazuyuki
AU - Maezawa, Hiroyuki
AU - Onishi, Toshikazu
AU - Ogawa, Hideo
N1 - Funding Information:
The 1.85-m telescope project is promoted on a lot of contributions of people engaged in this project, so the authors would like to thank all those people, Takafumi Kojima, Taku Nakajima, Toshihisa Tsutsumi, Ryoko Amari, Kozuki Yuto, Noriaki Arima, Ryosuke Kiridoshi, Takao Matsumoto, Shigeki Osaki, Touga Shiori, Minato Kozu, Yuya Ota, Yoshiharu Kojima, Akio Hashizume, Akihito Minami, Tsubasa Sakaguchi, Hidetoshi Tsuji, Tetsuya Katase, Shimpei Yashima, Masato Kunizane, Masahiro Minowa, Yukimasa Takenaka, Shinpei Yashima, Hirotaka Kurimoto, Atsushi Ezaki, Kazutoshi Maruyama, Hirofumi Okuno, Takashi Nohara, Kiyoko Tsuji, Yoshihide Tokko, Kazuki Toki, Tatsuro Nakayama, and Jun Korogi. We are also grateful to Shigeru Fuji, Akira Mori and Hiroyuki Iwashita, and the entire staff of the Nobeyama Radio Observatory for their useful support. This work was supported by JSPS KAKENHI Grant Numbers JP18H05440, JP15K05025, JP26247026, JP14J12320, JP22244014, and JP15071205, by the Mitsubishi Foundation and the Toray Science Foundation.
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PY - 2020
Y1 - 2020
N2 - We report the current status of the 1.85-m mm-submm telescope installed at the Nobeyama Radio Observatory (altitude 1400 m) and the future plan. The scientific goal is to reveal the physical/chemical properties of molecular clouds in the Galaxy by obtaining large-scale distributions of molecular gas with an angular resolution of several arcminutes. A semi-automatic observation system created mainly in Python on Linux-PCs enables effective operations. A large-scale CO J =2-1 survey of the molecular clouds (e.g., Orion-A/B, Cygnus-X/OB7, Taurus- California-Perseus complex, and Galactic Plane), and a pilot survey of emission lines from minor molecular species toward Orion clouds have been conducted so far. The telescope also is providing the opportunities for technical demonstrations of new devices and ideas. For example, the practical realizations of PLM (Path Length Modulator) and waveguide-based sideband separating filter, installation of the newly designed waveguide-based circular polarizer and OMT (Orthomode Transducer), and so on. As the next step, we are now planning to relocate the telescope to San Pedro de Atacama in Chile (altitude 2500 m), and are developing very wideband receiver covering 210-375 GHz (corresponding to Bands 6-7 of ALMA) and full-automatic observation system. The new telescope system will provide large-scale data in the spatial and frequency domain of molecular clouds of Galactic plane and Large/Small Magellanic Clouds at the southern hemisphere. The data will be precious for the comparison with those of extra-galactic ones that will be obtained with ALMA as the Bands 6/7 are the most efficient frequency bands for the surveys in extra-galaxies for ALMA.
AB - We report the current status of the 1.85-m mm-submm telescope installed at the Nobeyama Radio Observatory (altitude 1400 m) and the future plan. The scientific goal is to reveal the physical/chemical properties of molecular clouds in the Galaxy by obtaining large-scale distributions of molecular gas with an angular resolution of several arcminutes. A semi-automatic observation system created mainly in Python on Linux-PCs enables effective operations. A large-scale CO J =2-1 survey of the molecular clouds (e.g., Orion-A/B, Cygnus-X/OB7, Taurus- California-Perseus complex, and Galactic Plane), and a pilot survey of emission lines from minor molecular species toward Orion clouds have been conducted so far. The telescope also is providing the opportunities for technical demonstrations of new devices and ideas. For example, the practical realizations of PLM (Path Length Modulator) and waveguide-based sideband separating filter, installation of the newly designed waveguide-based circular polarizer and OMT (Orthomode Transducer), and so on. As the next step, we are now planning to relocate the telescope to San Pedro de Atacama in Chile (altitude 2500 m), and are developing very wideband receiver covering 210-375 GHz (corresponding to Bands 6-7 of ALMA) and full-automatic observation system. The new telescope system will provide large-scale data in the spatial and frequency domain of molecular clouds of Galactic plane and Large/Small Magellanic Clouds at the southern hemisphere. The data will be precious for the comparison with those of extra-galactic ones that will be obtained with ALMA as the Bands 6/7 are the most efficient frequency bands for the surveys in extra-galaxies for ALMA.
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U2 - 10.1117/12.2560955
DO - 10.1117/12.2560955
M3 - Conference contribution
AN - SCOPUS:85099077357
T3 - Proceedings of SPIE - The International Society for Optical Engineering
BT - Ground-Based and Airborne Telescopes VIII
A2 - Marshall, Heather K.
A2 - Spyromilio, Jason
A2 - Usuda, Tomonori
PB - SPIE
T2 - Ground-Based and Airborne Telescopes VIII 2020
Y2 - 14 December 2020 through 22 December 2020
ER -