The Mt. Fuji submillimeter-wave telescope

• 資料種別: 文書・図像類
• タイトル: The Mt. Fuji submillimeter-wave telescope
• 著者・編者: SEKIMOTO, Yutaro; YAMAMOTO, Satoshi; OKA, Tomoharu; IKEDA, Masafumi; MAEZAWA, Hiroyuki; ITO, Tetsuya; SAITO, Gaku; IWATA, Mitsuhiro; KAMEGAI, Kazuhisa; SAKAI, Takeshi; TATEMATSU, Ken-ichi; ARIKAWA, Yuji; ASO, Yoshiyuki; NOGUCHI, Takashi; MIYAZAWA, Keisuke; SHI, Sheng-Cai; SAITO, Shuji; OZEKI, Hiroyuki; FUJIWARA, Hideo; INATANI, Junji; OHISHI, Masatoshi; NODA, Kazufusa; TOGASHI, Yuichi
• 著者標目: SEKIMOTO, Yutaro; YAMAMOTO, Satoshi; OKA, Tomoharu; IKEDA, Masafumi; MAEZAWA, Hiroyuki; ITO, Tetsuya; SAITO, Gaku; IWATA, Mitsuhiro; KAMEGAI, Kazuhisa; SAKAI, Takeshi; TATEMATSU, Ken-ichi; ARIKAWA, Yuji; ASO, Yoshiyuki; NOGUCHI, Takashi; MIYAZAWA, Keisuke; SHI, Sheng-Cai; SAITO, Shuji; OZEKI, Hiroyuki; FUJIWARA, Hideo; INATANI, Junji; OHISHI, Masatoshi; NODA, Kazufusa; TOGASHI, Yuichi
• 出版事項: American Institute of Physics
• 出版年月日等: 2000-07
• 出版年（W3CDTF）: 2000-07
• タイトル（掲載誌）: Review of Scientific Instruments
• 巻号年月日等（掲載誌）: 71 7
• 掲載巻: 71
• 掲載号: 7
• 掲載ページ: 2895-2907
• 本文の言語コード: eng
• 対象利用者: 一般
• 一般注記: We have developed a 1.2 m submillimeter-wave telescope at the summit of Mt. Fuji to survey emission lines of the neutral carbon atom (CI) toward the Milky Way. A superconductor-insulator-superconductor mixer receiver on the Nasmyth focus is used to observe the 492 GHz band in SSB and the 345 GHz band in DSB simultaneously. The receiver noise temperature is 300 K in SSB and 200 K in DSB for 492 and 345 GHz, respectively. The intermediate frequency frequency is 1.8–2.5 GHz. An acousto-optical spectrometer which has the total bandwidth of 0.9 GHz and 1024 channel outputs has also been developed. The telescope was installed at the summit of Mt. Fuji (alt. 3725 m) in July 1998. It has been remotely operated via a satellite communication system from Tokyo or Nobeyama. Atmospheric opacity at Mt. Fuji was 0.4–1.0 at 492 GHz during 30% of the time and 0.07–0.5 at 345 GHz during 60% of the time from November 1998 to February 1999. The system noise temperature was 1000–3000 K in SSB at 492 GHz and 500–2000 K in DSB at 345 GHz. We observed the CI (3P1–3P0: 492 GHz) and CO (J = 3–2: 345 GHz) emission lines from nearby molecular clouds with the beam size of 22 and 31, respectively. We describe the telescope system and report the performance obtained in the 1998 winter.
• 一次資料へのリンクURL: https://u-fukui.repo.nii.ac.jp/?action=repository_action_common_download&item_id=22455&item_no=1&attribute_id=22&file_no=1
• オンライン閲覧公開範囲: 限定公開
• 連携機関・データベース: 国立情報学研究所 : 学術機関リポジトリデータベース（IRDB）（機関リポジトリ）; https://irdb.nii.ac.jp
• 提供元機関・データベース: 福井大学 : 福井大学学術機関リポジトリ