The Mt. Fuji submillimeter-wave telescope

Yutaro Sekimoto; Satoshi Yamamoto; Tomoharu Oka; Masafumi Ikeda; Hiroyuki Maezawa; Tetsuya Ito; Gaku Saito; Mitsuhiro Iwata; Kazuhisa Kamegai; Takeshi Sakai; Ke N.Ichi Tatematsu; Yuji Arikawa; Yoshiyuki Aso; Takashi Noguchi; Keisuke Miyazawa; Sheng Cai Shi; Shuji Saito; Hiroyuki Ozeki; Hideo Fujiwara; Junji Inatani; Masatoshi Ohishi; Kazufusa Noda; Yuichi Togashi

doi:10.1063/1.1150709

The Mt. Fuji submillimeter-wave telescope

Yutaro Sekimoto, Satoshi Yamamoto, Tomoharu Oka, Masafumi Ikeda, Hiroyuki Maezawa, Tetsuya Ito, Gaku Saito, Mitsuhiro Iwata, Kazuhisa Kamegai, Takeshi Sakai, Ke N.Ichi Tatematsu, Yuji Arikawa, Yoshiyuki Aso, Takashi Noguchi, Keisuke Miyazawa, Sheng Cai Shi, Shuji Saito, Hiroyuki Ozeki, Hideo Fujiwara, Junji InataniMasatoshi Ohishi, Kazufusa Noda, Yuichi Togashi

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Abstract

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 (C_I) 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 2′.2 and 3′.1, respectively. We describe the telescope system and report the performance obtained in the 1998 winter.

Original language	English
Pages (from-to)	2895-2907
Number of pages	13
Journal	Review of Scientific Instruments
Volume	71
Issue number	7
DOIs	https://doi.org/10.1063/1.1150709
Publication status	Published - 2000
Externally published	Yes

ASJC Scopus subject areas

Instrumentation

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10.1063/1.1150709

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Sekimoto, Y., Yamamoto, S., Oka, T., Ikeda, M., Maezawa, H., Ito, T., Saito, G., Iwata, M., Kamegai, K., Sakai, T., Tatematsu, K. N. I., Arikawa, Y., Aso, Y., Noguchi, T., Miyazawa, K., Shi, S. C., Saito, S., Ozeki, H., Fujiwara, H., ... Togashi, Y. (2000). The Mt. Fuji submillimeter-wave telescope. Review of Scientific Instruments, 71(7), 2895-2907. https://doi.org/10.1063/1.1150709

Sekimoto, Y, Yamamoto, S, Oka, T, Ikeda, M, Maezawa, H, Ito, T, Saito, G, Iwata, M, Kamegai, K, Sakai, T, Tatematsu, KNI, Arikawa, Y, Aso, Y, Noguchi, T, Miyazawa, K, Shi, SC, Saito, S, Ozeki, H, Fujiwara, H, Inatani, J, Ohishi, M, Noda, K & Togashi, Y 2000, 'The Mt. Fuji submillimeter-wave telescope', Review of Scientific Instruments, vol. 71, no. 7, pp. 2895-2907. https://doi.org/10.1063/1.1150709

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title = "The Mt. Fuji submillimeter-wave telescope",

abstract = "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 2′.2 and 3′.1, respectively. We describe the telescope system and report the performance obtained in the 1998 winter.",

author = "Yutaro Sekimoto and Satoshi Yamamoto and Tomoharu Oka and Masafumi Ikeda and Hiroyuki Maezawa and Tetsuya Ito and Gaku Saito and Mitsuhiro Iwata and Kazuhisa Kamegai and Takeshi Sakai and Tatematsu, {Ke N.Ichi} and Yuji Arikawa and Yoshiyuki Aso and Takashi Noguchi and Keisuke Miyazawa and Shi, {Sheng Cai} and Shuji Saito and Hiroyuki Ozeki and Hideo Fujiwara and Junji Inatani and Masatoshi Ohishi and Kazufusa Noda and Yuichi Togashi",

year = "2000",

doi = "10.1063/1.1150709",

language = "English",

volume = "71",

pages = "2895--2907",

journal = "Review of Scientific Instruments",

issn = "0034-6748",

publisher = "American Institute of Physics Publising LLC",

number = "7",

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TY - JOUR

T1 - The Mt. Fuji submillimeter-wave telescope

AU - Sekimoto, Yutaro

AU - Yamamoto, Satoshi

AU - Oka, Tomoharu

AU - Ikeda, Masafumi

AU - Maezawa, Hiroyuki

AU - Ito, Tetsuya

AU - Saito, Gaku

AU - Iwata, Mitsuhiro

AU - Kamegai, Kazuhisa

AU - Sakai, Takeshi

AU - Tatematsu, Ke N.Ichi

AU - Arikawa, Yuji

AU - Aso, Yoshiyuki

AU - Noguchi, Takashi

AU - Miyazawa, Keisuke

AU - Shi, Sheng Cai

AU - Saito, Shuji

AU - Ozeki, Hiroyuki

AU - Fujiwara, Hideo

AU - Inatani, Junji

AU - Ohishi, Masatoshi

AU - Noda, Kazufusa

AU - Togashi, Yuichi

PY - 2000

Y1 - 2000

N2 - 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 2′.2 and 3′.1, respectively. We describe the telescope system and report the performance obtained in the 1998 winter.

AB - 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 2′.2 and 3′.1, respectively. We describe the telescope system and report the performance obtained in the 1998 winter.

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DO - 10.1063/1.1150709

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SN - 0034-6748

VL - 71

SP - 2895

EP - 2907

JO - Review of Scientific Instruments

JF - Review of Scientific Instruments

IS - 7

ER -

The Mt. Fuji submillimeter-wave telescope

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