A 350 GHz SIS receiver on the nobeyama 10 m submillimeter telescope

Yutaro Sekimoto; Takeshi Sakai; Gaku Saito; Ken'ichi Tatematsu; Kunihiko Tanaka; Kotaro Kohno; Takashi Noguchi; Hiroyuki Iwashita; Toshikazu Takahashi; Naohisa Satou; Sozo Yokogawa; Seiichi Sakamoto; Nobuharu Ukita; Ryohei Kawabe; Tetsuya Ito; Hiroyuki Maezawa; Satoshi Yamamoto

doi:10.1093/pasj/53.5.951

A 350 GHz SIS receiver on the nobeyama 10 m submillimeter telescope

Yutaro Sekimoto, Takeshi Sakai, Gaku Saito, Ken'ichi Tatematsu, Kunihiko Tanaka, Kotaro Kohno, Takashi Noguchi, Hiroyuki Iwashita, Toshikazu Takahashi, Naohisa Satou, Sozo Yokogawa, Seiichi Sakamoto, Nobuharu Ukita, Ryohei Kawabe, Tetsuya Ito, Hiroyuki Maezawa, Satoshi Yamamoto

Research output: Contribution to journal › Article › peer-review

11 Citations (Scopus)

Abstract

We have developed a low-noise submillimeter-wave SIS receiver (320-360 GHz) for a 10 m submillimeter telescope, which was installed at Nobeyama in 2000 February. This receiver and a millimeter-wave SIS receiver are mounted on the ceiling of the Cassegrain receiver cabin of the 10 m telescope. Two curved mirrors couple a shaped Cassegrain beam from the subreflector to mixer horns. The minimum noise temperature measured in front of the receiver was 52 K in double sideband (DSB) at a local oscillator (LO) frequency of 354 GHz, which corresponds to three-times quantum limits (3hv/k_B). This noise temperature contributions are resolved into the optics, mixer, and IF parts. The temperature ripple of a two-stage Gifford-McMahon cryocooler has been reduced to be 2 mK peak-to-peak at the mixer block with a helium pot temperature stabilizer. Mechanical vibration (30 μm peak-to-peak) of the cold head degrades the receiver stability.

Original language	English
Pages (from-to)	951-958
Number of pages	8
Journal	Publications of the Astronomical Society of Japan
Volume	53
Issue number	5
DOIs	https://doi.org/10.1093/pasj/53.5.951
Publication status	Published - 2001 Oct 25
Externally published	Yes

Keywords

Instrumentation: detectors
Radio lines: general
Submillimeter
Techniques: spectroscopic

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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10.1093/pasj/53.5.951

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Sekimoto, Y., Sakai, T., Saito, G., Tatematsu, K., Tanaka, K., Kohno, K., Noguchi, T., Iwashita, H., Takahashi, T., Satou, N., Yokogawa, S., Sakamoto, S., Ukita, N., Kawabe, R., Ito, T., Maezawa, H., & Yamamoto, S. (2001). A 350 GHz SIS receiver on the nobeyama 10 m submillimeter telescope. Publications of the Astronomical Society of Japan, 53(5), 951-958. https://doi.org/10.1093/pasj/53.5.951

Sekimoto, Y, Sakai, T, Saito, G, Tatematsu, K, Tanaka, K, Kohno, K, Noguchi, T, Iwashita, H, Takahashi, T, Satou, N, Yokogawa, S, Sakamoto, S, Ukita, N, Kawabe, R, Ito, T, Maezawa, H & Yamamoto, S 2001, 'A 350 GHz SIS receiver on the nobeyama 10 m submillimeter telescope', Publications of the Astronomical Society of Japan, vol. 53, no. 5, pp. 951-958. https://doi.org/10.1093/pasj/53.5.951

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abstract = "We have developed a low-noise submillimeter-wave SIS receiver (320-360 GHz) for a 10 m submillimeter telescope, which was installed at Nobeyama in 2000 February. This receiver and a millimeter-wave SIS receiver are mounted on the ceiling of the Cassegrain receiver cabin of the 10 m telescope. Two curved mirrors couple a shaped Cassegrain beam from the subreflector to mixer horns. The minimum noise temperature measured in front of the receiver was 52 K in double sideband (DSB) at a local oscillator (LO) frequency of 354 GHz, which corresponds to three-times quantum limits (3hv/kB). This noise temperature contributions are resolved into the optics, mixer, and IF parts. The temperature ripple of a two-stage Gifford-McMahon cryocooler has been reduced to be 2 mK peak-to-peak at the mixer block with a helium pot temperature stabilizer. Mechanical vibration (30 μm peak-to-peak) of the cold head degrades the receiver stability.",

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AU - Tatematsu, Ken'ichi

AU - Tanaka, Kunihiko

AU - Kohno, Kotaro

AU - Noguchi, Takashi

AU - Iwashita, Hiroyuki

AU - Takahashi, Toshikazu

AU - Satou, Naohisa

AU - Yokogawa, Sozo

AU - Sakamoto, Seiichi

AU - Ukita, Nobuharu

AU - Kawabe, Ryohei

AU - Ito, Tetsuya

AU - Maezawa, Hiroyuki

AU - Yamamoto, Satoshi

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AB - We have developed a low-noise submillimeter-wave SIS receiver (320-360 GHz) for a 10 m submillimeter telescope, which was installed at Nobeyama in 2000 February. This receiver and a millimeter-wave SIS receiver are mounted on the ceiling of the Cassegrain receiver cabin of the 10 m telescope. Two curved mirrors couple a shaped Cassegrain beam from the subreflector to mixer horns. The minimum noise temperature measured in front of the receiver was 52 K in double sideband (DSB) at a local oscillator (LO) frequency of 354 GHz, which corresponds to three-times quantum limits (3hv/kB). This noise temperature contributions are resolved into the optics, mixer, and IF parts. The temperature ripple of a two-stage Gifford-McMahon cryocooler has been reduced to be 2 mK peak-to-peak at the mixer block with a helium pot temperature stabilizer. Mechanical vibration (30 μm peak-to-peak) of the cold head degrades the receiver stability.

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KW - Radio lines: general

KW - Submillimeter

KW - Techniques: spectroscopic

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A 350 GHz SIS receiver on the nobeyama 10 m submillimeter telescope

Abstract

Keywords

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