Journal Article

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 and Satoshi Yamamoto

in Publications of the Astronomical Society of Japan

Volume 53, issue 5, pages 951-958
Published in print October 2001 | ISSN: 0004-6264
Published online October 2001 | e-ISSN: 2053-051X | DOI: http://dx.doi.org/10.1093/pasj/53.5.951
A 350 GHz SIS Receiver on the Nobeyama 10 m Submillimeter Telescope

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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 ([math]). 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 [math] peak-to-peak) of the cold head degrades the receiver stability.

Keywords: instrumentation: detectors; submillimeter; techniques: spectroscopic; radio lines: general

Journal Article.  3947 words.  Illustrated.

Subjects: Astronomy and Astrophysics ; Astronomical Instrumentation, Methods, and Techniques

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