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Dome Fuji in Antarctica as a Site for Infrared and Terahertz Astronomy

Published online by Cambridge University Press:  30 January 2013

Masumichi Seta ,
Naomasa Nakai ,
Shun Ishii ,
Makoto Nagai ,
Yusuke Miyamoto ,
Takashi Ichikawa ,
Naruhisa Takato  and
Hideaki Motoyama
Masumichi Seta
Affiliation:
Institute of Physics, University of Tsukuba, 305-8571, 1-1-1 Ten-nodai, Tsukuba, Ibaraki, Japan email: [email protected]
Naomasa Nakai
Affiliation:
Institute of Physics, University of Tsukuba, 305-8571, 1-1-1 Ten-nodai, Tsukuba, Ibaraki, Japan email: [email protected]
Shun Ishii
Affiliation:
Institute of Physics, University of Tsukuba, 305-8571, 1-1-1 Ten-nodai, Tsukuba, Ibaraki, Japan email: [email protected]
Makoto Nagai
Affiliation:
Institute of Physics, University of Tsukuba, 305-8571, 1-1-1 Ten-nodai, Tsukuba, Ibaraki, Japan email: [email protected]
Yusuke Miyamoto
Affiliation:
Institute of Physics, University of Tsukuba, 305-8571, 1-1-1 Ten-nodai, Tsukuba, Ibaraki, Japan email: [email protected]
Takashi Ichikawa
Affiliation:
Astronomical Institute, Tohoku University, 980-8578, Aramaki, Aoba, Sendai, Miyagi, Japan
Naruhisa Takato
Affiliation:
Subaru Telescope, National Astronomical Observatory of Japan, 96720, 650 North A'ohoku Place, Hilo, HI, USA
Hideaki Motoyama
Affiliation:
National Institute of Polar Research, 190-8518, 10-3 Midoricho, Tachikawa, Tokyo, Japan
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Abstract

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Dome Fuji on the Antarctic high plateau may be a good site for terahertz astronomy because of its high altitude of 3,810 m and low average temperature of −54°C. We have demonstrated that the opacity at 220 GHz from Dome Fuji in summer is very good and stable; τ = 0.045 ± 0.007. We have developed a transportable 30 cm telescope to map the Milky Way in the CO (J=4–3) and the [CI] (3P1–3P0) lines at Dome Fuji from 2014. It has a 9′ beam. Physical conditions such as density and temperature of molecular clouds could be derived from a direct comparison of CO (J=4–3) and [CI] (3P1–3P0) with CO (J=1–0) taken by the Columbia–CfA survey. We are also developing a 1.2 m sub-millimeter telescope. It will be equipped with a dual superconducting device (SIS) receiver for 500/800 GHz. The 1.2 m telescope produces a 2.2′ beam at 492 GHz and could map a molecular cloud entirely. It could also observe nearby galaxies in the CO (J=4–3), CO (J=7–6), [CI] (3P1–3P0), [CI] (3P2–3P1) and in continuum emission between 460–810 GHz.

Keywords

Site testingtelescopessub-millimeter
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S288: Astrophysics from Antarctica , August 2012 , pp. 251 - 255
Copyright
Copyright © International Astronomical Union 2013

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