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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

References

Dame, T. M., Ungerechts, H., Cohen, R., deAAAAGeus, E., Grenier, I., May, J., Murphy, D., Nyman, L., & Thaddeus, P. 1995, ApJ, 322, 706Google Scholar
Ishii, S., Seta, M., Nakai, N., Nagai, M., Miyagawa, N., Yamauchi, A., Motoyama, H., & Taguchi, M. 2010, Polar Science, 3, 213Google Scholar
Ishii, S., Seta, M., Nakai, N., Miyamoto, Y., Nagai, M., Maezawa, H., Nagasaki, T., Miyagawa, N., Motoyama, H., Sekimoto, Y., & Bronfman, L. 2012, 23rd Int. Symp. Space. THz Tech.Google Scholar
Okita, H. 2012, IAU Symposium 288Google Scholar
Sakamoto, S., Hasegawa, T., Handa, T., Hayashi, M., & Oka, T. 1997, ApJ, 486, 276CrossRefGoogle Scholar
Scoville, N. Z, Yun, M. S., Clements, D. P., Sanders, D. B., & Waller, W. H. 2003, ApJ Suppl., 63, 821Google Scholar
Sekimoto, Y., Yamamoto, S., Oka, T., Ikeda, M., Maezawa, H., Ito, T., Saito, G., Iwata, M., Kamegai, K., Sakai, T., Tatematsu, K., Arikawa, Y., Aso, Y., Noguchi, T., Maezawa, K., Shi, S., Saito, S., Ozeki, H., Fujiwara, H., Inatani, J., Ohishi, M., Noda, K., & Togashi, Y. 2000, Review of Scientific Instruments, 71, 7CrossRefGoogle Scholar
Watanabe, O., Kamiyama, K., Motoyama, H., Fujii, F., Shoji, H. & Satou, K 1999, East Antarctica, Annals of Glaciology, 29, 176Google Scholar
Yamanouchi, T., Hirasawa, N., Hayashi, M., Takahashi, S., & Kaneto, S. 2004, Mem. Natl. Inst. Polar Res. Spec. Issue, 94Google Scholar
Yang, H., Kulesa, C. A., Walker, C. K., Tothill, N. F. H., Yang, J., Ashley, M. C. B., Cui, X., Feng, L., Lawrence, J. S., Luong-van, D. M, McCaughrean, M. J., Storey, J. W. V., Wang, L., Zhou, X., & Zhu, Z. 2000, PASP, 122, 490Google Scholar