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Scientific goals of Nano-JASMINE

Published online by Cambridge University Press:  26 February 2013

Yoshiyuki Yamada ,
Sho Fujita ,
Naoteru Gouda ,
Yukiyasu Kobayashi ,
Takuji Hara ,
Ryoichi Nishi ,
Satoshi Yoshioka ,
Shunsuke Hozumi  and
the JASMINE Working Group
Yoshiyuki Yamada
Affiliation:
Department of Physics, Faculty of Science, Kyoto University, Sakyo-ku, Kyoto 606-8502, Japan email: [email protected]
Sho Fujita
Affiliation:
Department of Physics, Faculty of Science, Kyoto University, Sakyo-ku, Kyoto 606-8502, Japan email: [email protected]
Naoteru Gouda
Affiliation:
JASMINE Project Office, National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
Yukiyasu Kobayashi
Affiliation:
JASMINE Project Office, National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
Takuji Hara
Affiliation:
JASMINE Project Office, National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan Department of Astronomy, School of Science, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan
Ryoichi Nishi
Affiliation:
Department of Physics, Niigata University, 8050 Ikarashi-2, Niigata 950-2181, Japan
Satoshi Yoshioka
Affiliation:
Department of Marine Electronics and Mechanical Engineering, Tokyo University of Marine Science and Technology, 2-1-6 Ecchu-Jima, Koto-ku, Tokyo 135-8533, Japan
Shunsuke Hozumi
Affiliation:
Faculty of Education, Shiga University, 2-5-1 Hiratsu, Otsu, Shiga 520-0862, Japan
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Abstract

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Nano-JASMINE is an ultrasmall Japanese satellite (with a weight of 35 kg), designed to carry out an astrometric mission. The target accuracy is 3 milliarcseconds (mas) for stars brighter than magnitude 7.5 at zw-band wavelengths of 0.6–1.0 μm. The observational strategy is the same as that of Gaia and Hipparcos. The time span of 20 years since the Hipparcos mission will enable us to update the proper motion data obtained at that time. With the help of these updated measurements, we expect that some stars will be resolved into multiple stars. In addition, taking advantage of the small primary mirror (with a diameter of 5 cm), we can measure bright stars which cannot be observed with Gaia because of saturation limits. The core data reduction for the Nano-JASMINE mission will use Gaia's Astrometric Global Iterative Solution (agis). A collaboration between the Gaiaagis and Nano-JASMINE teams was initiated in 2007.

Keywords

astrometry
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S289: Advancing the Physics of Cosmic Distances , August 2012 , pp. 429 - 432
Copyright
Copyright © International Astronomical Union 2013

References

Yamada, Y., Hara, T., Yoshioka, S., et al. 2012, ASP Conf. Ser., 461, 585Google Scholar