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Phase referencing VLBI astrometry observation system: VERA

Published online by Cambridge University Press:  01 October 2007

H. Kobayashi ,
N. Kawaguchi ,
S. Manabe ,
K. M. Shibata ,
M. Honma ,
Y. Tamura ,
O. Kameya ,
T. Hirota ,
T. Jike  and
H. Imai
...Show all authors
H. Kobayashi
Affiliation:
Mizusawa VERA Observatory, National Astronomical Observatory of Japan
N. Kawaguchi
Affiliation:
Mizusawa VERA Observatory, National Astronomical Observatory of Japan
S. Manabe
Affiliation:
Mizusawa VERA Observatory, National Astronomical Observatory of Japan
K. M. Shibata
Affiliation:
Mizusawa VERA Observatory, National Astronomical Observatory of Japan
M. Honma
Affiliation:
Mizusawa VERA Observatory, National Astronomical Observatory of Japan
Y. Tamura
Affiliation:
Mizusawa VERA Observatory, National Astronomical Observatory of Japan
O. Kameya
Affiliation:
Mizusawa VERA Observatory, National Astronomical Observatory of Japan
T. Hirota
Affiliation:
Mizusawa VERA Observatory, National Astronomical Observatory of Japan
T. Jike
Affiliation:
Mizusawa VERA Observatory, National Astronomical Observatory of Japan
H. Imai
Affiliation:
Division of Astronomy, Department of Science, Kagoshima University email: hideyuki.kobayashi@nao.ac.jp
T. Omodaka
Affiliation:
Division of Astronomy, Department of Science, Kagoshima University email: hideyuki.kobayashi@nao.ac.jp
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Abstract

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VERA aims at astrometric observations using phase referencing VLBI techniques, whose goal is a 10 micro arc-second accuracy for annual parallax measurements. VERA has four 20-m diameter VLBI radio telescopes in Japanese archipelago with the maximum baseline length of 2,300 km. They have the two-beam observing system, which makes simultaneous observations of two objects possible. This leads to very accurate phase referencing VLBI observations. An important science goal is to make a 3-dimensional map of the Galaxy and reveal its dynamics. In order to achieve this, VERA has the 22GHz and 43GHz bands for H2O and SiO maser objects, respectively. Maser objects are compact and suitable for astrometry observations. VERA's construction was started in 2000 and the array became operational in 2004. We have already measured annual parallaxes and proper motions of some galactic objects. In the future, VERA will collaborate with Korean and Chinese VLBI stations.

Keywords

instrumentation: interferometersmasers
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S248: A Giant Step: from Milli- to Micro-arcsecond Astrometry , October 2007 , pp. 148 - 155
Copyright
Copyright © International Astronomical Union 2008

References

Choi, Y. K., et al. , 2008, in this volume p.192Google Scholar
Genzel, R., et al. , 1981, ApJ, 244, 884CrossRefGoogle Scholar
Loinard, L., et al. , 2008, in this volume p.186CrossRefGoogle Scholar
Hirota, T., et al. , 2007, PASJ, 59, 897CrossRefGoogle Scholar
Honma, M., et al. , 2003, PASJ, 55, L57CrossRefGoogle Scholar
Honma, M., et al. , 2007, PASJ, 59, 889CrossRefGoogle Scholar
Menten, K., et al. , 2007, A&A, 474, 515Google Scholar
Nakagawa, A., et al. , 2008, this volume p.206Google Scholar
Sandstrom, M., et al. , 2007, ApJ, 667, 1161CrossRefGoogle Scholar
Sato, M., et al. , 2007, PASJ, 59, 743CrossRefGoogle Scholar