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Maser astrometry with VERA and Galactic structure

Published online by Cambridge University Press:  24 July 2012

Mareki Honma ,
Takumi Nagayama ,
Tomoya Hirota ,
Naoko Matsumoto ,
Nobuyuki Sakai  and
Noriyuki Kawaguchi
Mareki Honma
Affiliation:
Mizusawa VLBI observatory, NAOJ, Osawa, Mitaka, Tokyo, 181-8588, Japan email: [email protected] Department of Astronomical Science, School of Physical Sciences, The Graduate University of Advanced Studies (Sokendai), Osawa, Mitaka, Tokyo, 181-8588, Japan
Takumi Nagayama
Affiliation:
Mizusawa VLBI observatory, NAOJ, Osawa, Mitaka, Tokyo, 181-8588, Japan email: [email protected]
Tomoya Hirota
Affiliation:
Mizusawa VLBI observatory, NAOJ, Osawa, Mitaka, Tokyo, 181-8588, Japan email: [email protected] Department of Astronomical Science, School of Physical Sciences, The Graduate University of Advanced Studies (Sokendai), Osawa, Mitaka, Tokyo, 181-8588, Japan
Naoko Matsumoto
Affiliation:
Mizusawa VLBI observatory, NAOJ, Osawa, Mitaka, Tokyo, 181-8588, Japan email: [email protected]
Nobuyuki Sakai
Affiliation:
Mizusawa VLBI observatory, NAOJ, Osawa, Mitaka, Tokyo, 181-8588, Japan email: [email protected] Department of Astronomical Science, School of Physical Sciences, The Graduate University of Advanced Studies (Sokendai), Osawa, Mitaka, Tokyo, 181-8588, Japan
Noriyuki Kawaguchi
Affiliation:
Mizusawa VLBI observatory, NAOJ, Osawa, Mitaka, Tokyo, 181-8588, Japan email: [email protected] Department of Astronomical Science, School of Physical Sciences, The Graduate University of Advanced Studies (Sokendai), Osawa, Mitaka, Tokyo, 181-8588, Japan
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Abstract

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Since 2007 VERA (VLBI Exploration of Radio Astrometry) has been producing astrometric results (distances and/or proper motions) for Galactic maser sources. Nearly 30 parallaxes have been obtained for star-forming regions and late-type stars. By using VERA's astrometric results for star-forming regions, combined with those obtained with VLBA and EVN, fundamental Galactic parameters and Galactic structure may be derived. Our results show that R0 = 8.4 ± 0.4 kpc and Ω⊙ ≡ Ω0 + V⊙/R0=30.7±0.8 km s−1 kpc−1, and also show that the rotation curve of the Galaxy is nearly flat. The determinations of Galactic parameters and structures demonstrate that the maser astrometry can not only contribute significantly to research of individual maser sources, but also to studies of the structure of the Galaxy.

Keywords

maserastrometryVERAthe Galaxy
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S287: Cosmic Masers - from OH to H0 , January 2012 , pp. 386 - 390
Copyright
Copyright © International Astronomical Union 2012

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