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VLBI monitoring of Mira variables with VERA

Published online by Cambridge University Press:  01 March 2007

A. Nakagawa ,
T. Omodaka ,
K. M. Shibata ,
T. Kurayama ,
H. Imai ,
S. Kameno ,
M. Tsushima ,
M. Shintani ,
N. Matsumoto  and
M. Matsui
...Show all authors
A. Nakagawa
Affiliation:
Faculty of science, Kagoshima University, 1-21-35, Korimoto, Kagoshima, 890-0065, JAPAN email:[email protected]
T. Omodaka
Affiliation:
Faculty of science, Kagoshima University, 1-21-35, Korimoto, Kagoshima, 890-0065, JAPAN email:[email protected]
K. M. Shibata
Affiliation:
Mizusawa VERA observatory, National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo, 181-8588, JAPAN
T. Kurayama
Affiliation:
Mizusawa VERA observatory, National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo, 181-8588, JAPAN
H. Imai
Affiliation:
Faculty of science, Kagoshima University, 1-21-35, Korimoto, Kagoshima, 890-0065, JAPAN email:[email protected]
S. Kameno
Affiliation:
Faculty of science, Kagoshima University, 1-21-35, Korimoto, Kagoshima, 890-0065, JAPAN email:[email protected]
M. Tsushima
Affiliation:
Faculty of science, Kagoshima University, 1-21-35, Korimoto, Kagoshima, 890-0065, JAPAN email:[email protected]
M. Shintani
Affiliation:
Faculty of science, Kagoshima University, 1-21-35, Korimoto, Kagoshima, 890-0065, JAPAN email:[email protected]
N. Matsumoto
Affiliation:
Faculty of science, Kagoshima University, 1-21-35, Korimoto, Kagoshima, 890-0065, JAPAN email:[email protected]
M. Matsui
Affiliation:
Faculty of science, Kagoshima University, 1-21-35, Korimoto, Kagoshima, 890-0065, JAPAN email:[email protected]
S. Oizumi
Affiliation:
Faculty of science, Kagoshima University, 1-21-35, Korimoto, Kagoshima, 890-0065, JAPAN email:[email protected]
T. Yasuda
Affiliation:
Faculty of science, Kagoshima University, 1-21-35, Korimoto, Kagoshima, 890-0065, JAPAN email:[email protected]
Y. Arao
Affiliation:
Faculty of science, Kagoshima University, 1-21-35, Korimoto, Kagoshima, 890-0065, JAPAN email:[email protected]
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Abstract

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We have started a VLBI monitoring program for Asymptotic Giant Branch (AGB) stars at 22 and 43 GHz as part of a project of the VLBI Exploration of Radio Astrometry (VERA) for precisely obtaining the period-luminosity (PL) relation of Galactic Mira variables. Using accurate distances measured with VERA, we reveal PL relation in the Galaxy based on the absolute magnitudes of the sources. We selected the sources for VLBI monitoring so that they have a good coverage of various pulsation periods. Photometry in the infrared J, H, and K bands for over 600 AGB stars has also started since 2003 with the 1m telescope of Kagoshima University to obtain the pulsation periods and magnitudes. Current analysis of the phase referencing VLBI observations of S Crt shows that the parallax of 2.3±0.2 milliarcsec (mas) corresponds to a distance of 435+41−35 pc. From the infrared monitoring data, pulsation periods and magnitudes in K band for 248 sources were obtained.

Keywords

astrometrymasersAGB and post-AGBinterferometricphotometric
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S242: Astrophysical Masers and their Environments , March 2007 , pp. 326 - 327
Copyright
Copyright © International Astronomical Union 2008

References

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