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Parallax measurement of the Galactic Mira variables with VERA

Published online by Cambridge University Press:  01 October 2007

A. Nakagawa
Affiliation:
Faculty of Science, Kagoshima University, 1-21-35, Korimoto, Kagoshima, JAPAN email: nakagawa@astro.sci.kagoshima-u.ac.jp
T. Omodaka
Affiliation:
Faculty of Science, Kagoshima University, 1-21-35, Korimoto, Kagoshima, JAPAN email: nakagawa@astro.sci.kagoshima-u.ac.jp
K. M. Shibata
Affiliation:
National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo, JAPAN
T. Kurayama
Affiliation:
National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo, JAPAN
H. Imai
Affiliation:
Faculty of Science, Kagoshima University, 1-21-35, Korimoto, Kagoshima, JAPAN email: nakagawa@astro.sci.kagoshima-u.ac.jp
S. Kameno
Affiliation:
Faculty of Science, Kagoshima University, 1-21-35, Korimoto, Kagoshima, JAPAN email: nakagawa@astro.sci.kagoshima-u.ac.jp
M. Tsushima
Affiliation:
Faculty of Science, Kagoshima University, 1-21-35, Korimoto, Kagoshima, JAPAN email: nakagawa@astro.sci.kagoshima-u.ac.jp
N. Matsumoto
Affiliation:
Faculty of Science, Kagoshima University, 1-21-35, Korimoto, Kagoshima, JAPAN email: nakagawa@astro.sci.kagoshima-u.ac.jp
M. Matsui
Affiliation:
Faculty of Science, Kagoshima University, 1-21-35, Korimoto, Kagoshima, JAPAN email: nakagawa@astro.sci.kagoshima-u.ac.jp
Corresponding
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Abstract

Parallax measurements of the Galactic Mira variables with VERA have started since 2004 to establish their Period-Luminosity (PL) relationship in the Galaxy. Multi-epoch VLBI observations of a semiregular variable S Crt yielded an accurate parallax of 2.27±0.14 mas corresponding to the distance of 441+29−24 pc. In addition to the distance, we obtained physical properties of S Crt. Temperature of the photosphere was found to be ~3000 K by fitting the infrared spectrum with a blackbody radiation. The stellar radius was obtained based on the distance, apparent magnitude, and the temperature. Internal proper motions of circularly-arranged maser spots in S Crt were detected for the first time. Observations of the other Mira variables, such as R UMa, SY Scl, AP Lyn, and WX Psc are in progress.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2008

References

Feast, M. W., Glass, I. S., Whitelock, P. A., & Catchpole, R. M. 1989, MNRAS 241, 375CrossRefGoogle Scholar
van Leeuwen, F., Feast, M. W., Whitelock, P. A., & Yudin, B. 1997, MNRAS 287, 955CrossRefGoogle Scholar
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