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VLBI monitoring of Mira variables with VERA

  • A. Nakagawa (a1), T. Omodaka (a1), K. M. Shibata (a2), T. Kurayama (a2), H. Imai (a1), S. Kameno (a1), M. Tsushima (a1), M. Shintani (a1), N. Matsumoto (a1), M. Matsui (a1), S. Oizumi (a1), T. Yasuda (a1), Y. Arao (a1) and the VERA project (a2)...

Abstract

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.

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References

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Bowers, P. F., & Johnston, K. J. 1994, ApJS 92, 189
Feast, M. W., Glass, I. S., Whitelock, P. A., & Catchpole, R. M. 1989, MNRAS 241, 375
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Keywords

VLBI monitoring of Mira variables with VERA

  • A. Nakagawa (a1), T. Omodaka (a1), K. M. Shibata (a2), T. Kurayama (a2), H. Imai (a1), S. Kameno (a1), M. Tsushima (a1), M. Shintani (a1), N. Matsumoto (a1), M. Matsui (a1), S. Oizumi (a1), T. Yasuda (a1), Y. Arao (a1) and the VERA project (a2)...

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