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Astrometric VLBI Observations of the Galactic LPVs, Miras, and OH/IR stars

Published online by Cambridge University Press:  16 July 2018

Akiharu Nakagawa
Affiliation:
Kagoshima University, 1-21-35, Korimoto, Kagoshima-shi, Kagoshima, Japan email: nakagawa@sci.kagoshima-u.ac.jp
Tomoharu Kurayama
Affiliation:
Teikyo University of Science, 2-2-1 Sakuragi, Senjyu, Adachi-ku, Tokyo, Japan
Gabor Orosz
Affiliation:
Kagoshima University, 1-21-35, Korimoto, Kagoshima-shi, Kagoshima, Japan email: nakagawa@sci.kagoshima-u.ac.jp
Ross A. Burns
Affiliation:
Joint Institute for VLBI ERIC (JIVE), Postbus 2, 7990 AA Dwingeloo, the Netherlands
Tomoaki Oyama
Affiliation:
National Astronomical Observatory of Japan, Mizusawa VLBI Observatory, 2-12 Hoshigaoka-cho, Mizusawa-ku, Oshu, Iwate, Japan
Takumi Nagayama
Affiliation:
National Astronomical Observatory of Japan, Mizusawa VLBI Observatory, 2-12 Hoshigaoka-cho, Mizusawa-ku, Oshu, Iwate, Japan
Takashi Miyata
Affiliation:
Institute of Astronomy, The University of Tokyo, 2-21-1Osawa, Mitaka, Tokyo, Japan
Mamoru Sekido
Affiliation:
National Institute of Information and Communications Technology, Kashima Space Technology Center, 893-1 Hirai, Kashima, Ibaraki, Japan
Junichi Baba
Affiliation:
National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo, Japan
Kiichi Wada
Affiliation:
Kagoshima University, 1-21-35, Korimoto, Kagoshima-shi, Kagoshima, Japan email: nakagawa@sci.kagoshima-u.ac.jp
Corresponding
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Abstract

Studies of Galactic LPVs based on astrometric VLBI are presented. We use a VLBI array, “VERA”, to measure parallaxes and calibrate the K-band period luminosity relation (PLR) of the Galactic Miras. Since the PLR offers a distance indicator, its calibration is crucial to reveal their spatial distribution. Parallaxes of dozens of LPVs are presented. For the longer period stars, the mass-loss is high and the stars are obscured and recognized as OH/IR stars. We estimated mid-infrared absolute magnitudes of dozens of OH/IR stars and found that they show a loose concentration around −14 mag at λ of 11.6 μm, indicating an existence of PLR for OH/IR stars. Astrometry of OH/IR stars will also help us to study non-steady spiral arms as proposed from the latest simulation study of the galactic dynamics. We will start astrometric VLBI observation of two OH/IR stars NSV25875 and OH127.8+0.0 at 43 GHz with VERA.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2018 

References

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Astrometric VLBI Observations of the Galactic LPVs, Miras, and OH/IR stars
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