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A study on evolved stars by simultaneous observations of H2O and SiO masers using KVN

Published online by Cambridge University Press:  16 July 2018

Se-Hyung Cho
Affiliation:
Korea Astronomy and Space Science Institute, 776, Daedukdae-ro, Yuseong-gu, Daejeon, 34055, Republic of Korea email: cho@kasi.re.kr
Youngjoo Yun
Affiliation:
Korea Astronomy and Space Science Institute, 776, Daedukdae-ro, Yuseong-gu, Daejeon, 34055, Republic of Korea email: cho@kasi.re.kr
Jaeheon Kim
Affiliation:
Shanghai Astronomical Observatory, Chinese Academy of Sciences, China
Dong-Hwan Yoon
Affiliation:
Korea Astronomy and Space Science Institute, 776, Daedukdae-ro, Yuseong-gu, Daejeon, 34055, Republic of Korea email: cho@kasi.re.kr
Dong-Jin Kim
Affiliation:
Korea Astronomy and Space Science Institute, 776, Daedukdae-ro, Yuseong-gu, Daejeon, 34055, Republic of Korea email: cho@kasi.re.kr Department of Astronomy, Yonsei University, Republic of Korea
Yoon Kyung Choi
Affiliation:
Korea Astronomy and Space Science Institute, 776, Daedukdae-ro, Yuseong-gu, Daejeon, 34055, Republic of Korea email: cho@kasi.re.kr
Richard Dodson
Affiliation:
International Center for Radio Astronomy Research, The University of Western Australia, Australia
María Rioja
Affiliation:
International Center for Radio Astronomy Research, The University of Western Australia, Australia
Hiroshi Imai
Affiliation:
Department of Physics and Astronomy, Kagoshima University, Japan
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Abstract

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The Korean VLBI Network (KVN) is a unique millimeter VLBI system which is consisted of three 21 m telescopes with relatively short baselines. We present the preliminary results of simultaneous monitoring observations of the 22.2 GHz H2O and 43.1/42.8/86.2/129.3 GHz SiO masers based on the KVN Key Science Project (KSP). We obtained the astrometrically registered maps of the H2O and SiO masers toward nine evolved stars using the source frequency phase referencing method (SFPR). The SFPR maps of the H2O and SiO masers enabled us to investigate the spatial structure and kinematics from the SiO to H2O maser regions including the development of an outward motion from the ring-like or elliptical structures of SiO masers to the asymmetric structures of the 22.2 GHz H2O maser features. In particular, the 86.2/129.3 GHz SiO (v=1, J=2–1 and J=3–2) masers were clearly imaged toward several objects for the first time. The SiO v=1, J=3–2 maser shows different distributions compared to those of the SiO v=1, 2, J=1–0 and v=1, J=2–1 masers implying a different physical condition.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2018 

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