First mm-VLBI Observations between the TRAO 14-m and the NRO 45-m Telescopes: Observations of 86 GHz SiO Masers in VY Canis Majoris-猫眼课题宝

DOI：

10.1093/pasj/56.3.475

发表时间：

2004-06

期刊：

Publications of the Astronomical Society of Japan

影响因子：

2.3

通讯作者：

中科院分区：

物理与天体物理4区

文献类型：

作者：

K. Shibata;H. Chung;S. Kameno;D. Roh;T. Umemoto;Kwang-Dong Kim;K. Asada;Seog-Tae Han;N. Mochizuki;Se-Hyung Cho;S. Sawada-Satoh;Hyun-Goo Kim;T. Bushimata;Y. Minh;T. Miyaji;N. Kuno;H. Mikoshiba;K. Sunada;M. Inoue;H. Kobayashi

我们利用韩国和日本之间1000公里的基线在86 GHz进行了VLBI观测，并于2001年6月成功地探测到了VY CMA和猎户座KL的SiO v=1，J=2-1脉泽辐射。这是这一基线的第一次VLBI结果，也是韩国望远镜的第一次天文VLBI观测。从那时起，我们在2002年1月和2003年2月观测了VY CMA的SiO v=1，J=2-1脉泽辐射，并得出了脉泽辐射的分布。我们的结果表明，脉泽辐射超过2-4个恒星半径，并且在尘埃壳的内径范围内。我们观测到了其他SiO脉泽源和连续谱源，并从三个连续谱源中探测到了86 GHz的连续谱发射。经验证，该基线具有与VLBA和CMVA中最敏感的基线相当的性能，并能够通过监测观测来研究星周包层中脉泽特征的自行。

We have made VLBI observations at 86GHz using a 1000-km baseline between Korea and Japan with successful detections of SiO v =1 ,J = 2–1 maser emissions from VY CMa and Orion KL in 2001 June. This was the first VLBI result for this baseline and the first astronomical VLBI observation for the Korean telescope. Since then, we observed SiO v =1 ,J = 2–1 maser emission in VY CMa in 2002 January and 2003 February and derived the distributions of the maser emissions. Our results show that the maser emissions extend over 2–4 stellar radii, and were within the inner radius of the dust shell. We observed other SiO maser sources and continuum sources, and 86-GHz continuum emissions were detected from three continuum sources. It was verified that this baseline has a performance comparable to the most sensitive baseline in the VLBA and the CMVA, and is capable of investigating the proper motions of maser features in circumstellar envelopes using monitoring observations.

First mm-VLBI Observations between the TRAO 14-m and the NRO 45-m Telescopes: Observations of 86 GHz SiO Masers in VY Canis Majoris

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