TY - JOUR
T1 - The VLBI Monitoring Project for 6.7 GHz Methanol Masers Using the JVN/EAVN
AU - Sugiyama, Koichiro
AU - Fujisawa, Kenta
AU - Hachisuka, Kazuya
AU - Yonekura, Yoshinori
AU - Motogi, Kazuhito
AU - Sawada-Satoh, Satoko
AU - Matsumoto, Naoko
AU - Saito, Yu
AU - Hirano, Daiki
AU - Hayashi, Kyonosuke
AU - Shen, Zhi Qiang
AU - Honma, Mareki
AU - Hirota, Tomoya
AU - Murata, Yasuhiro
AU - Doi, Akihiro
AU - Niinuma, Kotaro
AU - Dodson, Richard
AU - Rioja, Maria
AU - Ellingsen, Simon
AU - Chen, Xi
AU - Kim, Kee Tae
AU - Ogawa, Hideo
PY - 2015/9
Y1 - 2015/9
N2 - We have initiated a Very Long Baseline Interferometer (VLBI) monitoring project of 36 methanol maser sources at 6.7 GHz using the Japanese VLBI Network (JVN) and East-Asian VLBI Network (EAVN), starting in August 2010. The purpose of this project is to systematically reveal 3-dimensional (3-D) kinematics of rotating disks around forming high-mass protostars. As an initial result, we present proper motion detections for two methanol maser sources showing an elliptical spatial morphology, G 002.53+00.19 and G 006.79-00.25, which could be the best candidates associated with the disk. The detected proper motions indicate a simple rotation in G 002.53+00.19 and rotation with expansion in G 006.79-00.25, respectively, on the basis of disk model fits with rotating and expanding components. The expanding motions might be caused by the magnetic-centrifugal wind on the disk.
AB - We have initiated a Very Long Baseline Interferometer (VLBI) monitoring project of 36 methanol maser sources at 6.7 GHz using the Japanese VLBI Network (JVN) and East-Asian VLBI Network (EAVN), starting in August 2010. The purpose of this project is to systematically reveal 3-dimensional (3-D) kinematics of rotating disks around forming high-mass protostars. As an initial result, we present proper motion detections for two methanol maser sources showing an elliptical spatial morphology, G 002.53+00.19 and G 006.79-00.25, which could be the best candidates associated with the disk. The detected proper motions indicate a simple rotation in G 002.53+00.19 and rotation with expansion in G 006.79-00.25, respectively, on the basis of disk model fits with rotating and expanding components. The expanding motions might be caused by the magnetic-centrifugal wind on the disk.
U2 - 10.5303/PKAS.2015.30.2.645
DO - 10.5303/PKAS.2015.30.2.645
M3 - Article
SN - 1225-1534
VL - 30
SP - 645
EP - 647
JO - Publications of The Korean Astronomical Society
JF - Publications of The Korean Astronomical Society
IS - 2
ER -