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SiO MASERS AROUND WX PSC MAPPED WITH THE KVN AND VERA ARRAY (KaVA)

  • Authors: Youngjoo Yun, Se-Hyung Cho, Hiroshi Imai, Jaeheon Kim, Yoshiharu Asaki, James O. Chibueze, Yoon Kyung Choi, Richard Dodson, Dong-Jin Kim, Kozue Kusuno, Naoko Matsumoto, Cheulhong Min, Miyako Oyadomari, María J. Rioja, Dong-Hwan Yoon, Do-Young Byun, Hyunsoo Chung, Moon-Hee Chung, Yoshiaki Hagiwara, Myoung-Hee Han, Seog-Tae Han, Tomoya Hirota, Mareki Honma, Jung-Wook Hwang, Do-Heung Je, Takaaki Jike, Dong-Kyu Jung, Taehyun Jung, Ji-Hyun Kang, Jiman Kang, Yong-Woo Kang, Yukitoshi Kan-ya, Masahiro Kanaguchi, Noriyuki Kawaguchi, Bong Gyu Kim, Hyo Ryoung Kim, Hyun-Goo Kim, Jongsoo Kim, Kee-Tae Kim, Mikyoung Kim, Hideyuki Kobayashi, Yusuke Kono, Tomoharu Kurayama, Changhoon Lee, Jeewon Lee, Jeong Ae Lee, Jung-Won Lee, Sang Hyun Lee, Sang-Sung Lee, A-Ran Lyo, Young Chol Minh, Chungsik Oh, Se-Jin Oh, Tomoaki Oyama, Duk-Gyoo Roh, Satoko Sawada-Satoh, Katsunori M. Shibata, Bong Won Sohn, Min-Gyu Song, Yoshiaki Tamura, Seog-Oh Wi, and Jae-Hwan Yeom

2016 The Astrophysical Journal 822 3.

  • Provider: AAS Journals

Caption: Figure 1.

Intensity variability of the v = 1 and v = 2 J = 1 → 0 SiO masers around WX Psc. Filled circles and open circles represent the single-dish observations of KVN, and the vertical dashed line corresponds to the time of this KaVA observation. The conversion factor for KVN is about 12 Jy K−1 at 43 GHz.

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