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VLBI observations of bright AGN jets with KVN and VERA Array (KaVA): Evaluation of Imaging Capability

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arxiv 1406.4356 v1 pith:STJ5ZMHH submitted 2014-06-17 astro-ph.IM astro-ph.HE

VLBI observations of bright AGN jets with KVN and VERA Array (KaVA): Evaluation of Imaging Capability

Kotaro Niinuma , Sang-Sung Lee , Motoki Kino , Bong Won Sohn , Kazunori Akiyama , Guang-Yao Zhao , Satoko Sawada-Satoh , Sascha Trippe
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Kazuhiro Hada Taehyun Jung Yoshiaki Hagiwara Richard Dodson Shoko Koyama Mareki Honma Hiroshi Nagai Aeree Chung Akihiro Doi Kenta Fujisawa Myoung-Hee Han Joeng-Sook Kim Jeewon Lee Jeong Ae Lee Atsushi Miyazaki Tomoaki Oyama Kazuo Sorai Kiyoaki Wajima Jaehan Bae Do-Young Byun Se-Hyung Cho Yoon Kyung Choi Hyunsoo Chung Moon-Hee Chung Seog-Tae Han Tomoya Hirota Jung-Wook Hwang Do-Heung Je Takaaki Jike Dong-Kyu Jung Jin-Seung 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 Jaeheon Kim Jongsoo Kim Kee-Tae Kim Mikyoung Kim Hideyuki Kobayashi Yusuke Kono Tomoharu Kurayama Changhoon Lee Jung-Won Lee Sang Hyun Lee Young Chol Minh Naoko Matsumoto Akiharu Nakagawa Chung Sik Oh Se-Jin Oh Sun-Youp Park Duk-Gyoo Roh Tetsuo Sasao Katsunori M. Shibata Min-Gyu Song Yoshiaki Tamura Seog-Oh Wi Jae-Hwan Yeom Young Joo Yun
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The Korean very-long-baseline interferometry (VLBI) network (KVN) and VLBI Exploration of Radio Astrometry (VERA) Array (KaVA) is the first international VLBI array dedicated to high-frequency (23 and 43 GHz bands) observations in East Asia. Here, we report the first imaging observations of three bright active galactic nuclei (AGNs) known for their complex morphologies: 4C 39.25, 3C 273, and M 87. This is one of the initial result of KaVA early science. Our KaVA images reveal extended outflows with complex substructure such as knots and limb brightening, in agreement with previous Very Long Baseline Array (VLBA) observations. Angular resolutions are better than 1.4 and 0.8 milliarcsecond at 23 GHz and 43 GHz, respectively. KaVA achieves a high dynamic range of ~1000, more than three times the value achieved by VERA. We conclude that KaVA is a powerful array with a great potential for the study of AGN outflows, at least comparable to the best existing radio interferometric arrays.

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