천문학회보 (The Bulletin of The Korean Astronomical Society)

한국천문학회 (The Korean Astronomical Society)
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Connection between the gamma-ray outbursts and the jet activity of BL Lacertae

  • Kim, Dae-Won (Department of Physics and Astronomy, Seoul National University) ;
  • Trippe, Sascha (Department of Physics and Astronomy, Seoul National University) ;
  • Park, Jong-Ho (Department of Physics and Astronomy, Seoul National University) ;
  • Oh, Jung-Hwan (Department of Physics and Astronomy, Seoul National University) ;
  • Lee, Tae-Seok (Department of Physics and Astronomy, Seoul National University) ;
  • Lee, Sang-Sung (Korea Astronomy and Space Science Institute) ;
  • Algaba, Juan-Carlos (Korea Astronomy and Space Science Institute) ;
  • Zhao, Guangyao (Korea Astronomy and Space Science Institute) ;
  • Kino, Motoki (Korea Astronomy and Space Science Institute) ;
  • Wajima, Kiyoaki (Korea Astronomy and Space Science Institute) ;
  • Kang, Sin-Cheol (Korea Astronomy and Space Science Institute) ;
  • Kim, Jae-Young (Department of Physics and Astronomy, Seoul National University)
  • 발행 : 2016.04.12
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초록

We present our observational results of BL Lacertae(2200+420) obtained at 22, 43, 86, and 129 GHz simultaneously during 27 months(2013.Jan ~ 2015.Mar) which includes their two gamma-ray outbursts(2013.Oct & 2015.Mar) to study a connection between the gamma-ray outbursts and the radio activity. We mainly use a Korean VLBI monitoring program, IMOGABA(Interferometric Monitoring Of Gamma-ray Bright AGNs) which is a monthly monitoring program with the KVN(Korean VLBI Network). Overall, our KVN image shows two components in the map, a stationary core at the center and one moving jet component to the south, but almost core only at 86, 129 GHz. The location of the moving jet component in the maps depend on the frequencies that 22, 43, 86, and 129 GHz. We have checked light curves, spectral index, kinematics, and radio structure to find differences before and after the gamma-ray outbursts, but there was no significant correlation. We also have derived a decay time scale of ~9 months for the major radio outburst by applying an exponential decay fitting.

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