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http://dx.doi.org/10.5303/JKAS.2015.48.5.237

INTERFEROMETRIC MONITORING OF GAMMA–RAY BRIGHT ACTIVE GALACTIC NUCLEI II: FREQUENCY PHASE TRANSFER  

ALGABA, JUAN-CARLOS (Korea Astronomy and Space Science Institute)
ZHAO, GUANG-YAO (Korea Astronomy and Space Science Institute)
LEE, SANG-SUNG (Korea Astronomy and Space Science Institute)
BYUN, DO-YOUNG (Korea Astronomy and Space Science Institute)
KANG, SIN-CHEOL (Korea Astronomy and Space Science Institute)
KIM, DAE-WON (Department of Physics and Astronomy, Seoul National University)
KIM, JAE-YOUNG (Department of Physics and Astronomy, Seoul National University)
KIM, JEONG-SOOK (National Astronomical Observatory of Japan)
KIM, SOON-WOOK (Korea Astronomy and Space Science Institute)
KINO, MOTOKI (Korea Astronomy and Space Science Institute)
MIYAZAKI, ATSUSHI (Korea Astronomy and Space Science Institute)
PARK, JONG-HO (Department of Physics and Astronomy, Seoul National University)
TRIPPE, SASCHA (Department of Physics and Astronomy, Seoul National University)
WAJIMA, KIYOAKI (Korea Astronomy and Space Science Institute)
Publication Information
Journal of The Korean Astronomical Society / v.48, no.5, 2015 , pp. 237-255 More about this Journal
Abstract
The Interferometric Monitoring of Gamma–ray Bright Active galactic nuclei (iMOGABA) program provides not only simultaneous multifrequency observations of bright gamma–ray detected active galactic nuclei (AGN), but also covers the highest Very Large Baseline Interferometry (VLBI) frequencies ever being systematically monitored, up to 129 GHz. However, observation and imaging of weak sources at the highest observed frequencies is very challenging. In the second paper in this series, we evaluate the viability of the frequency phase transfer technique to iMOGABA in order to obtain larger coherence time at the higher frequencies of this program (86 and 129 GHz) and image additional sources that were not detected using standard techniques. We find that this method is applicable to the iMOGABA program even under non–optimal weather conditions.
Keywords
galaxies: active; methods: data analysis; techniques: high angular resolution; techniques: interferometric;
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