A1 Refereed original research article in a scientific journal
3C 66A: Variability in 2007-2015
Authors: Hagen-Thorn VA, Morozova DA, Arkharov AA, Hagen-Thorn EI, Troitsky IS, Troitskaya YV, Milanova YV, Volkov EV, Takalo LO, Sillanpää A
Publisher: MAIK NAUKA/INTERPERIODICA/SPRINGER
Publication year: 2017
Journal: Astronomicheskii Zhurnal / Astronomy Reports
Journal name in source: ASTRONOMY REPORTS
Journal acronym: ASTRON REP+
Volume: 61
Issue: 6
First page : 503
Last page: 512
Number of pages: 10
ISSN: 1063-7729
eISSN: 1562-6881
DOI: https://doi.org/10.1134/S1063772917060051
Abstract
The results of photometric (BV RIJHK) and polarimetric (R)monitoring of the blazar 3C 66A performed at the St. Petersburg State University and the Central AstronomicalObservatory of the Russian Academy of Sciences in 2007-2015, radio observations performed by the Boston University team with the Very Long Baseline Array at 43 GHz, and a gamma-ray light curve based on observations with the Fermi SpaceObservatory are presented. Color variations of the object are studied. Changes in the optical spectral energy distribution are observed at some times, indicating the appearance and disappearance of individual variable sources. A variable source with a degree of polarization of 36% is identified, which is responsible for the polarization variations observed during one episode. The correlations between the variations in the different spectral ranges indicate that the optical and gamma-ray radiation originates near the radio core detected at 43 GHz. The presence of five superluminal components emerging from the core is detected.
The results of photometric (BV RIJHK) and polarimetric (R)monitoring of the blazar 3C 66A performed at the St. Petersburg State University and the Central AstronomicalObservatory of the Russian Academy of Sciences in 2007-2015, radio observations performed by the Boston University team with the Very Long Baseline Array at 43 GHz, and a gamma-ray light curve based on observations with the Fermi SpaceObservatory are presented. Color variations of the object are studied. Changes in the optical spectral energy distribution are observed at some times, indicating the appearance and disappearance of individual variable sources. A variable source with a degree of polarization of 36% is identified, which is responsible for the polarization variations observed during one episode. The correlations between the variations in the different spectral ranges indicate that the optical and gamma-ray radiation originates near the radio core detected at 43 GHz. The presence of five superluminal components emerging from the core is detected.
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