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arxiv: 1711.03983 · v1 · pith:MAKBWPMMnew · submitted 2017-11-10 · 🌌 astro-ph.GA · astro-ph.HE

Kinematics of Parsec-Scale Jets of Gamma-Ray Blazars at 43~GHz within the VLBA-BU-BLAZAR Program

Svetlana G. Jorstad , Alan P. Marscher , Daria A. Morozova , Ivan S. Troitsky , Iv\'an Agudo , Carolina Casadio , Adi Foord , Jos\'e L. G\'omez
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Nicholas R. MacDonald Sol N. Molina Anne L\"ahteenm\"aki Joni Tammi Merja Tornikoski
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classification 🌌 astro-ph.GA astro-ph.HE
keywords knotscorebllacsquasarsvaluesangleanglesapparent
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We analyze the parsec-scale jet kinematics from 2007 June to 2013 January of a sample of $\gamma$-ray bright blazars monitored roughly monthly with the Very Long Baseline Array at 43~GHz. In a total of 1929 images, we measure apparent speeds of 252 emission knots in 21 quasars, 12 BL~Lacertae objects (BLLacs), and 3 radio galaxies, ranging from 0.02$c$ to 78$c$; 21\% of the knots are quasi-stationary. Approximately 1/3 of the moving knots execute non-ballistic motions, with the quasars exhibiting acceleration along the jet within 5~pc (projected) of the core, and knots in the BLLacs tending to decelerate near the core. Using apparent speeds of components and timescales of variability from their light curves, we derive physical parameters of 120 superluminal knots, including variability Doppler factors, Lorentz factors, and viewing angles. We estimate the half-opening angle of each jet based on the projected opening angle and scatter of intrinsic viewing angles of knots. We determine characteristic values of physical parameters for each jet and AGN class based on the range of values obtained for individual features. We calculate intrinsic brightness temperatures of the cores, $T_{\rm b,int}^{\rm core}$, at all epochs, finding that the radio galaxies usually maintain equipartition conditions in the cores, while $\sim$30\% of $T_{\rm b,int}^{\rm core}$ measurements in the quasars and BLLacs deviate from equipartition values by a factor $>$10. This probably occurs during transient events connected with active states. In the Appendix we briefly describe the behavior of each blazar during the period analyzed.

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