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In March 2018, Mukherjee (2018) reported the detection by VERITAS ofvery-high-energy emission (VHE; > 100 GeV) from 3C 264. This is the sixth, andsecond most distant, radio galaxy ever detected in the TeV regime. In thisarticle we present a radio and X-ray analysis of the jet in 3C 264. Wedetermine the main physical parameters of the parsec-scale flow and explore theimplications of the inferred kinematic structure for radiative models of thisgamma-ray emitting jet. The radio data set is comprised of VLBI observations at15 GHz from the MOJAVE program, and cover a time period of ~2 years. Through asegmented wavelet decomposition method we estimate the apparent displacement ofindividual plasma features; we then perform a pixel-based analysis of thestacked image to determine the jet shape. The X-ray data set includes allavailable observations from the Chandra, XMM, and Swift satellites, and isused, together with archival data in the other bands, to build the SED. Propermotion is mostly detected along the edges of the flow, which appears stronglylimb-brightened. The apparent speeds increase as a function of distance fromthe core up to a maximum of ~$11.5$ c. This constrains the jet viewing angle toassume relatively small values ($\theta\lesssim10^{\circ}$). In theacceleration region, extending up to a de-projected distance of~$4.8\times10^4$ Schwarzschild radii (~$11$ pc), the jet is collimating($r\propto z^{0.40\pm 0.04}$), as predicted for a magnetically-driven plasmaflow. By assuming that the core region is indeed magnetically dominated($U_B/U_e>1$), the SED and the jet power can be well reproduced in theframework of leptonic models, provided that the high-energy component isassociated to a second emitting region. The possibility that this region islocated at the end of the acceleration zone, either in the jet layer or in thespine, is explored in the modeling.

The TeV-emitting radio galaxy 3C 264. VLBI kinematics and SED modeling