The extreme blazar AO 0235+164 as seen by extensive ground and space radio observations

TL;DR

This study uses multi-frequency radio observations, including space VLBI, to analyze the ultra-compact blazar AO 0235+164, revealing extreme brightness temperatures, jet structure, and physical conditions in the core region.

Contribution

It provides new insights into the ultra-compact structure and physical parameters of AO 0235+164 using extensive ground and space radio observations, including visibility modeling and Gaussian process regression.

Findings

Brightness temperature up to 10^14 K in the core.

Detection of ultra-compact features less than 10 μas.

Jet structure shows a bend and collimation within 1.5 mas.

Abstract

Clues to the physical conditions in radio cores of blazars come from measurements of brightness temperatures as well as effects produced by intrinsic opacity. We study the properties of the ultra compact blazar AO 0235+164 with RadioAstron ground-space radio interferometer, multi-frequency VLBA, EVN and single-dish radio observations. We employ visibility modeling and image stacking for deriving structure and kinematics of the source, and use Gaussian process regression to find the relative multi-band time delays of the flares. The multi-frequency core size and time lags support prevailing synchrotron self absorption. The intrinsic brightness temperature of the core derived from ground-based VLBI is close to the equipartition regime value. In the same time, there is evidence for ultra-compact features of the size of less than 10 $\mu$as in the source, which might be responsible for the extreme apparent brightness temperatures of up to $10^{14}$ K as measured by RadioAstron. In 2007--2016 the VLBI components in the source at 43 GHz are found predominantly in two directions, suggesting a bend of the outflow from southern to northern direction. The apparent opening angle of the jet seen in the stacked image at 43 GHz is two times wider than that at 15 GHz, indicating a collimation of the flow within the central 1.5 mas. We estimate the Lorentz factor $\Gamma = 14$, the Doppler factor $\delta=21$, and the viewing angle $\theta = 1.7^\circ$ of the apparent jet base, derive the gradients of magnetic field strength and electron density in the outflow, and the distance between jet apex and the core at each frequency.