Superluminal Motion and Jet Parameters in the High-Redshift Blazar J1429+5406

TL;DR

This study analyzes the relativistic jet of the high-redshift blazar J1429+5406 over two decades, revealing superluminal motion, jet parameters, and confirming its blazar nature through high-resolution radio observations.

Contribution

It provides the first detailed kinematic analysis of a z>3 blazar's jet, measuring proper motions and jet parameters with VLBI over 24 years, including the fastest known jet component at this redshift.

Findings

Inner jet components show significant proper motion.

Outer jet components are stationary within measurement limits.

Jet is highly Doppler-boosted with a low inclination angle.

Abstract

We investigate the relativistic jet of the powerful radio-emitting blazar J1429+5406 at redshift z=3.015. Our understanding of jet kinematics in z>3 quasars is still rather limited, based on a sample of less than about 50 objects. The blazar J1429+5406 was observed at a high angular resolution using the method of very long baseline interferometry over more than two decades, between 1994 and 2018. These observations were conducted at five radio frequencies, covering a wide range from 1.7 to 15 GHz. The outer jet components at ~20-40 milliarcsecond (mas) separations from the core do not show discernible apparent motion. On the other hand, three jet components within the central 10 mas region exhibit significant proper motion in the range of (0.045-0.16)mas/year, including one that is among the fastest-moving jet components at z>3 known to date. Based on the proper motion of the innermost jet component and the measured brightness temperature of the core, we estimated the Doppler factor, the bulk Lorentz factor, and the inclination angle of the jet with respect to the line of sight. The core brightness temperature is at least 3.6 x 10^{11} K, well exceeding the equipartition limit, indicating Doppler-boosted radio emission. The low jet inclination (<5.4 deg) firmly places J1429+5406 into the blazar category.