Causal connection in parsec-scale relativistic jets: results from the MOJAVE VLBI survey

TL;DR

This study demonstrates that AGN jets are causally connected on parsec scales by measuring the product of Lorentz factor and intrinsic opening angle, revealing differences from GRB jets and enabling estimation of jet beaming parameters.

Contribution

Introduces a new method to measure Gamma*theta_j from VLBA data, confirming causal connection in AGN jets and contrasting with GRB jets.

Findings

AGN jets have Gamma*theta_j ≈ 0.2, indicating causal connection.

Jets viewed close to the line of sight have smaller intrinsic opening angles.

GRB jets have much higher Gamma*theta_j, suggesting different physics.

Abstract

We report that active galactic nucleus (AGN) jets are causally connected on parsec scales, based on 15 GHz Very Long Baseline Array (VLBA) data from a sample of 133 AGN jets. This result is achieved through a new method for measuring the product of the jet Lorentz factor and the intrinsic opening angle Gamma*theta_j from measured apparent opening angles in flux density limited samples of AGN jets. The Gamma*theta_j parameter is important for jet physics because it is related to the jet-frame sidewise expansion speed and causal connection between the jet edges and its symmetry axis. Most importantly, the standard model of jet production requires that the jet be causally connected with its symmetry axis, implying that Gamma*theta_j < 1. When we apply our method to the MOJAVE flux density limited sample of radio loud objects, we find Gamma*theta_j = 0.2, implying that AGN jets are causally connected. We also find evidence that AGN jets viewed very close to the line of sight effectively have smaller intrinsic opening angles compared with jets viewed more off-axis, which is consistent with Doppler beaming and a fast inner spine/slow outer sheath velocity field. Notably, gamma-ray burst (GRB) jets have a typical Gamma*theta_j that is two orders of magnitude higher, suggesting that different physical mechanisms are at work in GRB jets compared to AGN jets. A useful application of our result is that a jet's beaming parameters can be derived. Assuming Gamma*theta_j is approximately constant in the AGN jet population, an individual jet's Doppler factor and Lorentz factor (and therefore also its viewing angle) can be determined using two observable quantities: apparent jet opening angle and the apparent speed of jet components.