Radio astrometry with chromatic AGN core positions

TL;DR

This paper investigates how frequency-dependent core-shifts in AGN affect radio VLBI astrometry, revealing that phase and group-delay measurements can yield different source positions, which is crucial for future high-precision astrometric comparisons.

Contribution

It introduces a power-law model for core-shifts based on observations and theory, and analyzes their impact on VLBI astrometry measurements, especially for future high-accuracy applications.

Findings

Phase and group-delay positions differ in the presence of core-shifts.

For beta=1, group delays measure the jet base position, not the core shift.

Estimated offset between phase and group-delay positions at 8.4 GHz is ~170 microarcseconds.

Abstract

Aims: The effect of frequency-dependent AGN core positions (``core-shifts'') on radio Very Long Baseline Interferometry (VLBI) global astrometry measurements is investigated. Methods: The basic equations relating to VLBI astrometry are reviewed, including the effects of source structure. A power-law representation of core-shifts, based on both observations and theoretical considerations of jet conditions, is incorporated. Results: It is shown that, in the presence of core-shifts, phase and group-delay astrometry measurements yield different positions. For a core displacement from the jet base parametrized by Delta x (lambda) = k lambda^beta group delays measure a ``reduced'' core-shift of (1-beta) Delta x (lambda). For the astrophysically-significant case of beta = 1, group delays measure no shift at all, giving the position of the jet base. At 8.4 GHz an estimated typical offset between phase and group-delay positions of ~170 uas is smaller than the current ~250 uas precision of group-delay positions of the sources used to define the ICRF; however, this effect must be taken into account for future measurements planned with improved accuracy when comparing with optical positions of AGN to be obtained with the GAIA mission.