Influence of a continuous plane gravitational wave on Gaia-like astrometry

TL;DR

This study analyzes how continuous plane gravitational waves affect Gaia-like astrometric measurements, revealing that many GW signals are absorbed into astrometric parameters, complicating detection but leaving residuals that could enable future GW detection methods.

Contribution

The paper introduces a geometric model for GW effects on Gaia-like astrometry and evaluates the impact of continuous GWs on astrometric solutions through simulated data.

Findings

Significant GW signals are absorbed into astrometric parameters, mimicking errors.

Astrometric residuals retain parts of the GW signal, offering potential detection avenues.

Errors are largest at specific GW frequencies related to the scanning law.

Abstract

A gravitational wave (GW) passing through an astrometric observer causes periodic shifts of the apparent star positions measured by the observer. For a GW of sufficient amplitude and duration, and of suitable frequency, these shifts might be detected with a Gaia-like astrometric telescope. This paper aims to analyse in detail the effects of GWs on an astrometric solution based on Gaia-like observations, which are one-dimensional, strictly differential between two widely separated fields of view and following a prescribed scanning law. We present a simple geometric model for the astrometric effects of a plane GW in terms of the time-dependent positional shifts. Using this model, the general interaction between the GW and a Gaia-like observation is discussed. Numerous Gaia-like astrometric solutions are made, taking as input simulated observations that include the effects of a continuous plain GW with constant parameters and periods ranging from ~50 days to 100 years. The resulting solutions are analysed in terms of the systematic errors on astrometric and attitude parameters, as well as the observational residuals. It is found that a significant part of the GW signal is absorbed by the astrometric parameters, leading to astrometric errors of a magnitude (in radians) comparable to the strain parameters. These astrometric errors are in general not possible to detect, because the true (unperturbed) astrometric parameters are not known to corresponding accuracy. The astrometric errors are especially large for specific GW frequencies that are linear combinations of two characteristic frequencies of the scanning law. Nevertheless, for all GW periods smaller than the time span covered by the observations, significant parts of the GW signal also go into the astrometric residuals. This fosters the hope for a GW detection algorithm based on the residuals of standard astrometric solutions.