Parameter choices and ranges for continuous gravitational wave searches for steadily spinning neutron stars

TL;DR

This paper analyzes parameter choices and degeneracies in continuous gravitational wave searches from rotating neutron stars, proposing methods to remove degeneracies and improve search strategies.

Contribution

It introduces a systematic approach to identify and eliminate parameter degeneracies in gravitational wave models of neutron stars, aiding search design and parameter estimation.

Findings

Identifies discrete and continuous degeneracies in source parameters.

Proposes parameter range restrictions to remove degeneracies.

Simplifies waveform parameterization for different stellar models.

Abstract

We consider the issue of selecting parameters and their associated ranges for carrying out searches for continuous gravitational waves from steadily rotating neutron stars. We consider three different cases (i) the "classic" case of a star spinning about a principal axis; (ii) a biaxial star, not spinning about a principal axis; (iii) a triaxial star spinning steady, but not about a principal axis (as described in Jones, MNRAS vol 402, 2503 (2010)). The first of these emits only at one frequency; the other two at a pair of harmonically related frequencies. We show that in all three cases, when written in terms of the original "source parameters", there exist a number of discrete degeneracies, with different parameter values giving rise to the same gravitational wave signal. We show how these can be removed by suitably restricting the source parameter ranges. In the case of the model as written down by Jones, there is also a continuous degeneracy. We show how to remove this through a suitable rewriting in terms of "waveform parameters", chosen so as to make the specialisations to the other stellar models particularly simple. We briefly consider the (non-trivial) relation between the assignment of prior probabilities on one set of parameters verses the other. The results of this paper will be of use when designing strategies for carrying out searches for such multi-harmonic gravitational wave signals, and when performing parameter estimation in the event of a detection.