First results and future prospects for dual-harmonic searches for gravitational waves from spinning neutron stars. Issue 4 (16th September 2015)

• Record Type: Journal Article
• Authors: Pitkin, M.; Gill, C.; Jones, D. I.; Woan, G.; Davies, G. S.
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 453:Issue 4(2015)
• Page Start: 4399
• Page End: 4420
• Publication Date: 2015-09-16
• Subjects: gravitational waves -- methods: data analysis -- methods: statistical -- stars: neutron -- pulsars: general; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/stv1931
• Languages: English
• ISSNs: 0035-8711

Abstract

Abstract: We investigate a method to incorporate signal models that allow an additional frequency harmonic in searches for gravitational waves from spinning neutron stars. We assume that emission is given by the general triaxial non-aligned model of Jones, whose waveform under certain conditions reduces to that of a biaxial precessing star, or a simple rigidly rotating triaxial aligned star. The triaxial non-aligned and biaxial models can produce emission at both the star's rotation frequency ( f ) and 2 f, whilst the latter only emits at 2 f . We have studied parameter estimation for signal models using both a set of physical source parameters and a set of waveform parameters that remove a degeneracy. We have assessed the signal detection efficiency, and used Bayesian model selection to investigate how well we can distinguish between the three models. We found that for signal-to-noise ratios (SNRs) ≳6, there is no significant loss in efficiency if performing a search for a signal at f and 2 f when the source is only producing emission at 2 f . However, for sources with emission at both f and 2 f, signals could be missed by a search only at 2 f . We also find that for a triaxial aligned source, the correct model is always favoured, but for a triaxial non-aligned source it can be hard to distinguish between the triaxial non-aligned model and the biaxial model, even at high SNR. Finally, we apply the method to a selection of known pulsars using data from the LIGO fifth science run. We give the first upper limits on gravitational wave amplitude at both f and 2 f and apply the model selection criteria on real data.