Multi-pipeline follow-up recovers the G347.3-0.5 outlier in O3 data but finds no standard persistent continuous-wave signal in O4a or O4b, disfavouring the astrophysical interpretation under the assumed model.
Modeling the Galactic Neutron Star Population for Use in Continuous Gravitational Wave Searches
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abstract
Searches for continuous gravitational waves from \textit{unknown} Galactic neutron stars provide limits on the shapes of neutron stars. A rotating neutron star will produce gravitational waves if asymmetric deformations exist in its structure that are characterized by the star's ellipticity. In this study, we use a simple model of the spatial and spin distribution of Galactic neutron stars to estimate the total number of neutron stars probed, using gravitational waves, to a given upper limit on the ellipticity. This may help optimize future searches with improved sensitivity. The improved sensitivity of third-generation gravitational wave detectors may increase the number of neutron stars probed, to a given ellipticity, by factors of 100 to 1000.
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The G347.3-0.5 outlier from O3: a follow-up case study for continuous gravitational-wave candidates
Multi-pipeline follow-up recovers the G347.3-0.5 outlier in O3 data but finds no standard persistent continuous-wave signal in O4a or O4b, disfavouring the astrophysical interpretation under the assumed model.