Gravitational-wave emission from compact Galactic binaries

TL;DR

This paper assesses how revised local densities of white-dwarf binaries influence gravitational-wave detection prospects and foreground estimates for future space-based observatories, considering various formation scenarios and detection strategies.

Contribution

It evaluates the impact of new observational constraints on population models and GW detection forecasts for Galactic binaries.

Findings

Thousands of detached binary detections expected

Few tens to hundreds of interacting binary detections projected

Confusion noise estimates are generally consistent with previous studies

Abstract

Compact Galactic binaries where at least one member is a white dwarf or neutron star constitute the majority of individually detectable sources for future low-frequency space-based gravitational-wave (GW) observatories; they also form an unresolved continuum, the dominant Galactic foreground at frequencies below a few mHz. Due to the paucity of electromagnetic observations, the majority of studies of Galactic-binary populations so far have been based on population-synthesis simulations. However, recent surveys have reported several new detections of white-dwarf binaries, providing new constraints for population estimates. In this article, we evaluate the impact of revised local densities of interacting white-dwarf binaries on future GW observations. Specifically: we consider five scenarios that explain these densities with different assumptions on the formation of interacting systems; we simulate corresponding populations of detached and interacting white-dwarf binaries; we estimate the number of individually detectable GW sources and the magnitude of the confusion-noise foreground, as observed by space-based detectors with 5- and 1-Mkm arms. We confirm earlier estimates of thousands of detached-binary detections, but project only few ten to few hundred detections of interacting systems. This reduction is partly due to our assessment of detection prospects, based on the iterative identification and subtraction of bright sources with respect to both instrument and confusion noise. We also confirm earlier estimates for the confusion-noise foreground, except in one scenario that explains smaller local densities of interacting systems with smaller numbers of progenitor detached systems.