Identifying LISA verification binaries among the Galactic population of double white dwarfs

TL;DR

This paper evaluates the detectability of known verification binaries with LISA using Bayesian analysis, estimating detection times and exploring combined GW and EM observation strategies amidst a realistic Galactic white dwarf population.

Contribution

It provides a Bayesian framework for analyzing known verification binaries with LISA, estimating detection prospects and strategies in a complex Galactic environment.

Findings

25 verification binaries detectable within 4 years

Detection times can be estimated early in LISA operations

Analysis includes competing signals from the Galactic white dwarf population

Abstract

Double white dwarfs (DWDs) will be the most numerous gravitational-wave (GW) sources for the Laser Interferometer Space Antenna (LISA). Most of the Galactic DWDs will be unresolved and will superpose to form a confusion noise foreground, the dominant LISA noise source around $\sim 0.5\mathrm{-}3\,\mathrm{mHz}$. A small fraction of these sources will stand out from the background and be individually detectable. Uniquely among GW sources, a handful of these binaries will be known in advance from electromagnetic (EM) observations and will be guaranteed sources of detectable GWs in the LISA band; these are known as verification binaries (VBs). High-cadence photometric surveys are continuously discovering new VB systems, and their number will continue to grow ahead of the launch of LISA. We analyse, in a fully Bayesian framework, all the currently known VB candidates with the latest design requirements for the LISA mission and find that 25 of the considered sources can be detected within a $4\,\mathrm{yr}$ observation time. We explore what can be expected from GW observations, both alone and in combination with EM observations, and estimate the VB's time to detection in the early months of LISA operations. We also show how VBs can be analysed in the case where their GW signals compete with many other unknown binary signals (both resolved and unresolved) from a realistic Galactic population of DWDs.