LISA verification binaries with updated distances from Gaia Data Release 2
Abstract
Ultracompact binaries with orbital periods less than a few hours will dominate the gravitational wave signal in the mHz regime. Until recently, 10 systems were expected to have a predicted gravitational wave signal strong enough to be detectable by the Laser Interferometer Space Antenna (LISA), the socalled `verification binaries'. System parameters, including distances, are needed to provide an accurate prediction of the expected gravitational wave strength to be measured by LISA. Using parallaxes from Gaia Data Release 2 we calculate signaltonoise ratios (SNR) for ≈50 verification binary candidates. We find that 11 binaries reach an SNR ≥ 20, two further binaries reaching an SNR≥ 5, and three more systems are expected to have a SNR≈ 5 after 4 yr integration with LISA. For these 16 systems, we present predictions of the gravitational wave amplitude (A) and parameter uncertainties from Fisher information matrix on the amplitude (A) and inclination (ι).
 Publication:

Monthly Notices of the Royal Astronomical Society
 Pub Date:
 October 2018
 DOI:
 10.1093/mnras/sty1545
 arXiv:
 arXiv:1805.00482
 Bibcode:
 2018MNRAS.480..302K
 Keywords:

 binaries: close;
 stars: distances;
 stars: individual: white dwarfs: AM CVns;
 Astrophysics  Solar and Stellar Astrophysics
 EPrint:
 accepted for publication in MNRAS, 9 pages, 4 figures