LISA verification binaries with updated distances from Gaia Data Release 2
dc.contributor | Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA 91125, USA | |
dc.contributor | Leiden Observatory, Leiden University, PO Box 9513, NL-2300 RA, Leiden, the Netherlands | |
dc.contributor | Albert-Einstein-Institut, Max-Planck-Institut fúr Gravitationsphysik, D-30167 Hannover, Germany | |
dc.contributor | Department of Astrophysics/IMAPP, Radboud University Nijmegen, POBox 9010, NL-6500 GL, Nijmegen, the Netherlands; Institute of Astronomy, KU Leuven, Celestijnenlaan 200D, B-3001 Leuven, Belgium | |
dc.contributor | Department of Physics, University of Warwick, Coventry CV4 7AL, UK | |
dc.contributor | Armagh Observatory and Planetarium, College Hill, Armagh, BT61 9DG, UK | |
dc.contributor | Department of Astrophysics/IMAPP, Radboud University Nijmegen, POBox 9010, NL-6500 GL, Nijmegen, the Netherlands | |
dc.contributor.author | Kupfer, T. | |
dc.contributor.author | Korol, V. | |
dc.contributor.author | Shah, S. | |
dc.contributor.author | Nelemans, G. | |
dc.contributor.author | Marsh, T. R. | |
dc.contributor.author | Ramsay, G. | |
dc.contributor.author | Groot, P. J. | |
dc.contributor.author | Steeghs, D. T. H. | |
dc.contributor.author | Rossi, E. M. | |
dc.date.accessioned | 2024-02-01T17:10:47Z | |
dc.date.available | 2024-02-01T17:10:47Z | |
dc.date.issued | 2018-10-01T00:00:00Z | |
dc.identifier.doi | 10.1093/mnras/sty1545 | |
dc.identifier.doi | 10.48550/arXiv.1805.00482 | |
dc.identifier.other | 2018MNRAS.tmp.1473K | |
dc.identifier.other | 2018arXiv180500482K | |
dc.identifier.other | astro-ph.SR | |
dc.identifier.other | 2018MNRAS.tmp.1473K | |
dc.identifier.other | 2018MNRAS.480..302K | |
dc.identifier.other | 2018arXiv180500482K | |
dc.identifier.other | 10.48550/arXiv.1805.00482 | |
dc.identifier.other | arXiv:1805.00482 | |
dc.identifier.other | 10.1093/mnras/sty1545 | |
dc.identifier.other | - | |
dc.identifier.uri | http://hdl.handle.net/20.500.14302/1366 | |
dc.description.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 so-called `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 signal-to-noise 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). | |
dc.publisher | Monthly Notices of the Royal Astronomical Society | |
dc.title | LISA verification binaries with updated distances from Gaia Data Release 2 | |
dc.type | article | |
dc.source.journal | MNRAS | |
dc.source.journal | MNRAS.480 | |
dc.source.volume | 480 | |
refterms.dateFOA | 2024-02-01T17:10:47Z | |
dc.identifier.bibcode | 2018MNRAS.480..302K |