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Gravitational-wave parameter estimation with gaps in LISA: A Bayesian data augmentation method

Quentin Baghi1,*, James Ira Thorpe1, Jacob Slutsky1, John Baker1, Tito Dal Canton1, Natalia Korsakova2, and Nikos Karnesis3

  • 1NASA Goddard Space Flight Center, 8800 Greenbelt Road, Maryland 20771, USA
  • 2Artémis UMR 7250, Observatoire de la Côte d’Azur, Boulevard de l’Observatoire, CS 34229-F, 06304 NICE Cedex 4
  • 3Laboratoire Astroparticules et Cosmologie, Université Paris Diderot, 10 Rue Alice Domon et Léonie Duquet, 75013 Paris, France

  • *quentin.s.baghi@nasa.gov
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Phys. Rev. D 100, 022003 – Published 17 July, 2019

DOI: https://doi.org/10.1103/PhysRevD.100.022003

Abstract

By listening to gravity in the low-frequency band, between 0.1 mHz and 1 Hz, the future space-based gravitational-wave observatory LISA will be able to detect tens of thousands of astrophysical sources from cosmic dawn to the present. The detection and characterization of all resolvable sources is a challenge in itself, but LISA data analysis will be further complicated by interruptions occurring in the interferometric measurements. These interruptions will be due to various causes occurring at various rates, such as laser frequency switches, high-gain antenna repointing, orbit corrections, or even unplanned random events. Extracting long-lasting gravitational-wave signals from gapped data raises problems such as noise leakage and increased computational complexity. We address these issues by using Bayesian data augmentation, a method that reintroduces the missing data as auxiliary variables in the sampling of the posterior distribution of astrophysical parameters. This provides a statistically consistent way to handle gaps while improving the sampling efficiency and mitigating leakage effects. We apply the method to the estimation of galactic binary parameters with different gap patterns, and we compare the results to the case of complete data.

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Phys. Rev. D 100, 022003– Published 17 July, 2019
  • Received 9 May 2019
Article part of CHORUS
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