Bayesian time delay interferometry

Page, J.; Littenberg, T. B.

doi:10.1103/physrevd.104.084037

Cited by 17 publications

(4 citation statements)

References 20 publications

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“…The most basic configuration can be thought of as a TDI-Michelson-Morley interferometer, where one constructs a response such as that in Equation (58). However, the great advantage of TDI is that it is possible to construct channels that suppress detector noise and enhance the signal [138]; this is a very active area of study [139][140][141][142][143][144]. For the purposes of this review, let us cite the TDI {X, Y, Z} set of channels, which are based on the Michelson-Morley style measurement in Equation (58), where nominally X is centered around spacecraft 1, referred to hereafter as S 1 ; Y around spacecraft 2, S 2 ; and Z around spacecraft 3, S 3 .…”

Section: Interdetector and Spatial Correlationsmentioning

confidence: 99%

Stochastic Gravitational-Wave Backgrounds: Current Detection Efforts and Future Prospects

et al. 2022

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The collection of individually resolvable gravitational wave (GW) events makes up a tiny fraction of all GW signals that reach our detectors, while most lie below the confusion limit and are undetected. Similarly to voices in a crowded room, the collection of unresolved signals gives rise to a background that is well-described via stochastic variables and, hence, referred to as the stochastic GW background (SGWB). In this review, we provide an overview of stochastic GW signals and characterise them based on features of interest such as generation processes and observational properties. We then review the current detection strategies for stochastic backgrounds, offering a ready-to-use manual for stochastic GW searches in real data. In the process, we distinguish between interferometric measurements of GWs, either by ground-based or space-based laser interferometers, and timing-residuals analyses with pulsar timing arrays (PTAs). These detection methods have been applied to real data both by large GW collaborations and smaller research groups, and the most recent and instructive results are reported here. We close this review with an outlook on future observations with third generation detectors, space-based interferometers, and potential noninterferometric detection methods proposed in the literature.

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Section: Interdetector and Spatial Correlationsmentioning

confidence: 99%

Stochastic Gravitational-Wave Backgrounds: Current Detection Efforts and Future Prospects

et al. 2022

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“…The sparse time-domain signal is then transformed to the frequency domain and convolved with a 𝛿 function at the carrier frequency. The convolution produces projections along the LISA constellation arms that are combined into time-delay interferometry (TDI, Tinto & Armstrong 1999;Armstrong et al 1999;Estabrook et al 2000;Dhurandhar et al 2002;Tinto & Dhurandhar 2005;Vallisneri et al 2021;Tinto & Dhurandhar 2021;Baghi et al 2021;Page & Littenberg 2021) observables: 𝑋, 𝑌 , 𝑍. These three TDI variables are correlated between them, but one could linearly combine them to build the noise orthogonal Vallisneri (2005); Prince et al ( 2002)…”

Section: Galactic Binary Waveformsmentioning

confidence: 99%

Bayesian Characterisation of Circumbinary Exoplanets with LISA

Katz,

Danielski,

Karnesis

et al. 2022

Preprint

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The Laser Interferometer Space Antenna (LISA) will detect and characterize ∼ 10 4 Galactic Binaries consisting predominantly of two White Dwarfs (WD). An interesting prospect within this population is a third object-another WD star, a Circumbinary Exoplanet (CBP), or a Brown Dwarf (BD)-in orbit about the inner WD pair. We present the first fully Bayesian detection and posterior analysis of sub-stellar objects with LISA, focusing on the characterization of CBPs. We used an optimistic astrophysically motivated catalogue of these CBP third-body sources, including their orbital eccentricity around the inner binary for the first time. We examined Bayesian Evidence computations for detectability, as well as the effects on the posterior distributions for both the inner binary parameters and the third-body parameters. We find that the posterior behavior bifurcates based on whether the third-body period is above or below half the observation time. Additionally, we find that undetectable third-body sources can bias the inner binary parameters whether or not the correct template is used. We used the information retrieved from the study of the CBP population to make an initial conservative prediction for the number of detectable BD systems in the original catalogue. We end with commentary on the predicted qualitative effects on LISA global fitting and Galactic Binary population analysis. The procedure used in this work is generic and can be directly applied to other astrophysical effects expected within the Galactic Binary population.

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“…The sparse time-domain signal is then transformed to the frequency domain and convolved with a δ function at the carrier frequency. The convolution produces projections along the LISA constellation arms that are combined into time-delay interferometry (TDI; Armstrong, Estabrook & Tinto 1999 ;Estabrook, Tinto & Armstrong 2000 ;Dhurandhar, Nayak & Vinet 2002 ;Tinto & Dhurandhar 2005 ;Baghi et al 2021 ;Page & Littenberg 2021 ;Tinto & Dhurandhar 2021 ;Vallisneri et al 2021 ) observables: X , Y , Z . These three TDI variables are correlated between them, but one could linearly combine them to build the noise orthogonal Vallisneri ( 2005 ) and Prince et al ( 2002)…”

Section: G a L Ac T I C B I Na Ry Wav E F O R M Smentioning

confidence: 99%

Bayesian characterization of circumbinary sub-stellar objects with LISA

Katz

Danielski

Karnesis

et al. 2022

Monthly Notices of the Royal Astronomical Society

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The Laser Interferometer Space Antenna (LISA) will detect and characterize ∼104 Galactic Binaries consisting predominantly of two White Dwarfs (WD). An interesting prospect within this population is a third object–another WD star, a Circumbinary Exoplanet (CBP), or a Brown Dwarf (BD)–in orbit about the inner WD pair. We present the first fully Bayesian detection and posterior analysis of sub-stellar objects with LISA, focusing on the characterization of CBPs. We used an optimistic astrophysically motivated catalogue of these CBP third-body sources, including their orbital eccentricity around the inner binary for the first time. We examined Bayesian Evidence computations for detectability, as well as the effects on the posterior distributions for both the inner binary parameters and the third-body parameters. We find that the posterior behavior bifurcates based on whether the third-body period is above or below half the observation time. Additionally, we find that undetectable third-body sources can bias the inner binary parameters whether or not the correct template is used. We used the information retrieved from the study of the CBP population to make an initial conservative prediction for the number of detectable BD systems in the original catalogue. We end with commentary on the predicted qualitative effects on LISA global fitting and Galactic Binary population analysis. The procedure used in this work is generic and can be directly applied to other astrophysical effects expected within the Galactic Binary population.

show abstract

Bayesian time delay interferometry

Cited by 17 publications

References 20 publications

Stochastic Gravitational-Wave Backgrounds: Current Detection Efforts and Future Prospects

Stochastic Gravitational-Wave Backgrounds: Current Detection Efforts and Future Prospects

Bayesian Characterisation of Circumbinary Exoplanets with LISA

Bayesian characterization of circumbinary sub-stellar objects with LISA

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