Forward modeling of space-borne gravitational wave detectors

Rubbo, Louis J.; Cornish, N.; Poujade, Olivier

doi:10.1103/physrevd.69.082003

Cited by 138 publications

(170 citation statements)

References 28 publications

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“…II C, are essentially equivalent to the rigid adiabatic approximation of Ref. [20], and to the formalism of Ref. [18].…”

Section: Time-delay Interferometrymentioning

confidence: 99%

“…Seto [18] extended Cutler's formalism to high frequencies (and to noise-canceling observables), in the context of studying optimal-filtering parameter estimation for supermassive-black-hole binaries. Cornish, Rubbo, and Poujade [19,20] obtained general expressions valid in the entire LISA frequency band, and for arbitrary GW signals; these expressions are given as integrals over the LISA arms, and they provide the basic building blocks to assemble the TDI observables. By contrast, in this paper we work out explicit time-domain expressions for the LISA response to moderately chirping binary systems, for all the second-generation TDI combinations.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Erratum: Optimal filtering of the LISA data [Phys. Rev. D70, 022003 (2004)]

Królak¹,

Tinto²,

Vallisneri³

2007

Phys. Rev. D

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The LISA time-delay-interferometry responses to a gravitational-wave signal are rewritten in a form that accounts for the motion of the LISA constellation around the Sun; the responses are given in closed analytic forms valid for any frequency in the band accessible to LISA. We then present a complete procedure, based on the principle of maximum likelihood, to search for stellar-mass binary systems in the LISA data. We define the required optimal filters, the amplitude-maximized detection statistic (analogous to the F statistic used in pulsar searches with ground-based interferometers), and discuss the false-alarm and detection probabilities. We test the procedure in numerical simulations of gravitational-wave detection.PACS numbers: 95.55. Ym, 04.80.Nn, 95.75.Pq, 97.60.Gb

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“…II C, are essentially equivalent to the rigid adiabatic approximation of Ref. [20], and to the formalism of Ref. [18].…”

Section: Time-delay Interferometrymentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Erratum: Optimal filtering of the LISA data [Phys. Rev. D70, 022003 (2004)]

Królak¹,

Tinto²,

Vallisneri³

2007

Phys. Rev. D

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“…These approximations, together with the treatment of the moving-LISA GW response discussed in [8] are essentially equivalent to the rigid adiabatic approximation of Ref. [16], and to the formalism of Ref. [7].…”

Section: The Lisa Response To Signals From Binary Systemsmentioning

confidence: 99%

White-dwarf–white-dwarf galactic background in the LISA data

et al. 2005

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LISA (Laser Interferometer Space Antenna) is a proposed space mission, which will use coherent laser beams exchanged between three remote spacecraft to detect and study low-frequency cosmic gravitational radiation. In the low-part of its frequency band, the LISA strain sensitivity will be dominated by the incoherent superposition of hundreds of millions of gravitational wave signals radiated by inspiraling white-dwarf binaries present in our own galaxy. In order to estimate the magnitude of the LISA response to this background, we have simulated a synthesized population that recently appeared in the literature. Our approach relies on entirely analytic expressions of the LISA Time-Delay Interferometric responses to the gravitational radiation emitted by such systems, which allows us to implement a computationally efficient and accurate simulation of the background in the LISA data. We find the amplitude of the galactic white-dwarf binary background in the LISA data to be modulated in time, reaching a minimum equal to about twice that of the LISA noise for a period of about two months around the time when the Sun-LISA direction is roughly oriented towards the Autumn equinox. This suggests that, during this time period, LISA could search for other gravitational wave signals incoming from directions that are away from the galactic plane. Since the galactic white-dwarfs background will be observed by LISA not as a stationary but rather as a cyclostationary random process with a period of one year, we summarize the theory of cyclostationary random processes, present the corresponding generalized spectral method needed to characterize such process, and make a comparison between our analytic results and those obtained by applying our method to the simulated data. We find that, by measuring the generalized spectral components of the white-dwarf background, LISA will be able to infer properties of the distribution of the white-dwarfs binary systems present in our Galaxy.

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“…To include the LISA response we made use of the static LISA model as described in [25]. This approximation is valid for burst sources, as LISA does not move significantly over the typically short duration of the bursts, which is of the order of 1000s.…”

Section: Detector Modelmentioning

confidence: 99%

Classifying LISA gravitational wave burst signals using Bayesian evidence

Feroz

Gair

Graff

et al. 2010

Class. Quantum Grav.

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Abstract. We consider the problem of characterisation of burst sources detected with the Laser Interferometer Space Antenna (LISA) using the multi-modal nested sampling algorithm, MULTINEST. We use MULTINEST as a tool to search for modelled bursts from cosmic string cusps, and compute the Bayesian evidence associated with the cosmic string model. As an alternative burst model, we consider sine-Gaussian burst signals, and show how the evidence ratio can be used to choose between these two alternatives. We present results from an application of MULTINEST to the last round of the Mock LISA Data Challenge, in which we were able to successfully detect and characterise all three of the cosmic string burst sources present in the release data set. We also present results of independent trials and show that MULTINEST can detect cosmic string signals with signal-to-noise ratio (SNR) as low as ∼ 7 and sine-Gaussian signals with SNR as low as ∼ 8. In both cases, we show that the threshold at which the sources become detectable coincides with the SNR at which the evidence ratio begins to favour the correct model over the alternative.

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Forward modeling of space-borne gravitational wave detectors

Cited by 138 publications

References 28 publications

Erratum: Optimal filtering of the LISA data [Phys. Rev. D70, 022003 (2004)]

Erratum: Optimal filtering of the LISA data [Phys. Rev. D70, 022003 (2004)]

White-dwarf–white-dwarf galactic background in the LISA data

Classifying LISA gravitational wave burst signals using Bayesian evidence

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