The work provides the first quantitative characterization of how spacecraft orbit uncertainties and velocity mismodeling propagate into LISA gravitational-wave response mismatches and parameter biases.
Cutler, Angular resolution of the LISA gravitational wave detector, Phys
9 Pith papers cite this work. Polarity classification is still indexing.
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Defines residual ε between Shapiro-delay and GW-derived inclinations for LISA-SKA pulsars and estimates attainable precision at 4e-3 to 9e-4 using Fisher matrix and sky-averaged sensitivity.
Introduces a minimal quadratic statistic to isolate temporal correlations in intrinsic phase fluctuations of double white dwarf binaries and derives an analytic SNR scaling with total observation time and intrinsic correlation time.
Eccentricity-induced higher harmonics allow binary neutron star gravitational wave signals to reach detection thresholds and achieve useful localization several minutes earlier in 2G detector networks than circular signals.
Derives the fifth action for 1.5PN BBH with arbitrary eccentricity, spins, and masses, completing action-angle variables for analytical dynamics solution.
LISA observations of inspiraling stellar-mass BBHs around SMBHs can achieve relative uncertainties of 10^{-5} for SMBH mass and a few percent for spin in high-SNR cases.
LISA EMRIs can constrain deviations from Kerr equatorial symmetry to 10^{-2} and axial symmetry to 10^{-3} using Analytic Kludge waveforms and Fisher analysis.
LISA can constrain non-axisymmetric mass quadrupole deformations at the 10^{-3} level and axisymmetric mass octupole deformations at the 10^{-2} level in EMRI signals to test fuzzball proposals.
LGWA could observe more than one third of known binary black hole events, detect ~90 mergers per year, and measure chirp mass better than third-generation detectors for massive systems.
citing papers explorer
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Impact of Spacecraft Orbit Uncertainties and Velocity Mismodeling on the LISA Gravitational-Wave Response
The work provides the first quantitative characterization of how spacecraft orbit uncertainties and velocity mismodeling propagate into LISA gravitational-wave response mismatches and parameter biases.
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A geometric multimessenger consistency test of radiative and near-zone gravity with LISA and SKA
Defines residual ε between Shapiro-delay and GW-derived inclinations for LISA-SKA pulsars and estimates attainable precision at 4e-3 to 9e-4 using Fisher matrix and sky-averaged sensitivity.
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Temporal Correlation Statistic for Intrinsic Phase Fluctuation in Double White Dwarf Gravitational-Wave Signals
Introduces a minimal quadratic statistic to isolate temporal correlations in intrinsic phase fluctuations of double white dwarf binaries and derives an analytic SNR scaling with total observation time and intrinsic correlation time.
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Enhancing Early Detection and Localization of Gravitational Waves via Eccentricity-Induced Higher Harmonic Modes with 2G Detector Networks
Eccentricity-induced higher harmonics allow binary neutron star gravitational wave signals to reach detection thresholds and achieve useful localization several minutes earlier in 2G detector networks than circular signals.
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Action-angle variables of a binary black hole with arbitrary eccentricity, spins, and masses at 1.5 post-Newtonian order
Derives the fifth action for 1.5PN BBH with arbitrary eccentricity, spins, and masses, completing action-angle variables for analytical dynamics solution.
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Constraining Kerr supermassive black hole properties using gravitational waves from inspiraling stellar-mass binary black holes
LISA observations of inspiraling stellar-mass BBHs around SMBHs can achieve relative uncertainties of 10^{-5} for SMBH mass and a few percent for spin in high-SNR cases.
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Probing Kerr Symmetry Breaking with LISA Extreme-Mass-Ratio Inspirals
LISA EMRIs can constrain deviations from Kerr equatorial symmetry to 10^{-2} and axial symmetry to 10^{-3} using Analytic Kludge waveforms and Fisher analysis.
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Are Black Holes Fuzzballs? Probing Horizon-Scale Structure with LISA
LISA can constrain non-axisymmetric mass quadrupole deformations at the 10^{-3} level and axisymmetric mass octupole deformations at the 10^{-2} level in EMRI signals to test fuzzball proposals.
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Gravitational-wave parameter estimation to the Moon and back: massive binaries and the case of GW231123
LGWA could observe more than one third of known binary black hole events, detect ~90 mergers per year, and measure chirp mass better than third-generation detectors for massive systems.