Defines peak-integrated sensitivity curves (PISCs) that fold in the expected spectral shape of gravitational waves from cosmological phase transitions and supplies semianalytical fits plus public data for major detectors.
Interferometer design of the KAGRA gravitational wave detector
11 Pith papers cite this work. Polarity classification is still indexing.
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Pith papers citing it
abstract
KAGRA is a cryogenic interferometric gravitational wave detector being constructed at the underground site of Kamioka mine in Gifu prefecture, Japan. We performed an optimization of the interferomter design, to achieve the best sensitivity and a stable operation, with boundary conditions of classical noises and under various practical constraints, such as the size of the tunnel or the mirror cooling capacity. Length and alignment sensing schemes for the robust control of the interferometer are developed. In this paper, we describe the detailed design of the KAGRA interferometer as well as the reasoning behind design choices.
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Conditional normalizing flows perform likelihood-free parameter estimation for single and overlapping LISA galactic binaries, generating thousands of posterior samples per second after training on simulations.
Mode-by-mode filtering of higher-order modes enables low-latency marginalization over mode information in NSBH gravitational-wave signals, tightening constraints on distance, inclination, and secondary mass.
Strong lensing of MBHBs produces identifiable beat patterns in about 7% of detectable two-image LISA events, with Bayesian inference recovering time delay and magnification parameters.
Targeted eccentric search detects GW200105 with SNR 13.4 and FAR <1/1000 yr, consistent with dynamical formation of the NSBH binary.
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.
Spin sorting with the default spin model distinguishes spinning and nonspinning binary black hole populations in simulations and shows real data rule out a fully nonspinning population but allow mixed ones with up to 80% nonspinning sources.
PyCBC Live for O4 adds time-dependent background modeling, early warning search, and improved autogating, delivering sensitivity gains of 1.7-2.3x for coincident searches in mock data challenges.
Numerical post-merger waveforms indicate that planned 3rd-generation GW detector networks can detect rotational instabilities in BNS remnants at distances up to 200 Mpc with a high-frequency design, and the main post-merger peak at 40 Mpc with upgraded HLV.
KAGRA enhances sky localization of binary neutron star mergers in the LVK network via added baselines, with measurable gains at current sensitivity and larger improvements as range reaches ~30 Mpc.
Baselines of 8-11 ms light travel time for two CE detectors provide a reasonable compromise for BBH sky localization, with third detectors eliminating multimodality for most or all events.
citing papers explorer
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New Sensitivity Curves for Gravitational-Wave Signals from Cosmological Phase Transitions
Defines peak-integrated sensitivity curves (PISCs) that fold in the expected spectral shape of gravitational waves from cosmological phase transitions and supplies semianalytical fits plus public data for major detectors.
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Neural posterior estimation of Galactic Binary signals for the LISA mission
Conditional normalizing flows perform likelihood-free parameter estimation for single and overlapping LISA galactic binaries, generating thousands of posterior samples per second after training on simulations.
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Improving low-latency multi-messenger follow-up of neutron star-black hole mergers with mode-by-mode filtering
Mode-by-mode filtering of higher-order modes enables low-latency marginalization over mode information in NSBH gravitational-wave signals, tightening constraints on distance, inclination, and secondary mass.
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Identification of Lensed Gravitational-Wave Beat Patterns by LISA
Strong lensing of MBHBs produces identifiable beat patterns in about 7% of detectable two-image LISA events, with Bayesian inference recovering time delay and magnification parameters.
-
Detection of GW200105 with a targeted eccentric search
Targeted eccentric search detects GW200105 with SNR 13.4 and FAR <1/1000 yr, consistent with dynamical formation of the NSBH binary.
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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.
-
Disentangling spinning and nonspinning binary black hole populations with spin sorting
Spin sorting with the default spin model distinguishes spinning and nonspinning binary black hole populations in simulations and shows real data rule out a fully nonspinning population but allow mixed ones with up to 80% nonspinning sources.
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PyCBC Live Search for Compact Binary Mergers in Advanced LIGO and Virgo's Fourth Observing Run
PyCBC Live for O4 adds time-dependent background modeling, early warning search, and improved autogating, delivering sensitivity gains of 1.7-2.3x for coincident searches in mock data challenges.
-
Exploring the Potential for Detecting Rotational Instabilities in Binary Neutron Star Merger Remnants with Gravitational Wave Detectors
Numerical post-merger waveforms indicate that planned 3rd-generation GW detector networks can detect rotational instabilities in BNS remnants at distances up to 200 Mpc with a high-frequency design, and the main post-merger peak at 40 Mpc with upgraded HLV.
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Investigating the effect of sensitivity of KAGRA on sky localization of gravitational-wave sources from compact binary coalescences
KAGRA enhances sky localization of binary neutron star mergers in the LVK network via added baselines, with measurable gains at current sensitivity and larger improvements as range reaches ~30 Mpc.
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Not too close! Evaluating the impact of the baseline on the localization of binary black holes by next-generation gravitational-wave detectors
Baselines of 8-11 ms light travel time for two CE detectors provide a reasonable compromise for BBH sky localization, with third detectors eliminating multimodality for most or all events.