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Fast Parameter Inference on Pulsar Timing Arrays with Normalizing Flows.
Phys Rev Lett
July 2024
Department of Physics, University of California Santa Cruz, 1156 High Street, Santa Cruz, California 95064, USA.
Pulsar timing arrays perform Bayesian posterior inference with expensive Markov chain Monte Carlo (MCMC) methods. Given a dataset of ∼10-100 pulsars and O(10^{3}) timing residuals each, producing a posterior distribution for the stochastic gravitational wave background (SGWB) can take days to a week. The computational bottleneck arises because the likelihood evaluation required for MCMC is extremely costly when considering the dimensionality of the search space.
View Article and Find Full Text PDFUsing Pulsar Parameter Drifts to Detect Subnanohertz Gravitational Waves.
Phys Rev Lett
March 2024
Department of Physics, University of California Santa Cruz, 1156 High Street, Santa Cruz, California 95064, USA and Santa Cruz Institute for Particle Physics, 1156 High Street, Santa Cruz, California 95064, USA.
Gravitational waves with frequencies below 1 nHz are notoriously difficult to detect. With periods exceeding current experimental lifetimes, they induce slow drifts in observables rather than periodic correlations. Observables with well-known intrinsic contributions provide a means to probe this regime.
View Article and Find Full Text PDFEfficient Large-Scale, Targeted Gravitational-Wave Probes of Supermassive Black-Hole Binaries.
Phys Rev Lett
February 2024
Department of Physics and Astronomy, Vanderbilt University, 2301 Vanderbilt Place, Nashville, Tennessee 37235, USA.
Binary systems of supermassive black holes are promising sources of low-frequency gravitational waves (GWs) and bright electromagnetic emission. Pulsar timing array GW searches for individual binaries have been limited to only a few candidate systems due to computational demands, which get worse as more pulsars are added. By modeling the GW signal using only components from when the GW passes Earth (rather than also each pulsar), we find constraints on the binary's total mass and GW frequency that are similar to a full signal analysis, yet ∼70 times more efficient.
View Article and Find Full Text PDFDirect Measurement of the Spectral Structure of Cosmic-Ray Electrons+Positrons in the TeV Region with CALET on the International Space Station.
Phys Rev Lett
November 2023
Department of Physics and McDonnell Center for the Space Sciences, Washington University, One Brookings Drive, St. Louis, Missouri 63130-4899, USA.
Detailed measurements of the spectral structure of cosmic-ray electrons and positrons from 10.6 GeV to 7.5 TeV are presented from over 7 years of observations with the CALorimetric Electron Telescope (CALET) on the International Space Station.
View Article and Find Full Text PDFLimits on scalar-induced gravitational waves from the stochastic background by pulsar timing array observations.
Sci Bull (Beijing)
December 2023
School of Astronomy and Space Science, University of Science and Technology of China, Hefei 230026, China; Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China; Theoretical Physics Division, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China.
Recently, the NANOGrav, PPTA, EPTA, and CPTA Collaborations independently reported their evidence of the Stochastic Gravitational Waves Background (SGWB). While the inferred gravitational-wave background amplitude and spectrum are consistent with astrophysical expectations for a signal from the population of supermassive black-hole binaries (SMBHBs), the search for new physics remains plausible in this observational window. In this work, we explore the possibility of explaining such a signal by the scalar-induced gravitational waves (IGWs) in the very early universe.
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