Massive black hole binary mergers produce orphaned low-frequency signals in PTA pulsar terms that can be stacked for archival multiband gravitational-wave detection.
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AM-CW lunar laser ranging achieves μHz SGWB sensitivity of 5.29×10^{-9} D_cov (80 μm range uncertainty) or 2.07×10^{-9} D_cov (50 μm) over 5 years, with discovery possible if covariance degradation stays below ~3.6-13.7.
Binary pulsar timing can constrain quadratic scalar ULDM couplings between 2e-22 and 2e-21 eV and vector ULDM couplings between 1e-23 and 1e-18 eV via resonant orbital effects.
Clustered primordial black holes may constitute all dark matter and produce a flat stochastic gravitational wave background detectable by the Einstein Telescope.
citing papers explorer
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Archival Multiband Gravitational-Wave Signals from Massive Black Hole Binary Mergers
Massive black hole binary mergers produce orphaned low-frequency signals in PTA pulsar terms that can be stacked for archival multiband gravitational-wave detection.
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High-Power AM-CW Lunar Laser Ranging as a $\mu$Hz SGWB Detector
AM-CW lunar laser ranging achieves μHz SGWB sensitivity of 5.29×10^{-9} D_cov (80 μm range uncertainty) or 2.07×10^{-9} D_cov (50 μm) over 5 years, with discovery possible if covariance degradation stays below ~3.6-13.7.
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Sensitivity of binary pulsar timing to spin-0 and spin-1 ultralight dark matter
Binary pulsar timing can constrain quadratic scalar ULDM couplings between 2e-22 and 2e-21 eV and vector ULDM couplings between 1e-23 and 1e-18 eV via resonant orbital effects.
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Hunting Dark Matter with the Einstein Telescope
Clustered primordial black holes may constitute all dark matter and produce a flat stochastic gravitational wave background detectable by the Einstein Telescope.