Fundamental quantum limits for detecting ultrahigh frequency gravitational waves
arXiv:2501.18146 · doi:10.1103/2w9f-yy8g
Abstract
The ultrahigh-frequency (above 10 kHz) gravitational waves (GW) window provides a unique opportunity to detect primordial GWs, free from astrophysical foregrounds that dominate lower frequencies. A stochastic GW background in this range is generically predicted from cosmological phase transitions and topological defects associated with grand unification and other ultra-high energy theories. We establish a universal quantum limit framework for various detection schemes, setting a fundamental bound on GW detectability. Our analysis reveals that backgrounds in the kHz-MHz range are in principle observable, whereas higher-frequency signals lie below the quantum limit. These results offer theoretical guidance for future detector designs and open new avenues for probing early universe physics.
21 pages, 5 figures
References in corpus (18)
- Advanced LIGO
- GWTC-3: Compact Binary Coalescences Observed by LIGO and Virgo During the Second Part of the Third Observing Run
- The NANOGrav 15-year Data Set: Evidence for a Gravitational-Wave Background
- Search for an isotropic gravitational-wave background with the Parkes Pulsar Timing Array
- Searching for the nano-Hertz stochastic gravitational wave background with the Chinese Pulsar Timing Array Data Release I
- The second data release from the European Pulsar Timing Array III. Search for gravitational wave signals
- Challenges and Opportunities of Gravitational Wave Searches at MHz to GHz Frequencies
- Stochastic gravitational wave background from smoothed cosmic string loops
- Frequency-Dependent Responses in 3rd Generation Gravitational-Wave Detectors
- Electromagnetic Antennas for the Resonant Detection of the Stochastic Gravitational Wave Background
- Unification, Proton Decay and Topological Defects in non-SUSY GUTs with Thresholds
- A Gravitational Wave Detector for Post Merger Neutron Stars: Beyond the Quantum Loss Limit of Michelson Fabry Perot Interferometer
- Classification of Abelian domain walls
- Improving the detection sensitivity to primordial stochastic gravitational waves with reduced astrophysical foregrounds
- Classical (and Quantum) Heuristics for Gravitational Wave Detection
- Stochastic waveform estimation at the fundamental quantum limit
- Non-Abelian Domain Walls and Gravitational Waves
- Photon counting for axion interferometry