Related papers: Quantum Noise Fraction and the Thermal Frontier in High-Frequency Gravitational Wave Detection

Quantum Noise Fraction and the Thermal Frontier in High-Frequency Gravitational Wave Detection

URL: http://arxiv.org/abs/2605.00053v1
Date: Wed, 29 Apr 2026 18:37:56 GMT
Title: Quantum Noise Fraction and the Thermal Frontier in High-Frequency Gravitational Wave Detection
Abstract summary: We introduce a diagnostic that determines the maximum sensitivity improvement achievable through quantum enhancement for any gravitational wave detector.<n>We propose a gravitational wave detector employing squeezed phononic states via circuit QED readout.<n>An array of $104$ such resonators with 10 dB mechanical squeezing reaches $sqrtS_h = 7.6 times 10-26/sqrtrm$ -- still a factor $109$ above the BBN bound on backgrounds at 1 GHz.
Score: 0.0
License: http://arxiv.org/licenses/nonexclusive-distrib/1.0/
Abstract: We introduce a diagnostic -- the quantum noise fraction $β$ -- that determines the maximum sensitivity improvement achievable through quantum enhancement for any gravitational wave detector. Applied to the landscape of proposed high-frequency (kHz-GHz) detectors, this diagnostic reveals that resonant mass detectors operating through tidal coupling are thermally dominated ($β\approx 0$) at all frequencies below ~230 MHz at dilution temperatures, rendering squeezing and entanglement limited in effectiveness. Only above this thermal frontier, defined by $\hbar ω= k_B T \ln 3$, does the quantum regime become accessible. We identify a single concrete realization: a bulk acoustic wave resonator at 1 GHz and 10 mK ($β= 0.98$), and propose a gravitational wave detector employing squeezed phononic states via circuit QED readout. An array of $10^4$ such resonators with 10 dB mechanical squeezing reaches $\sqrt{S_h} = 7.6 \times 10^{-26}/\sqrt{\rm Hz}$ -- still a factor ~$10^9$ above the BBN bound on stochastic backgrounds at 1 GHz, indicating that the sensitivity gap remains predominantly classical in origin and that concurrent advances in classical detector parameters will be required.

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