A potential third-generation gravitational-wave detector based on autocorrelative weak-value amplification

Abstract

Abstract Reducing noises and enhancing signal-to-noise ratios (SNRs) have become critical for designing third-generation gravitational-wave (GW) detectors with a GW strain of less than 10 − 23   H z − 1 . In this paper, we propose a potential third-generation GW detector based on autocorrelative weak-value amplification (AWVA) for GW detection with a strain of h g =   4 × 10 − 25   H z − 1 . In our scheme, a GW event induces a phase difference Δ ϕ by passing through a 11-bounce delay line, 10-km arm-length, zero-area Sagnac interferometer illuminated with a 1064-nm laser. Subsequently, Δ ϕ is amplified as the parameter of post-selection by choosing the appropriate pre-selected state and coupling strength in AWVA. In particular, we theoretically investigate the AWVA measurements for GW detection within the frequency band of 200 Hz ⩽   f g   ⩽ 800 Hz, considering Gaussian noises with negative-decibel SNRs. The peak response of the AWVA sensitivity κ ( f g ) occurs at frequency f g , m a x = 500 Hz, which falls within the frequency band of interest of the current third-generation GW detectors. Our simulation results indicate that AWVA can demonstrate a measurable sensitivity of the autocorrelation coefficient Θ ( f g ) within the frequency band of interest. Moreover, the robustness of WVA shows promising potential in mitigating the effects of Gaussian noises.