Towards the Design of Gravitational-Wave Detectors for Probing Neutron-Star Physics

TL;DR

This paper proposes an advanced gravitational-wave detector design that significantly improves high-frequency sensitivity, enabling detailed studies of neutron star mergers, black hole-neutron star systems, and supernovae, by reducing quantum noise with innovative techniques.

Contribution

The paper introduces a novel detector design combining active optomechanical filtering, frequency-dependent squeezing, and high optical power to enhance high-frequency sensitivity in gravitational-wave detectors.

Findings

Noise level approaches current facility limits from 1 kHz to 4 kHz

Achieves a factor of 20-30 sensitivity improvement over existing advanced detectors

Enables detection of post-merger signals, late inspiral, and supernova high-frequency modes

Abstract

The gravitational waveform of merging binary neutron stars encodes information about extreme states of matter. Probing these gravitational emissions requires the gravitational-wave detectors to have high sensitivity above 1 kHz. Fortunately for current advanced detectors, there is a sizeable gap between the quantum-limited sensitivity and the classical noise at high frequencies. Here we propose a detector design that closes such a gap by reducing the high-frequency quantum noise with an active optomechanical filter, frequency-dependent squeezing, and high optical power. The resulting noise level from 1 kHz to 4 kHz approaches the current facility limit and is a factor of 20 to 30 below the design of existing advanced detectors. This will allow for precision measurements of (i) the post-merger signal of the binary neutron star, (ii) late-time inspiral, merger, and ringdown of low-mass black hole-neutron star systems, and possible detection of (iii) high-frequency modes during supernovae explosions. This design tries to maximize the science return of current facilities by achieving a sensitive frequency band that is complementary to the longer-baseline third-generation detectors: the10 km Einstein Telescope, and 40 km Cosmic Explorer. We have highlighted the main technical challenges towards realizing the design, which requires dedicated research programs. If demonstrated in current facilities, the techniques can be transferred to new facilities with longer baselines.