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The gravitational waveform of merging binary neutron stars encodesinformation about extreme states of matter. Probing these gravitationalemissions requires the gravitational-wave detectors to have high sensitivityabove 1 kHz. Fortunately for current advanced detectors, there is a sizeablegap between the quantum-limited sensitivity and the classical noise at highfrequencies. Here we propose a detector design that closes such a gap byreducing the high-frequency quantum noise with an active optomechanical filter,frequency-dependent squeezing, and high optical power. The resulting noiselevel from 1 kHz to 4 kHz approaches the current facility limit and is a factorof 20 to 30 below the design of existing advanced detectors. This will allowfor precision measurements of (i) the post-merger signal of the binary neutronstar, (ii) late-time inspiral, merger, and ringdown of low-mass blackhole-neutron star systems, and possible detection of (iii) high-frequency modesduring supernovae explosions. This design tries to maximize the science returnof current facilities by achieving a sensitive frequency band that iscomplementary to the longer-baseline third-generation detectors: the10 kmEinstein Telescope, and 40 km Cosmic Explorer. We have highlighted the maintechnical challenges towards realizing the design, which requires dedicatedresearch programs. If demonstrated in current facilities, the techniques can betransferred to new facilities with longer baselines.

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