Boosting the sensitivity of high-frequency gravitational wave detectors using PT -symmetry

The kilo-Hertz gravitational waves radiated by the neutron star merger remnants carry rich information about the physics of high-density nuclear matter states, and many important astrophysical phenomena such as gamma-ray bursts and black hole formation. Current laser interferometer gravitational wave detectors, such as LIGO, VIRGO, and KAGRA have limited signal response at the kilo-Hertz band, thereby unable to capture these important physical phenomena. This work proposes an alternative protocol for boosting the sensitivity of the gravitational wave detectors at high frequency by implementing an optomechanical quantum amplifier. With the auxiliary quantum amplifier, this design has the feature of Parity-Time (PT) symmetry so that the detection band will be significantly broadened within the kilo-Hertz range. In this work, we carefully analyze the quantum-noise-limited sensitivity and the dynamical stability of this design. Based on our protocol, our result shows that the quantum-noise-limited sensitivity will be improved by one order of magnitude around 3kHz, which indicates the potential of our design for a future search of neutron star merger signals.

[1]  V. J. Hamedan,et al.  Neutron Star Extreme Matter Observatory: A kilohertz-band gravitational-wave detector in the global network , 2020, Publications of the Astronomical Society of Australia.

[2]  N. Kijbunchoo,et al.  Quantum enhanced kHz gravitational wave detector with internal squeezing , 2020, Classical and Quantum Gravity.

[3]  B. Metzger,et al.  The Multi-messenger Matrix: The Future of Neutron Star Merger Constraints on the Nuclear Equation of State , 2019, The Astrophysical Journal.

[4]  Yiqiu Ma,et al.  Quantum expander for gravitational-wave observatories , 2019, Light: Science & Applications.

[5]  L. Rezzolla,et al.  Using Gravitational-wave Observations and Quasi-universal Relations to Constrain the Maximum Mass of Neutron Stars , 2017, 1711.00314.

[6]  Hans-Thomas Janka,et al.  Neutron-star Radius Constraints from GW170817 and Future Detections , 2017, 1710.06843.

[7]  Hans-Thomas Janka,et al.  Exploring properties of high-density matter through remnants of neutron-star mergers , 2015, 1508.05493.

[8]  M. S. Shahriar,et al.  Characterization of the LIGO detectors during their sixth science run , 2014, 1410.7764.

[9]  C. Broeck,et al.  Advanced Virgo: a second-generation interferometric gravitational wave detector , 2014, 1408.3978.

[10]  Michael E. Tobar,et al.  Extremely Low Loss Phonon-Trapping Cryogenic Acoustic Cavities for Future Physical Experiments , 2013, Scientific Reports.

[11]  Yanbei Chen,et al.  Macroscopic quantum mechanics: theory and experimental concepts of optomechanics , 2013, 1302.1924.

[12]  Kei Kotake,et al.  Multiple physical elements to determine the gravitational-wave signatures of core-collapse supernovae , 2011, 1110.5107.

[13]  Swee-Ping Chia,et al.  AIP Conference Proceedings , 2008 .

[14]  F. Khalili,et al.  Energetic Quantum Limit in Large-Scale Interferometers , 1999, gr-qc/9907057.

[15]  Alfred Brian Pippard,et al.  Response and Stability: An Introduction to the Physical Theory , 1985 .