Abstract
Cosmic Explorer (CE) is a next-generation ground-based gravitational-wave observatory concept, envisioned to begin operation in the 2030s, and expected to be capable of observing binary neutron star and black hole mergers back to the time of the first stars. Cosmic Explorer's sensitive band will extend below 10 Hz, where the design is predominantly limited by geophysical, thermal, and quantum noises. In this work, thermal, seismic, gravity-gradient, quantum, residual gas, scattered-light, and servo-control noises are analyzed in order to motivate facility and vacuum system design requirements, potential test mass suspensions, Newtonian noise reduction strategies, improved inertial sensors, and cryogenic control requirements. Our analysis shows that with improved technologies, Cosmic Explorer can deliver a strain sensitivity better than $10^{-23}/\mathrm{Hz}^{1/2}$ down to 5 Hz. Our work refines and extends previous analysis of the Cosmic Explorer concept and outlines the key research areas needed to make this observatory a reality.
Highlights
The second generation of laser interferometric gravitational-wave observatories—the Advanced Laser Interferometer Gravitational-Wave Observatory (LIGO) [1], Advanced Virgo [2], and Kagra [3]—have opened a new window on the Universe by observing gravitational waves from merging systems of black holes [4,5] and neutron stars [6] and have ushered in a new era in multimessenger astronomy [7]
Research and development is underway toward a cryogenic silicon detector, LIGO Voyager, that could be implemented in the existing LIGO facilities [12], and a concept for a high-frequencyfocused Australian observatory is being developed [13]
This paper presents an assessment of the low-frequency sensitivity of Cosmic Explorer 1 (CE1) and Cosmic Explorer 2 (CE2) based on recent research and development progress
Summary
The second generation of laser interferometric gravitational-wave observatories—the Advanced Laser Interferometer Gravitational-Wave Observatory (LIGO) [1], Advanced Virgo [2], and Kagra [3]—have opened a new window on the Universe by observing gravitational waves from merging systems of black holes [4,5] and neutron stars [6] and have ushered in a new era in multimessenger astronomy [7]. In the rest of the paper, we will refer to detectors based on room-temperature fused silica test masses and 1 μm laser wavelength as the “1 μm technology” and those with cryogenic silicon test masses and 2 μm laser wavelength as the “2 μm technology.”. For both CE1 and CE2, the detector designs target observations above 5 Hz, while Einstein Telescope targets observations down to 3 Hz. This paper presents an assessment of the low-frequency sensitivity of CE1 and CE2 based on recent research and development progress. Appendix A summarizes the different technologies used in the two stages of Cosmic Explorer and Appendix B compares the displacement and force noises of Cosmic Explorer with those of other detectors
Sign-in/Register to view highlights & summary Sign-in/Register to access full text options 
Free) 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a call
