Landscape of stellar-mass black-hole spectroscopy with third-generation gravitational-wave detectors

• Published in: arXiv.org
• Main Authors: Bhagwat, Swetha, Costantino Pacilio, Pani, Paolo, Mapelli, Michela
• Format: Paper
• Language: English
• Published: Ithaca Cornell University Library, arXiv.org 05.04.2023
• Subjects: Binary stars; Black holes; Configurations; Detectors; Gravitational waves; Matrix methods; Sensors; Spectrum analysis
• ISSN: 2331-8422

Gravitational-wave black-hole spectroscopy provides a unique opportunity to test the strong-field regime of gravity and the nature of the final object formed in the aftermath of a merger. Here we investigate the prospects for black-hole spectroscopy with third-generation gravitational-wave detectors, in particular the Einstein Telescope in different configurations, possibly in combination with Cosmic Explorer. Using a state-of-the-art population model for stellar-origin binary black holes informed by LIGO-Virgo-KAGRA data, we compute the average number of expected events for precision black-hole spectroscopy using a Fisher-matrix analysis. We find that Einstein Telescope will measure two independent quasinormal modes within \({\cal O}(1)\%\) (resp. \({\cal O}(10)\%\)) relative uncertainty for at least \({\cal O}(1)\) (resp. \({\cal O}(500)\)) events per year, with similar performances in the case of a single triangular configuration or two L-shaped detectors with same arm length. A 15-km arm-length configuration would improve rates by roughly a factor of two relative to a 10-km arm-length configuration. When operating in synergy with Cosmic Explorer the rates will improve significantly, reaching few-percent accuracy for \({\cal O}(100)\) events per year.