http://arxiv.org/abs/2304.02283
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.
S. Bhagwat, C. Pacilio, P. Pani, et. al.
Thu, 6 Apr 23
24/76
Comments: 13 pages, 9 figures