Black hole spectroscopy beyond Kerr: Agnostic and theory-based tests with next-generation interferometers

Black hole spectroscopy is a clean and powerful tool to test gravity in the strong -field regime and to probe the nature of compact objects. Next -generation ground -based detectors, such as the Einstein Telescope and Cosmic Explorer, will observe thousands of binary black hole mergers with large signal-tonoise ratios, allowing for accurate measurements of the remnant black hole quasinormal mode frequencies and damping times. In previous work we developed an observable -based parametrization of the quasinormal mode spectrum of spinning black holes beyond general relativity (ParSpec). In this paper we use this parametrization to ask the following question: can next -generation detectors detect or constrain deviations from the Kerr spectrum by stacking multiple observations of binary mergers from astrophysically motivated populations? We focus on two families of tests: (i) agnostic (null) tests, and (ii) theorybased tests, which make use of quasinormal frequency calculations in specific modified theories of gravity. We consider in particular two quadratic gravity theories (Einstein -scalar -Gauss -Bonnet and dynamical Chern-Simons gravity) and various effective field theory -based extensions of general relativity. We find that robust inference of hypothetical corrections to general relativity requires pushing the slow -rotation expansion to high orders. Even when high -order expansions are available, ringdown observations alone may not be sufficient to measure deviations from the Kerr spectrum for theories with dimensionful coupling constants. This is because the constraints are dominated by "light" black hole remnants, and only few of them have sufficiently high signal-to-noise ratio in the ringdown. Black hole spectroscopy with nextgeneration detectors may be able to set tight constraints on theories with dimensionless coupling, as long as we assume prior knowledge of the mass and spin of the remnant black hole.