Fundaments of Black Hole Spectroscopy

Gravitational Wave (GW) astronomy has emerged as a fundamental field, allowing us to probe gravity in its strongest regime.

Black hole (BH) spectroscopy is a highly effective method for extracting spacetime information from observed GW signals. The late-time radiation of newly formed black holes is characterized by an exponentially damped, oscillating signal.

Measuring the decaying scales and oscillating frequencies the so-called quasinormal modes (QNMs) offers insightful information about the black hole's background.

Therefore, QNMs and BH spectroscopy are crucial in astrophysics, gravitational physics, and mathematical relativity.The goal of this project is to combine mathematical relativity, numerical relativity, and astrophysics to advance the fundamental theory of BH spectroscopy. Theoretical predictions indicate that small perturbations around a black hole can drastically change its QNM spectra.

Thus, in dirty environments, QNMs may deviate from the values expected for isolated BHs.

Modern tools from differential geometry and high-accuracy numerical methods allow us to understand this QNM instability.

This project will provide a solid theoretical foundation, which integrated into the efforts to measure QNMs, will optimise the scientific gains from BH spectroscopy in the upcoming era of high-accuracy GW astronomy.The applicant has solid expertise in the mathematical fundaments of general relativity.

With the MSCA fellowship, the applicant will enhance her knowledge of fundamental aspects of BH spectroscopy thanks to the expertise of the Niels Bohr Institute (NBI), University of Copenhagen.

The Strong group at NBI is composed of leading researchers in the area, providing the perfect environment for this multidisciplinary project.

An academic secondment at the University of Texas at Austin will consolidate the acquired knowledge and ensure the projects impact on key stakeholders, such as the Ligo-Virgo-Kagra collaboration and the Lisa Mission.