Leo C. Stein

Numerical relativity simulations provide the most accurate waveforms for binary black hole coalescences, but are prohibitively expensive for direct use in gravitational-wave data analysis.

Congratulations to Aniket Khairnar and Subhayu Bagchi on defending their PhDs!

Post-Newtonian (PN) theory provides the analytic foundation for modeling the early inspiral of binary black holes.

Accurate models of merger remnants are increasingly important for gravitational-wave science, including precision tests of gravity with ringdown, inference of black-hole populations, and modeling hierarchical mergers.

The name near-identity transformation (NIT) is just shorthand for a specific application of perturbation theory—one which is particularly useful in dynamical systems that have slow and fast timescales.

The Bondi–van der Burg–Metzner–Sachs (BMS) frame of gravitational waves produced by numerical relativity (NR) simulations is crucial for building accurate waveform models.

The photon ring of a Kerr black hole decomposes into a self-similar hierarchy of subrings.

We investigate how commonly used parameter definitions in Post-Newtonian (PN) theory compare with those from Numerical Relativity (NR) for binary black hole (BBH) systems.

The ‘ringdown’ radiation emitted by oscillating black holes has great scientific potential.

We present a major update to the Simulating eXtreme Spacetimes (SXS) Collaboration’s catalog of binary black hole simulations.