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A physicist who uses numerical relativity to study strong gravitational fields, especially curvature singularities and gravitational collapse. His simulations test how the Einstein field equations behave close to a singularity, including whether the behavior found in symmetric models survives when symmetry restrictions are removed.^[ref]

With José M. Martín Senovilla, he reviewed how the Penrose singularity theorem connects gravitational collapse with geodesic incompleteness.^[ref]

For detector $k$, model the calibrated data as $d_k(t)=h_k(t;\theta )+n_k(t)$, with a shared source parameter vector $\theta$, separate detector responses, propagation delays and noise $n_k$. Under an independent stationary Gaussian process approximation with one-sided power spectral density $S_k(f)$, define the noise-weighted inner product and likelihood functionStrain power spectral density has units ${\mathrm{Hz}}^{-1}$; the displayed inner product is dimensionless when the Fourier transform integrates over seconds. A matched filter rewards agreement over the full evolving wave phase, weighting frequency bands by their noise. One conspicuous peak is insufficient: a candidate should also have the right distribution of signal across frequency bands and compatible projections in the network.

The parameter paper used coherent Bayesian inference, numerical relativity-informed inspiral–merger–ringdown models and explicit calibration uncertainties. It found a strong distance–inclination correlation; source-frame masses additionally require converting the detector-frame masses by a cosmological redshift.^[ref] Conceptually, multiply the likelihood function by a prior distribution to obtain a posterior distribution. Changes in waveform families, residual structure after subtraction, and checks with a generic transient reconstruction test parts of the modeling assumptions. Detection significance and parameter uncertainty answer different questions.

Numerical relativity computes solutions of the Einstein field equations when an analytic solution or a small-perturbation approximation is insufficient. A 3+1 decomposition of spacetime separates initial spatial geometry and matter from their subsequent evolution. Initial data must satisfy the Hamiltonian constraint and momentum constraint, while the lapse function and shift vector specify the coordinate evolution.

The calculation also needs boundary conditions and a numerical evolution formulation. Resolution studies, constraint monitoring and comparison with known solutions test whether the computed result approximates the intended spacetime. Binary black-hole mergers provide an observational application: numerical waveforms connect strongly dynamical geometry with interferometer signals.^[ref] Extracting a physical wave requires controlling the frame and propagation model as well as solving grid equations.