The galaxy–halo connection
Empirical models linking dark matter haloes to galaxies, and full-sky mock catalogues of the radio sky for SKAO and Euclid.
My research is driven by a single question: how does what we do not see shape what we see? I study the physical interplay between the dark universe — dark matter and dark energy — and the observable one: baryons, and more recently gravitational waves. Connecting invisible structure to the observable properties of galaxies requires theoretical modelling, numerical simulations, and multi-wavelength observations, held together by computational tools and data-driven methods.
Three axes run through this work. They converge on a common methodological thread: building the computational bridge between dark-matter simulations and observable galaxy properties.
Empirical models linking dark matter haloes to galaxies, and full-sky mock catalogues of the radio sky for SKAO and Euclid.
Panchromatic SED modelling from X-rays to radio with GalaPy — Bayesian inference at almost 1000 SEDs per second on a single core.
Making the void size function a viable cosmological probe — from a new ridge-finding algorithm to Euclid Key Projects.
These axes are not independent. Starting from the theoretical study of cosmic voids, my work has moved progressively toward the empirical modelling of galaxy populations and, most recently, toward full panchromatic emission modelling. Each step has produced public software now actively used by the community, including within international collaborations such as Euclid and SKAO.
The convergence is not accidental. The tools form a coherent pipeline: SCAMPy populates dark-matter light-cones with galaxy populations, T-RECS provides their radio emission properties, and GalaPy infers — and can assign — panchromatic SEDs.