Over the past decades, cosmology has undergone a remarkable transformation. Measurements of the Cosmic Microwave Background and the detailed mapping of the Large-Scale Structure of the Universe have turned cosmology into a precision science, allowing us to constrain the composition, geometry, and evolution of the Universe with unprecedented accuracy.

The standard ΛCDM model provides an exceptionally successful description of a wide range of observations across cosmic time and scale. Yet, despite its empirical success, our understanding of the Universe remains incomplete. Several of its key ingredients point to deep open questions in fundamental physics. 

• Inflation is invoked to explain the initial conditions of the hot Big Bang evolution and the origin of primordial perturbations. 

• Cold dark matter is required to explain the formation of cosmic structures and the gravitational evidence for missing mass. 

• Dark energy, often described by a cosmological constant, is introduced to account for the observed late-time accelerated expansion of the Universe.

None of these ingredients is fully understood from first principles, either theoretically or experimentally. At the same time, increasingly precise cosmological and astrophysical measurements have revealed persistent tensions between different datasets and between early- and late-Universe probes. These tensions further challenge the completeness of the standard picture and motivate my work on exploring new physics with increasingly accurate theoretical, numerical, and statistical tools.

1 - Inflation and Primordial Cosmology

The primordial Universe is one of the few arenas in which cosmology can probe physics at energy scales far beyond the reach of terrestrial experiments.  Inflation provides a compelling framework for the origin of the initial conditions for the hot Big Bang evolution and of primordial fluctuations, but its fundamental nature remains unknown. 

The central challenge is to understand how the microscopic physics of the early Universe, including its degrees of freedom, symmetries, and gravitational dynamics, is translated into the statistical properties of the cosmic structures we observe today.

My research treats inflationary cosmology as an inverse problem: reconstructing primordial physics from the statistical structure of cosmic perturbations. I study how scalar and tensor spectra, their scale dependence, and their consistency relations encode information about inflationary dynamics, and how these signatures can be tested with CMB, Large-Scale Structure, B-mode polarization, and gravitational-wave observations. The broader goal is to separate universal predictions of inflation from assumptions tied to specific potentials, parametrizations, or background cosmologies.

2 - The Dark Sector: Interactions and Cosmic Acceleration

The dark sector is one of the clearest indications that our current understanding of fundamental physics is incomplete. Dark matter is required to explain the formation and gravitational clustering of cosmic structures, while dark energy is invoked to account for the late-time accelerated expansion of the Universe. Yet the physical nature of both components remains unknown. 

The central question is whether the dark sector is made of truly independent ingredients, or whether it reflects a richer set of fields, interactions, and gravitational dynamics beyond the minimal ΛCDM description. My research in this area focuses on theoretical and phenomenological descriptions of dark matter and dark energy, ranging from models of cosmic acceleration and dynamical dark energy to more exotic scenarios involving early dark energy, dark matter-dark energy interactions, and the cosmological implications of interactions between dark matter and Standard Model particles, such as neutrinos. 

These scenarios modify the expansion history of the Universe, the clustering of matter, and the propagation of cosmological perturbations, leaving correlated signatures in the Cosmic Microwave Background and Large-Scale Structure data. A key goal of my present and future work is to develop theory-to-data tests capable of isolating these signals, thereby opening a portal toward a deeper understanding of the Dark Universe.

5 - The Cosmology We Don’t Have Yet

Cosmology has entered an era in which the limiting factor is no longer only the amount of data, but our ability to turn data into physical understanding. The next DESI release, Euclid, LSST, CMB-S4, Roman, together with the next generation of gravitational-wave experiments, will be transformative. However, the challenge is not only to measure the same cosmological parameters with smaller error bars. It is to understand what cosmology should become when datasets are enormous, heterogeneous, correlated, and increasingly mediated by simulations, AI, and complex inference pipelines.

On the technical side, I am interested in contributing to faster, more robust, and more informative ways of doing cosmology with future surveys, gravitational-wave experiments, and multi-messenger probes. This means developing methods that can extract the maximum amount of physical information from forthcoming surveys and cosmic messengers, without reducing cosmology to larger parameter tables or automated pipelines.

On a conceptual side, I am interested in (re)thinking what cosmology, and the work of cosmologists, should look like in a future shaped by enormous heterogeneous datasets and AI-assisted analyses. At the end of the day, cosmology is (and must remain) more than just measuring parameters through AI-driven management of data and pipelines. It is a part of the Universe trying to understand itself.  The challenge will be to absorb future data and technologies without forgetting why we started asking these questions in the first place.