RESEARCH

Understanding how galaxies trace the Universe.

My research lies at the intersection of observational cosmology, large-scale structure, cosmological simulations, and statistical modelling.

I am particularly interested in how galaxies and quasars trace the underlying dark matter field, how this connection can be modelled realistically, and how observational and survey effects propagate into cosmological measurements.

Galaxy–halo connection

Galaxies form and evolve within dark matter halos, but the relationship between galaxies and halos is not directly observable.

I use simulation-based approaches to model this connection and study how different galaxy populations occupy dark matter halos. My work includes halo occupation models, subhalo-based approaches, and abundance-matching techniques for DESI tracers including quasars and emission-line galaxies.

A central goal is to understand how assumptions about the galaxy–halo connection affect the clustering of galaxies and quasars.

Key themes

SHAM · HOD · Vpeak · Vmean · satellite fraction

DESI and mock universes

The Dark Energy Spectroscopic Instrument (DESI) is producing large spectroscopic samples of galaxies and quasars that enable precision measurements of the expansion history and growth of structure.

My work contributes to the construction and validation of realistic DESI mock catalogs using large cosmological simulations, particularly Uchuu and GLAM.

These simulations are used to produce reference and covariance mocks for DESI analyses, including lightcone catalogs for multiple tracer populations.

DESI tracers

• Emission-line galaxies (ELGs)
• Luminous red galaxies (LRGs)
• Quasars (QSOs)
• Bright galaxy samples (BGS)

The goal is to reproduce not only the broad properties of the observed samples, but also their clustering and survey-specific characteristics.

Large-scale structure

The spatial distribution of galaxies contains information about the underlying matter field and the evolution of cosmic structure.

I compare simulated and observed clustering across redshift bins and tracer populations to validate mock catalogs and quantify systematic uncertainties.

My work includes two-point and higher-order clustering statistics, with applications to DESI reference mocks, covariance mocks, and cosmological analyses.

A recurring theme is connecting the physics and modelling of galaxies to the statistics that are ultimately measured from a survey.

Survey realism and systematic effects

A realistic mock catalog needs to reproduce more than the underlying cosmological density field.

Real surveys contain observational effects that can modify measured clustering. I study the impact of selection effects, redshift failures, survey geometry, and other observational systematics on large-scale structure measurements.

This includes work on redshift-failure modelling and its impact on two- and three-point statistics and constraints on primordial non-Gaussianity.

Time-domain cosmology

Alongside my large-scale structure work, I have worked on the use of nearby Type Ib/c core-collapse supernovae for cosmology.

Using ROTSE data, I have investigated cosmological distance measurements from stripped-envelope supernovae and the associated observational and time-domain systematics.

This provides a complementary low-redshift perspective to my work with high-redshift spectroscopic surveys.

From simulations to cosmology

A common thread throughout my research is the connection between simulations, observations, and cosmological inference.

Dark matter → Halos → Galaxies → Survey → Clustering → Cosmology

The broader goal is to develop increasingly realistic, simulation-based frameworks for extracting cosmological information from current and next-generation astronomical surveys.