Turbulence in the Intracluster Medium

Accurate estimation of galaxy cluster masses is a central problem in cosmology, underpinning precision constraints on structure formation and the matter content of the Universe. A key source of systematic uncertainty arises from non-thermal pressure support introduced by mergers, feedback processes, and motions of galaxies. These processes generate gas motions that are typically interpreted as turbulence.

My research has involved measuring the turbulence cascade rates, energies, and characteristic scales and how observations bias these measurements.

Some relevant work:

• Power spectrum estimation methods on intracluster medium surface brightness fluctuations

Solar Wind Transport Models

Charged particles are ejected from the sun and transported radially outward to the edge of the solar system, this plasma is called the solar wind. The evolution of magnetohydrodynamic scale fluctuations in the solar wind is a topic of long-standing interest, with relevance to various aspects of space physics including space weather, cosmic rays and their roles in connection with the global evolution of heliospheric fields.

My research has involved investigating different modelling assumptions and the affect it has on the evolution of energies and length scales and comparing these results to observations.

Some relevant work:

• Constraining Solar Wind Transport Model Parameters Using Bayesian Analysis
• Transport of turbulence in the solar wind

Full-sky Synchrotron Emission

Detection of the inflationary B-mode signal remains a primary goal for confirming the inflationary model and constraining the tensor properties of the universe. However, this cosmological signal is heavily obscured by Galactic foregrounds. Synchrotron emission dominates the B-mode signal at low (radio) frequencies, while thermal dust emission dominates at higher (radio) frequencies. Accurately characterizing and removing these foregrounds is therefore critical for unbiased cosmological parameter estimation.