How can we find big baby planets around young, active Solar-type stars?

Although our understanding of how planetary systems come to exist has drastically improved over the last two decades, there is still plenty of research to be made around the formation and evolution of massive, short-orbit exoplanets e.g. hot Jupiters, warm Neptunes. Do they form in-situ or far from their host star and later experience migration? By constraining the occurrence rates of these types of planets in every stage of a star's life, we can better understand their fate and hope to favour one formation/evolution mechanism over another. In this context, it is crucial to estimate the population of these weird planets around young stars. Unfortunately, probing young stars is notoriously difficult due to their strong magnetic activity (or 'jitter') inducing spurious radial velocity (RV) signals that often mask the planet(s) RV signature(s) used to detect them. My presentation will showcase a 2-step process to efficiently characterise hot Jupiters orbiting young and active Solar-type stars. First, I will demonstrate how we can assess the capability of two distinct activity-filtering techniques (Doppler imaging and Gaussian process) by attempting to recover simulated planetary signatures hidden behind real stellar RV data exhibiting large jitter. Utilising these same tools, I'll show you how we can then hunt for hot Jupiters around stars being observed by NASA's new planet-finding mission TESS, which can then be followed-up with our MINERVA-Australis facility at the Mount Kent Observatory.