The SkyMapper Transient (SMT) Survey is a currently searching and studying supernovae and other transient sources in southern sky.

This project is intended to search for the magnetic field signature of the Magellanic halo.

The goal of this project is to build a software pipeline that can take simulations of galactic winds, such as the one shown in the figure, and make simulated observational images from them that can be compared directly to telescopic data.

This project will simulate observations of the magnetic fields of a Milky Way-like galaxy from a recent, high-resolution simulation. The goal is to identify effective ways to reconstruct the 3D magnetic field geometry of this simulated galaxy using observables projected onto the 2D sky.

In order to further the MAVIS design, an image simulator was built in Python, allowing star catalogs to be fed in, which are used to generate realistic MAVIS images. MAVIS now requires an IFU simulator to be developed, providing realistic IFU images from star catalogs.

This project will build on work within the Dark-ages, Reionization And Galaxy-formation Observables Numerical Simulation project (DRAGONS).

Approximately 75% of SkyMapper's observing time will be initially dedicated to the Southern Sky Survey, a comprehensive digital survey of the entire southern sky.

This project will investigate the properties of binary neutron star progenitors and their host galaxies by applying state‑of‑the‑art transient modelling tools. By linking the astrophysical properties to their explosive counterparts, we will have a better idea of what types of sources will produce kilonovae. A deeper understanding of this astrophysics is essential for optimising future electromagnetic follow‑up strategies for gravitational‑wave detections.

Star Clusters as Engines of Ionisation and their HII Regions in NGC 7793

We will use simulations of the Milky Way to make predictions for SKA.

You will use new data from the Australian SKA Pathfinder survey, GASKAP-HI to help take the temperature of the Milky Way and Magellanic Clouds. PhD & Masters students on this project will have the opportunity to be among the first users of ASKAP.  

The effective temperature is one of the most fundamental parameters of a star, and its precise determination is crucial for a number of purposes, e.g., from measuring chemical abundances and ages, to improving stellar and atmosphere models.

M dwarfs are the most abundant stars in the universe, and prime targets for detecting Earth-like planets.

We have a variety of projects that will use the new GASKAP-HI data to study the structure and temperature of hydrogen in the Magellanic System.