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

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.  

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. 

The ISM of spiral galaxies is a dynamic environment consisting of thermal gas, relativistic particles, magnetic fields, and dust. The project aims to decipher the origin of filamentary structures in the ISM using numerical simulations as well as observational data.

This project will simulate observations of the rotation measure (RM) at high Galactic latitude that traces the magnetic structures of the Milky Way. The goal is to pinpoint the cause of the recently discovered asymmetry in the RM patterns between the two Galactic hemispheres.

This project will simulate observations of the rotation measure (RM) at high Galactic latitude that traces the magnetic structures of the Milky Way. The goal is to pinpoint the cause of the recently discovered asymmetry in the RM patterns between the two Galactic hemispheres.

Blue stragglers are main-sequence stars that are more luminous and bluer than stars of the same age, and their existence has long defied standard stellar evolution.

The student will model the gamma-ray emission around the Milky Way's central bubble.

In this project, the idea would be to combine the publicly available GALAH and APOGEE spectra and analyse them together: We should be able to measure up to 40 different elements from hundreds of lines and provide the community with reference values.

By conducting this comprehensive study, we will gain valuable insights into the distinctive properties of the HI gas in the Magellanic Stream. This will allow us to compare the properties of HI gas in the Magellanic Stream with those in the Magellanic Clouds and the Milky Way, shedding light on the differences between.

The goal of this project is to use new, high-resolution simulations to understand how key physical processes, like stellar feedback and gravitational instabilities, shape disk galaxies (from 11 Gyr ago to today).

Stellar spectra capture the light of a star across multiple wavelengths and include absorption features of numerous atoms and molecules from a star’s photosphere. The abundance data many stars then allow us to study the chemical evolution across large scales in our Galaxy and decipher Galactic trends.

In this project you will use a new cosmic ray propagation code, CRIPTIC, to model the injection, transport, and final annihilation of positrons in the interstellar medium of the inner Galaxy.

In this project you will use a new cosmic ray propagation code, CRIPTIC, to model the injection, transport, and final annihilation of positrons in the interstellar medium of the inner Galaxy.