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.

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

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

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.

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.

The student will work with Prof. Krumholz to design and run simulations using the enzo adaptive mesh refinement code.

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).