Workshop: Linking Galaxies from the Epoch of Initial Star Formation to Today

Published: 27 Nov 2018
Workshop poster

Sydney, Australia 18–22 February 2019

Over the last two decades, surveys mapping the Universe have made clear that star formation activity peaks about 10 billion years ago (known as cosmic noon). The driver of this behaviour is still an open area of research. A better understanding of star-forming regions and physical processes is required to explain the rise and fall of star formation around cosmic noon.  This joint Australia–ESO conference addresses a range of topical issues, more details are available below. This conference forms part of the Elizabeth and Frederick White research conference series.

With existing observational resources, we are able to resolve many detailed questions about the physical processes driving galaxy formation and evolution, including: the enrichment of the interstellar medium; gas infall; the role of galaxy environment; triggering mechanisms of starbursts and active galactic nuclei; and the role of gas dynamics and stellar kinematics. Cosmological simulations (Illustris, EAGLE, FIRE) indicate that the ISM and its constituents are important to understand galaxy formation but are poorly constrained. The discrepancy between observations and simulations is because the roles and physics of the above-mentioned processes are not well understood.

This conference will focus on:

  • Defining synergies between Australia and other ESO communities to follow up existing and planned optical and radio surveys to maximise impact and establish a better understanding of galaxy formation and evolution.
  • Defining questions for simulators to test and improve their simulations.
  • Encouraging interactions and collaborations between observers, theorist, and simulators internationally.

The deadline for talk abstracts is 3 December 2018 and the registration deadline is 4 January 2019. Further details can be found via the conference webpage. Questions can be directed to the organisers by email.