FLAMINGO — A large suite of state-of-the-art galaxy cluster simulations for emulations for high-precision cosmology

FLAMINGO — A large suite of state-of-the-art galaxy cluster simulations for emulations for high-precision cosmology

Leads: Ian McCarthy, Joop Schaye, Matthieu Schaller, Willem Elbers, and the Virgo II Team 

A diverse set of new observatories are about to map the large-scale structure in the Universe down to smaller scales than was possible before, which will greatly improve our ability to find inconsistencies in the standard cosmological model. However, the scientific potential of these surveys can only be realised if the model predictions are at least as accurate and precise as the observations. 

Although the clustering of the dark matter is well understood, mainly because it is collisionless and therefore only subject to gravity, this is not yet the case for the ordinary, baryonic matter. Unlike the dark matter, baryons are subject to pressure force and are hence redistributed by galactic winds driven by supernova explosions and accreting supermassive black holes. Unless these effects are taken into account, they will cause systematic errors in the measurements of cosmological parameters of tens of per cent for upcoming weak gravitational lensing studies, thus eliminating most of the foreseen improvements on the current constraints. 

The FLAMINGO project from the Virgo Consortium addresses this urgent problem by providing a suite of hydrodynamical simulations of volumes large enough to predict the large-scale structure with a resolution that is sufficiently high to model the gas flows caused by feedback processes 

associated with galaxy formation. Because these feedback processes cannot yet be predicted from first principles, the free parameters of the model are calibrated to key observables using machine learning techniques. 

The need to model large volumes at relatively high resolution necessitates massive simulations using state-of-the-art codes. Indeed, FLAMINGO includes the largest ever hydrodynamical simulation of the entire history of the Universe. The simulations vary the uncertain astrophysical parameters as well as the mass of the elusive neutrino particle, which we expect to be able to measure from upcoming observational surveys. 

The distribution of matter in the past light cone of an observer at the centre of the map. The expansion of the Universe has been scaled out. Circles indicate the redshift z, where (1+z) is the factor by which the Universe has expanded since the time light crossed the circle on its way to the observer. Looking further out, i.e., further away from the centre of the image, implies looking back further in time to an era when the matter was distributed more smoothly. The inset zooms in on a massive galaxy cluster (10^15 times more massive than the Sun). The ruler in the inset indicates the scale (5 Mpc = 16 million lightyears).