Yueying Ni (ITC)

"The ASTRID simulation: the evolution of massive black holes"

The launch of the next-generation telescopes will soon revolutionize the study of the high-redshift universe and allow us to better understand the evolution of the first galaxies and supermassive black holes. Making full use of future observations will require a new generation of cosmological simulations with large volumes for statistical samples of large structures and with high resolution to model the galaxy formation. In this talk, I will introduce the ASTRID simulation, one of the largest hydrodynamic simulations represented by 2x5500^3 particles in 250 Mpc/h cosmic volume evolved down to z=1.5. ASTRID concurrently models the evolution of galaxies and supermassive black holes through cosmic time and traces the black hole dynamics and mergers with higher fidelity. With the large volume and high resolution, it probes a broad mass spectrum of the black hole population from the extreme >1e10Msun ultramassive black holes to the population of 1e4-1e6Msun intermediate mass black holes. 

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Jake Bennett (ITC)

 "A disturbing FABLE of mergers, feedback, turbulence, and mass biases in simulated galaxy clusters"

The use of galaxy clusters as cosmological probes often relies on understanding the properties and evolution of ICM. However, the ICM is a complex plasma, regularly stirred by mergers and feedback, with non-negligible bulk and turbulent motions and a non-thermal pressure component, making it difficult to construct a coherent and comprehensive picture. To this end, we use the FABLE simulations to investigate how the hydrostatic mass bias is affected by cluster dynamical state, mergers, AGN feedback and turbulence over cosmic time. We also look at how this links to the evolution of chemo-thermodynamic cluster profiles, compared to observations and other simulations.

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 Carol Cuesta-Lazaro (IAIFI)

"Constraining νΛCDM with density-split clustering"

The dependence of galaxy clustering on local density provides an effective method for extracting non-Gaussian information from galaxy surveys. The two-point correlation function (2PCF) provides a complete statistical description of a Gaussian density field. However, the late-time density field becomes non-Gaussian due to non-linear gravitational evolution and higher-order summary statistics are required to capture all of its cosmological information. In this talk, I'll show how we can retrieve a large amount of this information by combining clustering statistics from regions of different environmental density. I'll also discuss the ongoing work of constructing simulation-based methods to model DS clustering statistics for a DESI-like survey.