Baryonification extended to thermal Sunyaev Zeldovich

TL;DR

This paper extends baryonification algorithms to include gas temperature and pressure, enabling accurate modeling of the thermal Sunyaev-Zeldovich effect and related observables, validated against hydrodynamical simulations.

Contribution

The authors introduce a self-consistent baryonification model for gas temperature and pressure, fitting multiple observables with only two additional parameters.

Findings

Reproduces electron pressure, gas, stellar, and dark matter power spectra within 10%.

Achieves 1% accuracy for convergence and 10% for thermal SZ angular power spectra down to l=5000.

Models baryonic effects efficiently for use in cosmological analyses and simulations.

Abstract

Baryonification algorithms model the impact of galaxy formation and feedback on the matter field in gravity-only simulations by adopting physically motivated parametric prescriptions. In this paper, we extend these models to describe gas temperature and pressure, allowing for a self-consistent modelling of the thermal Sunyaev-Zeldovich effect, weak gravitational lensing, and their cross-correlation, down to small scales. We validate our approach by showing that it can simultaneously reproduce the electron pressure, gas, stellar, and dark matter power spectra as measured in all BAHAMAS hydrodynamical simulations. Specifically, with only two additional free parameters, we can fit the electron pressure auto- and cross-power spectra at 10% while reproducing the suppression in the matter power spectrum induced by baryons at the per cent level, for different AGN feedback strengths in BAHAMAS. Furthermore, we reproduce BAHAMAS convergence and thermal Sunyaev Zeldovich angular power spectra within 1% and 10% accuracy, respectively, down to l = 5000. When used jointly with cosmological rescaling algorithms, the baryonification presented here will allow a fast and accurate exploration of cosmological and astrophysical scenarios. Therefore, it can be employed to create mock catalogues, lightcones, and large training sets for emulators aimed at interpreting forthcoming multi-wavelength observations of the large-scale structure of the Universe.