Constraining the properties of gaseous halos via cross-correlations of upcoming galaxy surveys and thermal Sunyaev-Zel'dovich maps

TL;DR

This paper forecasts how future galaxy and CMB surveys can constrain the thermodynamic properties of gaseous halos through cross-correlation of galaxy positions with thermal Sunyaev-Zel'dovich maps, improving understanding of baryonic feedback.

Contribution

It introduces a model fitting approach to forecast constraints on halo pressure profiles from upcoming surveys, accounting for observational systematics and degeneracies.

Findings

Future surveys can tightly constrain halo pressure profiles.

Measurements can confirm or rule out current feedback models.

Systematics like halo miscentering impact parameter estimation.

Abstract

The thermal Sunyaev-Zel'dovich (tSZ) effect induces a Compton-$y$ distortion in cosmic microwave background (CMB) temperature maps that is sensitive to a line of sight integral of the ionized gas pressure. By correlating the positions of galaxies with maps of the Compton-$y$ distortion, one can probe baryonic feedback processes and study the thermodynamic properties of a significant fraction of the gas in the Universe. Using a model fitting approach, we forecast how well future galaxy and CMB surveys will be able to measure these correlations, and show that powerful constraints on halo pressure profiles can be obtained. Our forecasts are focused on correlations between galaxies and halos identified by the upcoming Dark Energy Spectroscopic Instrument survey and tSZ maps from the Simons Observatory and CMB-S4 experiments, but have general applicability to other surveys, such as the Large Synoptic Survey Telescope. We include prescriptions for observational systematics, such as halo miscentering and halo mass bias, demonstrating several important degeneracies with pressure profile parameters. Assuming modest priors on these systematics, we find that measurements of halo-$y$ and galaxy-$y$ correlations with future surveys will yield tight constraints on the pressure profiles of group-scale dark matter halos, and enable current feedback models to either be confirmed or ruled out.