Cluster Survey Studies of the Dark Energy

TL;DR

Galaxy cluster surveys are crucial for understanding dark energy, but require careful calibration of mass-observable relations and redshift measurements to accurately constrain the dark energy equation of state.

Contribution

This paper discusses the self-calibration technique for cluster surveys, enabling simultaneous calibration and dark energy studies using survey data.

Findings

Self-calibration can effectively constrain dark energy parameters.

Cluster redshift distribution and power spectrum are key observables.

Calibration reduces uncertainties in mass-observable relations.

Abstract

Galaxy cluster surveys are power tools for studying the dark energy. In principle, the equation of state parameter w of the dark energy and its time evolution can be extracted from large solid angle, high yield surveys that deliver tens of thousands of clusters. Robust constraints require accurate knowledge of the survey selection, and crude cluster redshift estimates must be available. A simple survey observable like the cluster flux is connected to the underlying cluster halo mass through a so--called mass--observable relation. The calibration of this mass--observable relation and its redshift evolution is a key challenge in extracting precise cosmological constraints. Cluster survey self--calibration is a technique for meeting this challenge, and it can be applied to large solid angle surveys. In essence, the cluster redshift distribution, the cluster power spectrum, and a limited number of mass measurements can be brought together to calibrate the survey and study the dark energy simultaneously. Additional survey information like the shape of the mass function and its evolution with redshift can then be used to test the robustness of the dark energy constraints.