The Impact of Halo Properties, Energy Feedback and Projection Effects on the Mass-SZ Flux Relation

TL;DR

This paper analyzes how halo properties, feedback, and projection effects influence the scatter in the SZ effect–mass relation, identifying optimal measurement radii and factors affecting its precision.

Contribution

It provides a detailed assessment of the factors affecting the Y-M relation scatter, including feedback, halo concentration, substructure, and projection effects, with recommendations for optimal measurement strategies.

Findings

Y measured within smaller radii yields less scatter.

Energy feedback increases intrinsic scatter due to gas fraction variations.

Substructure accounts for about 20% of the scatter.

Abstract

We present a detailed analysis of the intrinsic scatter in the integrated SZ effect - cluster mass (Y-M) relation, using semi-analytic and simulated cluster samples. Specifically, we investigate the impact on the Y-M relation of energy feedback, variations in the host halo concentration and substructure populations, and projection effects due to unresolved clusters along the line of sight (the SZ background). Furthermore, we investigate at what radius (or overdensity) one should measure the integrated SZE and define cluster mass so as to achieve the tightest possible scaling. We find that the measure of Y with the least scatter is always obtained within a smaller radius than that at which the mass is defined; e.g. for M_{200} (M_{500}) the scatter is least for Y_{500} (Y_{1100}). The inclusion of energy feedback in the gas model significantly increases the intrinsic scatter in the Y-M relation due to larger variations in the gas mass fraction compared to models without feedback. We also find that variations in halo concentration for clusters of a given mass may partly explain why the integrated SZE provides a better mass proxy than the central decrement. Substructure is found to account for approximately 20% of the observed scatter in the Y-M relation. Above M_{200} = 2x10^{14} h^{-1} msun, the SZ background does not significantly effect cluster mass measurements; below this mass, variations in the background signal reduce the optimal angular radius within which one should measure Y to achieve the tightest scaling with M_{200}.