Thermal and non-thermal Sunyaev-Zel'dovich effect in the cavities of the galaxy cluster MS 0735.6+7421: the role of the thermal density in the cavity

TL;DR

This paper investigates how thermal and non-thermal electron populations in galaxy cluster cavities influence the Sunyaev-Zel'dovich effect, highlighting the importance of thermal density in interpreting observational data.

Contribution

It provides a detailed analysis of the interplay between thermal and non-thermal SZ effects in galaxy cluster cavities, emphasizing the role of thermal density and identifying optimal frequencies for disentangling contributions.

Findings

Non-thermal SZ effect dominates at temperatures >1500 keV.

High frequencies (>500 GHz) are optimal for separating thermal and non-thermal SZ effects.

Thermal density significantly influences the strength of the non-thermal SZ effect.

Abstract

The galaxy cluster MS 0735.6+7421 hosts two large X-ray cavities, filled with radio emission, where a decrease of the Sunyaev-Zel'dovich (SZ) effect has been detected, without establishing if its origin is thermal (from a gas with very high temperature) or non-thermal. In this paper we study how thermal and non-thermal contributions to the SZ effect in the cavities are related; in fact, Coulomb interactions with the thermal gas modify the spectrum of low energy non-thermal electrons, which dominate the non-thermal SZ effect; as a consequence, the intensity of the non-thermal SZ effect is stronger for lower density of the thermal gas inside the cavity. We calculate the non-thermal SZ effect in the cavities as a function of the thermal density, and compare the SZ effects produced by thermal and non-thermal components, and with the one from the external Intra Cluster Medium (ICM), searching for the best frequency range where it is possible to disentangle the different contributions. We find that for temperatures inside the cavities higher than $\sim1500$ keV the non-thermal SZ effect is expected to dominate on the thermal one, particularly at high frequencies ($\nu>500$ GHz), where it can also be a non-negligible fraction of the SZ effect from the external ICM. We also discuss the possible sources of astrophysical bias (as kinetic SZ effect and foreground emission from Galactic dust) and possible ways to address them, as well as necessary improvements in the modeling of the properties of cavities and the ICM.