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We explore the relationship between the thermal Sunyaev-Zel'dovich (tSZ)power spectrum amplitude and the halo mass and redshift of galaxy clusters inSouth Pole Telescope (SPT) data, in comparison with three $N$-body simulationscombined with semi-analytical gas models of the intra-cluster medium.Specifically, we calculate both the raw and fractional power contribution tothe full tSZ power spectrum amplitude at $\ell = 3000$ from clusters as afunction of halo mass and redshift. We use nine mass bins in the range $1\times 10^{14}\ M_\odot\ h^{-1} < M_{500} < 2 \times 10^{15}\ M_\odot\ h^{-1}$,and two redshift bins defined by $0.25 < z < 0.59$ and $0.59 < z < 1.5$. Weadditionally divide the raw power contribution in each mass bin by the numberof clusters in that bin, as a metric for comparison of different gas models. Atlower masses, the SPT data prefers a model that includes a mass-dependent boundgas fraction component and relatively high levels of AGN feedback, whereas athigher masses there is a preference for a model with a lower amount of feedbackand a complete lack of non-thermal pressure support. The former provides thebest fit to the data overall, in regards to all metrics for comparison. Still,discrepancies exist and the data notably exhibits a steep mass-dependence whichall of the simulations fail to reproduce. This suggests the need for additionalmass- and redshift-dependent adjustments to the gas models of each simulation,or the potential presence of contamination in the data at halo masses below thedetection threshold of SPT-SZ. Furthermore, the data does not demonstratesignificant redshift evolution in the per-cluster tSZ power spectrumcontribution, in contrast to self-similar model predictions.

Dissecting the Thermal SZ Power Spectrum by Halo Mass and Redshift in SPT-SZ Data and Simulations