Templates for the Sunyaev-Zel'dovich Angular Power Spectrum
We present templates for the Sunyaev-Zel'dovich (SZ) angular power spectrum based on four models for the nonlinear gas distribution. The frequency-dependent SZ temperature fluctuations, with thermal (TSZ) and kinetic (KSZ) contributions, are calculated by tracing through a dark matter simulation, processed to include gas in dark matter halos and in the filamentary intergalactic medium. Different halo gas models are compared to study how star formation, energetic feedback, and nonthermal pressure support influence the angular power spectrum. The standard model has been calibrated to reproduce the stellar and gas fractions and X-ray scaling relations measured from low-redshift clusters and groups. The other models illustrate the current theoretical and empirical uncertainties relating to properties of the intracluster medium. Relative to the standard model, their angular power spectra differ by approximately ±50% (TSZ), ±20% (KSZ), and ±40% (SZ at 148 GHz) for l = 3000, σ8 = 0.8, and homogeneous reionization at z = 10. The angular power spectrum decreases in amplitude as gas mass and binding energy are removed through star formation, and as gas is pushed out to larger radii by energetic feedback. With nonthermal pressure support, less pressure is required to maintain hydrostatic equilibrium, thus reducing the thermal contribution to the SZ power. We also calculate the SZ templates as a function of σ8 and quantify this dependence. Assuming Cl ∝ (σ8/0.8)α, the effective scaling index ranges from 7 αTSZ 9, 4.5 αKSZ 5.5, and 6.5 αSZ (148 GHz) 8 at l = 3000 for 0.6 < σ8 < 1. The template spectra are publicly available and can be used when fitting for the SZ contribution to the cosmic microwave background on arcminute scales.