  We search for signatures of cosmological shocks in gas pressure profiles of
galaxy clusters using the cluster catalogs from three surveys: the Dark Energy
Survey (DES) Year 3, the South Pole Telescope (SPT) SZ survey, and the Atacama
Cosmology Telescope (ACT) data releases 4, 5, and 6, and using thermal
Sunyaev-Zeldovich (SZ) maps from SPT and ACT. The combined cluster sample
contains around $10^5$ clusters with mass and redshift ranges $10^{13.7} <
M_{\rm 200m}/M_\odot < 10^{15.5}$ and $0.1 < z < 2$, and the total sky coverage
of the maps is $\approx 15,000 \,\,{\rm deg}^2$. We find a clear pressure
deficit at $R/R_{\rm 200m}\approx 1.1$ in SZ profiles around both ACT and SPT
clusters, estimated at $6\sigma$ significance, which is qualitatively
consistent with a shock-induced thermal non-equilibrium between electrons and
ions. The feature is not as clearly determined in profiles around DES clusters.
We verify that measurements using SPT or ACT maps are consistent across all
scales, including in the deficit feature. The SZ profiles of optically selected
and SZ-selected clusters are also consistent for higher mass clusters. Those of
less massive, optically selected clusters are suppressed on small scales by
factors of 2-5 compared to predictions, and we discuss possible interpretations
of this behavior. An oriented stacking of clusters -- where the orientation is
inferred from the SZ image, the brightest cluster galaxy, or the surrounding
large-scale structure measured using galaxy catalogs -- shows the normalization
of the one-halo and two-halo terms vary with orientation. Finally, the location
of the pressure deficit feature is statistically consistent with existing
estimates of the splashback radius.
