  An understanding of astrophysical feedback is important for constraining
models of galaxy formation and for extracting cosmological information from
current and future weak lensing surveys. The thermal Sunyaev-Zel'dovich effect,
quantified via the Compton-$y$ parameter, is a powerful tool for studying
feedback, because it directly probes the pressure of the hot, ionized gas
residing in dark matter halos. Cross-correlations between galaxies and maps of
Compton-$y$ obtained from cosmic microwave background surveys are sensitive to
the redshift evolution of the gas pressure, and its dependence on halo mass. In
this work, we use galaxies identified in year one data from the Dark Energy
Survey and Compton-$y$ maps constructed from Planck observations. We find
highly significant (roughly $12\sigma$) detections of galaxy-$y$
cross-correlation in multiple redshift bins. By jointly fitting these
measurements as well as measurements of galaxy clustering, we constrain the
halo bias-weighted, gas pressure of the Universe as a function of redshift
between $0.15 \lesssim z \lesssim 0.75$. We compare these measurements to
predictions from hydrodynamical simulations, allowing us to constrain the
amount of thermal energy in the halo gas relative to that resulting from
gravitational collapse.
