Quantifying the Thermal Sunyaev-Zel'dovich Effect and Excess Millimeter
  Emission in Quasar Environments
  In this paper we probe the hot, post-shock gas component of quasar-driven
winds through the thermal Sunyaev-Zel'dovich (tSZ) effect. Combining datasets
from the Atacama Cosmology Telescope, the $\textit{Herschel}$ Space
Observatory, and the Very Large Array, we measure average spectral energy
distributions (SEDs) of 109,829 optically-selected, radio quiet quasars from
1.4~GHz to 3000~GHz in six redshift bins between $0.3<z<3.5$. We model the
emission components in the radio and far-infrared, plus a spectral distortion
from the tSZ effect. At $z>1.91$, we measure the tSZ effect at $3.8\sigma$
significance with an amplitude corresponding to a total thermal energy of
$3.1\times10^{60}$ ergs. If this energy is due to virialized gas, then our
measurement implies quasar host halo masses are
$\sim6\times10^{12}~h^{-1}$M$_\odot$. Alternatively, if the host dark matter
halo masses are $\sim2\times10^{12}~h^{-1}$M$_\odot$ as some measurements
suggest, then we measure a $>$90 per cent excess in the thermal energy over
that expected due to virialization. If the measured SZ effect is primarily due
to hot bubbles from quasar-driven winds, we find that $(5^{+1.2}_{-1.3}$) per
cent of the quasar bolometric luminosity couples to the intergalactic medium
over a fiducial quasar lifetime of 100 Myr. An additional source of tSZ may be
correlated structure, and further work is required to separate the
contributions. At $z\leq1.91$, we detect emission at 95 and 148~GHz that is in
excess of thermal dust and optically thin synchrotron emission. We investigate
potential sources of this excess emission, finding that CO line emission and an
additional optically thick synchrotron component are the most viable
candidates.
