  We use observational measurements of thermal and kinetic Sunyaev-Zel'dovich
effects, as well as soft X-ray emission associated with galaxy groups to
constrain the gas density and temperature in the circumgalactic medium (CGM)
for dark matter halos with masses above $10^{12.5}M_{\odot}$. A number of
generic models are used together with a Bayesian scheme to make model
inferences. We find that gas with a single temperature component cannot provide
a consistent model to match the observational data. A simple two-phase model
assuming a hot component and an ionized warm component can accommodate all the
three observations. The total amount of the gas in individual halos is inferred
to be comparable to the universal baryon fraction corresponding to the halo
mass. The inferred temperature of the hot component is comparable to the halo
virial temperature. The fraction of the hot component increases from
$(15-40)\%$ for $10^{12.5}{M}_\odot$ halos to $(40-60)\%$ for
$10^{14.5}{M}_\odot$ halos, where the ranges reflect uncertainties in the
assumed gas density profile. Our results suggest that a significant fraction of
the halo gas is in a non-thermalized component with temperature much lower than
the virial temperature.
