  As the most common environment in the universe, groups of galaxies are likely
to contain a significant fraction of the missing baryons in the form of
intergalactic gas. The density of this gas is an important factor in whether
ram pressure stripping and strangulation affect the evolution of galaxies in
these systems. We present a method for measuring the density of intergalactic
gas using bent-double radio sources that is independent of temperature, making
it complementary to current absorption line measurements. We use this method to
probe intergalactic gas in two different environments: inside a small group of
galaxies as well as outside of a larger group at a 2 Mpc radius and measure
total gas densities of $4 \pm 1_{-2}^{+6} \times 10^{-3}$ and $9 \pm
3_{-5}^{+10} \times 10^{-4}$ per cubic centimeter (random and systematic
errors) respectively. We use X-ray data to place an upper limit of $2 \times
10^6$ K on the temperature of the intragroup gas in the small group.
