  Using the Planck far-infrared and Arecibo GALFA 21-cm line surveys, we
identified a set of isolated interstellar clouds (approximately degree-sized on
the sky and comprising 100 solar masses) and assessed the ratio of gas mass to
dust mass. Significant variations of the gas-to-dust ratio are found both from
cloud to cloud and within regions of individual clouds; within the clouds, the
atomic gas per unit dust decreases by more than a factor of 3 compared to the
standard gas-to-dust ratio. Three hypotheses are considered. First, the
apparently low gas-to-dust ratio could be due to molecular gas. Comparing to
Planck CO maps, the brightest clouds have a H2/CO ratio comparable to galactic
plane clouds, but a strong lower limit is placed on the ratio for other clouds,
such that the required amount of molecular gas is far higher than would be
expected based on the CO upper limits. Second, we consider self-absorbed 21-cm
lines and find the optical depth must be approximately 3, significantly higher
than found from surveys of radio sources. Third, grain properties may change
within the clouds: they become more emissive when they are colder, while not
utilizing heavy elements that already have their cosmic abundance fully locked
into grains. It is possible all three processes are active, and follow-up
studies will be required to disentangle them and measure the true total gas and
dust content of interstellar clouds.
