Gas Content and Kinematics in Clumpy, Turbulent Star-forming Disks
  We present molecular gas mass estimates for a sample of 13 local galaxies
whose kinematic and star forming properties closely resemble those observed in
$z\approx 1.5$ main-sequence galaxies. Plateau de Bure observations of the
CO[1-0] emission line and Herschel Space Observatory observations of the dust
emission both suggest molecular gas mass fractions of ~20%. Moreover, dust
emission modeling finds $T_{dust}<$30K, suggesting a cold dust distribution
compared to their high infrared luminosity. The gas mass estimates argue that
$z\sim$0.1 DYNAMO galaxies not only share similar kinematic properties with
high-z disks, but they are also similarly rich in molecular material. Pairing
the gas mass fractions with existing kinematics reveals a linear relationship
between $f_{gas}$ and $\sigma$/$v_{c}$, consistent with predictions from
stability theory of a self-gravitating disk. It thus follows that high gas
velocity dispersions are a natural consequence of large gas fractions. We also
find that the systems with lowest depletion times ($\sim$0.5 Gyr) have the
highest ratios of $\sigma$/$v_{c}$ and more pronounced clumps, even at the same
high molecular gas fraction.
