Stellar Masses of Clumps in Gas-rich, Turbulent Disk Galaxies
  In this paper we use HST/WFC3 observations of 6 galaxies from the DYNAMO
survey, combined with stellar population modelling of the SED, to determine the
stellar masses of DYNAMO clumps. The DYNAMO sample has been shown to have
properties similar to $z\approx1.5$ turbulent, clumpy disks. DYNAMO sample
clump masses offer a useful comparison for studies of $z>1$ in that the
galaxies have the same properties, yet the observational biases are
significantly different. Using DYNAMO we can more easily probe rest-frame
near-IR wavelengths and also probe finer spatial scales. We find that the
stellar mass of DYNAMO clumps is typically $10^{7}-10^8 \mathrm{M}_\odot$. We
employ a technique that makes non-parametric corrections in removal of light
from nearby clumps, and carries out a locally determined disk subtraction. The
process of disk subtraction is the dominant effect, and can alter clump masses
at the 0.3~dex level. Using these masses, we investigate the stellar mass
function of clumps in DYNAMO galaxies. DYNAMO stellar mass functions follow a
declining power law with slope $\alpha \approx -1.4$, which is slightly
shallower than, but similar to what is observed in $z>1$ lensed galaxies. We
compare DYNAMO clump masses to results of simulations. The masses and
galactocentric position of clumps in DYNAMO galaxies are more similar to
long-lived clumps in simulations. Similar to recent DYNAMO results on the
stellar population gradients, these results are consistent with simulations
that do not employ strong "early" radiative feedback prescriptions.
