K-Band Imaging of the Nearby, Clumpy Turbulent Disk Galaxy DYNAMO G04-1
  We present a case study of stellar clumps in G04-1, a clumpy, turbulent disk
galaxy located at $z$ = 0.13 from the DYNAMO sample, using adaptive optics
enabled K-band imaging ($\sim2.25$ kpc/arcsec) with Keck/NIRC2. We identify 15
stellar clumps in G04-1 with a range of masses from $3.6 \times 10^{6}$ to $2.7
\times 10^{8}\ \rm M_{\odot}$, and with a median mass of $\sim2.9 \times
10^{7}\ \rm M_{\odot}$. Note that these masses decrease by about one-half when
we apply a light correction for the underlying stellar disk. A majority (12 of
15) of clumps observed in the $K_{P}$-band imaging have associated components
in H$\alpha$ maps ($\sim2.75$ kpc/arcsec; $<$R$_{clump}> \sim$500 pc) and
appear co-located ($\overline{\Delta x} \sim 0.1$ arcsec). Using Hubble Space
Telescope WFC/ACS observations with the F336W and F467M filters, we also find
evidence of radial trends in clump stellar properties: clumps closer to the
centre of G04-1 are more massive (consistent with observations at high-$z$) and
appear more red, suggesting they may be more evolved. Using our high-resolution
data, we construct a star forming main sequence for G04-1 in terms of
spatially-resolved quantities and find that all regions (both clump and
intra-clump) within the galaxy are experiencing an enhanced mode of star
formation routinely observed in galaxies at high-$z$. In comparison to recent
simulations, our observation of a number of clumps with masses $10^{7}-10^{8}\
\rm M_{\odot}$ is not consistent with strong radiative feedback in this galaxy.
