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We present a case study of stellar clumps in G04-1, a clumpy, turbulent diskgalaxy located at $z$ = 0.13 from the DYNAMO sample, using adaptive opticsenabled K-band imaging ($\sim2.25$ kpc/arcsec) with Keck/NIRC2. We identify 15stellar 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 $\sim2.9 \times10^{7}\ \rm M_{\odot}$. Note that these masses decrease by about one-half whenwe apply a light correction for the underlying stellar disk. A majority (12 of15) of clumps observed in the $K_{P}$-band imaging have associated componentsin H$\alpha$ maps ($\sim2.75$ kpc/arcsec; $<$R$_{clump}> \sim$500 pc) andappear co-located ($\overline{\Delta x} \sim 0.1$ arcsec). Using Hubble SpaceTelescope WFC/ACS observations with the F336W and F467M filters, we also findevidence of radial trends in clump stellar properties: clumps closer to thecentre of G04-1 are more massive (consistent with observations at high-$z$) andappear more red, suggesting they may be more evolved. Using our high-resolutiondata, we construct a star forming main sequence for G04-1 in terms ofspatially-resolved quantities and find that all regions (both clump andintra-clump) within the galaxy are experiencing an enhanced mode of starformation routinely observed in galaxies at high-$z$. In comparison to recentsimulations, 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.

K-Band Imaging of the Nearby, Clumpy Turbulent Disk Galaxy DYNAMO G04-1