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

Abstract

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 ($\sim 2.25$ 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 $2.7\times 10^8{\mathrm{M}}_{\odot }$, and with a median mass of $\sim 2.9\times 10^7{\mathrm{M}}_{\odot }$. 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 ($\sim 2.75$ 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 $10^7-10^8{\mathrm{M}}_{\odot }$ is not consistent with strong radiative feedback in this galaxy.

18 pages, 7 figures. Accepted to The Astrophysical Journal (ApJ)

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