Stellar masses of clumps in gas-rich, turbulent disc galaxies

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