We present \sim 100 pc resolution Hubble Space Telescope H \alpha images of 10 galaxies from the DYnamics of Newly-Assembled Massive Objects ( DYNAMO ) survey of low- z turbulent disk galaxies , and use these to undertake the first detailed systematic study of the effects of resolution and clump clustering on observations of clumps in turbulent disks .
In the DYNAMO- HST sample we measure clump diameters spanning the range d _ { clump } \sim 100 - 800 pc , and individual clump star formation rates as high as \sim 5 M _ { \odot } yr ^ { -1 } .
DYNAMO clumps have very high SFR surface densities , \Sigma _ { SFR } \sim 1 - 15 M _ { \odot } yr ^ { -1 } kpc ^ { -2 } , \sim 100 \times higher than in H ii regions of nearby spirals .
Indeed , SFR surface density provides a simple dividing line between massive star forming clumps and local star forming regions , where massive star forming clumps have \Sigma _ { SFR } > 0.5 M _ { \odot } yr ^ { -1 } kpc ^ { -2 } .
When degraded to match the observations of galaxies in z \sim 1 - 3 surveys , DYNAMO galaxies are similar in morphology and measured clump properties to clumpy galaxies observed in the high- z Universe .
Emission peaks in the simulated high-redshift maps typically correspond to multiple clumps in full resolution images .
This clustering of clumps systematically increases the apparent size and SFR of clumps in 1 kpc resolution maps , and decreases the measured SFR surface density of clumps by as much as a factor of 20 \times .
From these results we can infer that clump clustering is likely to strongly effect the measured properties of clumps in high- z galaxies , which commonly have kiloparsec scale resolution .