deletions | additions       diff --git a/section_Science_1_Clumps_citep__.tex b/section_Science_1_Clumps_citep__.tex  index 9a1f86d..f59700e 100644  --- a/section_Science_1_Clumps_citep__.tex  +++ b/section_Science_1_Clumps_citep__.tex 
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With the GZH data, we would be able to:  Identify classes of clump distributions in clumpy galaxies  Investigate what physical processes may give rise to different clump morphologies. Elmegreen acknowledges that the different morphological types may not imply physical differences; ex double clumps may simply be smaller versions of chains, or chain galaxies and clump clusters may be identical but viewed at different angles. They identified ~100 galaxies / morphological type and did not find significant differences in the distributions of colors between the samples. With N_arrangement > 10 and p_line > 0.6, I find 700 galaxies which are highly likely to be of the chain morphological type; thus we can expect to have significantly larger samples to compare.   Things to compare between types:  -Environment - nearest neighbor? Not sure what data exists  -Colors  -SFR, can we measure per clump...?  -Clump size; perhaps there are size constraints limiting how clumps can be arranged?   -redshift - how do distributions evolve spatially over time?