deletions | additions       diff --git a/section_Science_1_Clumps_citep__.tex b/section_Science_1_Clumps_citep__.tex  index 13b875f..de671b6 100644  --- a/section_Science_1_Clumps_citep__.tex  +++ b/section_Science_1_Clumps_citep__.tex 
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[paragraph about what has been done @ high redshift, how can we do similar/more with GZH]  Although clumpy galaxies are most abundant at high redshift, there is a significant population that exist locally (z < 0.2). Analysis of this population is ideal for revealing the finer substructure of the clumps, which have typical sizes of 100pc ~ $\sim$  1kpc. HST/ACS imaging is capable of resolving [some size] at z=0.2, while SDSS can only resolve features of [this size] at the same redshift.