deletions | additions       diff --git a/subsection_Age_vs_lots_of__.tex b/subsection_Age_vs_lots_of__.tex  index 1fca423..6d8ca2f 100644  --- a/subsection_Age_vs_lots_of__.tex  +++ b/subsection_Age_vs_lots_of__.tex 
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\citet{Maiolino2008} found that at fixed stellar mass, galaxies at higher redshift tend to be more metal-poor than those at low redshift. Paper focuses on z>3 sample of galaxies, pulls lower redshift data from other sources for comparison. Current data suggests a downsizing effect - high mass galaxies reach high metallicities at high redshift quickly, while low mass systems enrich ISM over long period of time; caveat that thus far these results are subject to low sample statistics, and more data is needed to make claim with confidence.   \subsection{Clumps and large-scale morphology}  We find more clumpy galaxies at higher redshift -> redshift, which implies  star formation likes to occur in clumps that dissipate over time. It's also believed that galaxies form as disks and only later can transform to ellipticals - how does clumpiness fit into this process? Do all clumpy galaxies have a disk shape, or are they irregularly shaped? Is the galaxy formation model clumpy disk -> disk -> elliptical, or is there a clumpy irregular stage before the disk develops?