deletions | additions       diff --git a/subsection_Age_vs_lots_of__.tex b/subsection_Age_vs_lots_of__.tex  index 7281b32..c719fdf 100644  --- a/subsection_Age_vs_lots_of__.tex  +++ b/subsection_Age_vs_lots_of__.tex 
...
What has been done:   \citet{Mandelker2015}: Analyzed clumps in simulated high-redshift galaxies, found radiative pressure feedback can lower the stellar mass by a factor of 2 at $z=2$, or increase by a factor of 10 in low-mass galaxies.   \citet{Ma2015}:   What we'd need: stellar mass measurements  
...
\subsection{Morphological changes over time}  Current observations suggest that a large fraction of originally-disk galaxies can change morphology into elliptical shape. Does this transformation occur around the same time for all disks? Can disks spontaneously lose their disk structure over time, or does it have to undergo an interaction with another galaxy to transform? Is there a third option? Are there any very old disk galaxies, or do they all lose their disk structure at some point?   \subsection{Mass-Metallicity relation over time}  There is a reasonably-tight correlation between mass and metallicity - lower mass galaxies tend to be more metal-poor. Possible indication that low mass galaxies are at an earlier evolutionary stage and still have to convert most of their mass to stars, where massive galaxies are already evolved. This could be checked by analyzing this relationship at different redshifts.  \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.