deletions | additions       diff --git a/subsubsection_Bivariate_mas_size_distributions__.tex b/subsubsection_Bivariate_mas_size_distributions__.tex  index 1c236d5..de8dc6d 100644  --- a/subsubsection_Bivariate_mas_size_distributions__.tex  +++ b/subsubsection_Bivariate_mas_size_distributions__.tex 
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\textit{\textbf{M. R. Beck et al.}}\\  Better:\\  It is well known that the mass-size distribution evolves as a function of cosmic time and that this evolution is different between passive and star-forming galaxy populations. However, the devil is in the details and the precise evolution is still a matter of debate since this requires careful comparison between similar galaxy populations over cosmic time while simultaneously taking into account changes in image resolution, rest-frame wavelength, and surface brightness dimming in addition to properly selecting representative morphological samples.   Here we present the first step in an ambitious undertaking to calculate the bivariate mass-size distribution as a function of time and morphology. We begin with a large sample ($\sim300$ K) of SDSS galaxies at $z\sim.1$. Morphologies for this sample have been determined by Galaxy Zoo crowdsourced visual classifications. We demonstrate how the wealth of Galaxy Zoo classifications can be used not only to separate disk- and bulge-dominated galaxy populations but can also probe sub-classifications such as bulge strength.  Bivariate distribution functions are the only way to properly account for biases and selection effects. In particular, we quantify the mass-size distribution with a version of the parametric Maximum Likelihood estimator which has been modified to account for measurement errors as well as upper limits on galaxy sizes.We demonstrate how the wealth of Galaxy Zoo classifications can be used not only to separate disk- and bulge- dominated galaxy populations but can also probe sub-classifications such as bulge strength.  \textit{Closing sentence ... it's just dangling right now.} \\