deletions | additions       diff --git a/subsection_Cluster_parameter_estimation_Cluster__.tex b/subsection_Cluster_parameter_estimation_Cluster__.tex  index 5e8f476..decf696 100644  --- a/subsection_Cluster_parameter_estimation_Cluster__.tex  +++ b/subsection_Cluster_parameter_estimation_Cluster__.tex 
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\subsection{Cluster parameter estimation}  Cluster parameters were estimated through comparison to synthetic photometry produced by the Flexible Stellar Population Synthesis (FSPS) code \citep{Conroy_2009,Conroy_2010}. Padova isochrones \citep{Marigo_2008} were used with the BaSeL stellar library \citep{Westera_2002}.  Model points were generated from simulations with information on age, extinction, and metallicity as well as the magnitudes a $1$ M$_{sun}$ star with those properties would have under all desired HST filters. The points were arranged as a parameter-space``lattice'', where the allowed ages ranged from $10^{5.5}-10^{10.175}$ years on a log scale incrementing by $0.125$, allowed metallicities ranged from $1-22$ in increments of 1, where 20 is solar metallicity. Extinctions ranged from $0-3.0$ in increments of $0.25$.   Photometric data were obtained using the PYRAF task {\bf phot} and were converted to absolute magnitudes by subtracting the distance modulus of the galaxy from the magnitude of the cluster. The magnitudes of each cluster and each model point were then converted to ``colors'' by subtracting magnitudes at different filters from one another. Since this process depended on which filters the galaxy had images in, but the result was always three to four linearly independent colors depending on the number of usable images; in the case of ngc-3032: NUV-V, F475W-V, and V-I were the three colors used.     For each catalog point, a list of the Chi-squared value comparing it to each model point was compiled using the equation:   
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