deletions | additions       diff --git a/reconstructed_wedges.tex b/reconstructed_wedges.tex  index 1da7081..4ad100b 100644  --- a/reconstructed_wedges.tex  +++ b/reconstructed_wedges.tex 
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We now use the baroynic acoustic feature as a standardized sphere to determine $D_{\rm A}/r_{\rm s}$ and $1/H/r_{\rm s}$. We use the procedure used in (cite Kazin and Sanchez) to use information from the peak positions, and marginalize on over the shape information. This is performed by ... template fitting ... MCMC... The effectively yields model-independant constraints. In all results presented we use flat priors of $D_{\rm A}/r_{\rm s}$ and $1/H/r_{\rm s}$ between [0.5,1.5] of their fiducial cosmology values.   In Figure \ref{fig:HDA_z60_nopriors} we present the results for $0.6~ \sim  1/H/D_{\rm A}$. To assess reasonable priors on $\alpha$ and $\epsilon$, we examine propositions of MCMC when analyzing the Planck temperature anisotropies and examine predictions for $\alpha$ and $\epsilon$ at our redshifts of interest ($0.44,0.6,0.73$). Assuming an $ow$CDM model, we obtain a 68\% CL region of $22\%$ for $\alpha$ and $\sim 2.5\%$ for $\epsilon$. Examining a more restrictive flat-$\Lambda$CDM model we find a 68\% CL region of $2\%$ for $\alpha$ and similar for $\epsilon$. We argue that the reason the $\alpha$ of Planck are sensitive to assumption of flatness and $w$ and $\epsilon$ is not is due to the capability of Planck to constrain $H_{\rm 0}$, which $\alpha$ is sensitive to, but $\epsilon$ is not.