deletions | additions       diff --git a/reconstructed_wedges.tex b/reconstructed_wedges.tex  index f4d9610..cf96d55 100644  --- a/reconstructed_wedges.tex  +++ b/reconstructed_wedges.tex 
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To quantify the significant of detection of the anisotropic baryonic feature in the WiggleZ clustering wedges we compare $\chi^2$ results obtained with best fit models using a $\Lambda$CDM-based template to a ``no-wiggle"-based template, i.e, one with full shape and no baryonic feature \cite{Eisenstein_1998} ($\Delta\chi^2\equiv \chi^2_{\rm min \ no-wiggle}-\chi^2_{\rm min \ \Lambda CDM}$). In this procedure, for each model we vary $H r_{\rm s}$ and $D_{\rm A}/r_{\rm s}$ and marginalize over all other shape parameters, as explained in detail in \S 6.1 of \citet{Kazin_2013}. We find that the significance of detection, quantifies by $\sqrt{\Delta\chi^2}$ for $\Delta z^{\rm Near}$, $\Delta z^{\rm Mid}$ and $\Delta z^{\rm Far}$ to be $1.6, \ 2.7$ and $2.9$, respectively  We now use the baroynic acoustic feature as a standardized sphere to determine $D_{\rm A}/r_{\rm s}$ and $1/H/r_{\rm s}$. To obtain model-independent constraints we focus on the information contained the peak positions in $\xi_{||, \ \perp}$ and marginalize over the broad shape. This is performed by using a template based on $\Lambda$CDM based and using slight peak damping as due to coupling of $k-$modes, and described in the rernomalized perturbation theory of \citet{Crocce_2008}. Assuming perfect For simplicity we assume  reconstruction correction of the perfectly corrects for  linear anisotropic we set anisotropies, by setting  all \xi multipoles except for the monopole to be zero.For our results here we ran MCMC zero. We run MC-Markov chain when  fitting the models to the data  while varying $D_{\rm A}/r_{\rm s}$ and $1/H/r_{\rm s}$ with flat prior between [0.5,1.5] of their fiducial cosmology values. In addition we vary for each clustering wedge and amplitude parameter and three polynomial terms each, yielding 10 parameters in total. total (2+2+2X3).  In the results presented here we marginalize over these last eight parameters. A full detailed description of the procedure is described given  in our previous analysis of the SDSS DR9 CMASS galaxies \citet{Kazin_2013} (see \S 5.3). In Figure \ref{fig:HDA_z60_nopriors} we present the results for $0.6