deletions | additions       diff --git a/reconstructed_wedges.tex b/reconstructed_wedges.tex  index 4882fcd..477ca97 100644  --- a/reconstructed_wedges.tex  +++ b/reconstructed_wedges.tex 
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Here we apply the techhnique of reconstruction of the baroynic acoustic feature on the WiggleZ data, present the results in the form of clustering wedges, and describe constraints on $H$ and $D_{\rm A}$. We test our methodology and compare our results with those obtained when applied on the WiZCOLA mocks.   In \cite{Kazin_2014} we reported application of the reconstruction of the density field technique,   and have shown it useful for sharpening of the baryonic feature, and hence improved usage as a standard ruler. \cite{Eisenstein_2007} showed that the blurring of the baryonic peak due large-scale coherent motions of galaxies could be remidied by using the density-field information. In practice this procedure involves estimating the linear displacement vectors $\vec{\psi}$  of the galaxies in grid-cells of length 5 $h^{-1}$Mpc, and shifting them by $-\psi$. To overcome edge effects and holes within the survey We follow a Weiner filter procedure similar to that presented in \cite{Padmanabhan_2012}, which   Here we examine implications of the technique on the anistorpic baryonic signature. Figure (currently experienceing referencing problems ...) displays our results for the clustering wedges $\xi$ in the range $0.6