deletions | additions       diff --git a/reconstructed_wedges.tex b/reconstructed_wedges.tex  index dd87c96..57e2273 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 the model-independent constraints on $H$ and $D_{\rm A}$ obtained from them. We test our methodology and compare our results with those obtained when applied on the WiZCOLA mocks.   In \citet{Kazin_2014} we reported application of the reconstruction of the density field technique,   and have shown it useful for sharpening of the angel-averaged  baryonic feature, and hence improved usage as a standard ruler. \citet{Eisenstein_2007} showed that the blurring of the baryonic peak due large-scale coherent motions of galaxies could be remedied by using the density-field information. In practice we estimate the linear displacement vectors $\vec{\psi}$ of the galaxies in grid-cells of length 5 $h^{-1}$Mpc, and shift them by $-\vec{\psi}$. To overcome edge effects and holes within the survey, we apply a Weiner filter procedure similar to that presented in \citet{Padmanabhan_2012}. For full details of the procedure please refer to \S 2.3 in \cite{Kazin_2014}.  Here we examine implications of the reconstruction technique on the WiggleZ anistorpic baryonic signature.