deletions | additions       diff --git a/reconstructed_wedges.tex b/reconstructed_wedges.tex  index 28c3802..5ee211b 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{Eisenstein_2007} showed that the blurring of the baryonic peak due large-scale coherent motions of galaxies could be remedied by through a procedure of linear reconstrcution of the density-field.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 through a procedure of linear reconstrcution of the density-field.  In practice we estimate estimated  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 anistropic baryonic signature. Figure \ref{fig:z60_model_figure} displays our results for the clustering wedges $\xi_{||}$ (line-of-sight; red circles) and $\xi_{\perp}$ (transverse; blue circles) in the three redshift ranges investigated $\Delta z^{\rm Near}$, $\Delta z^{\rm Mid}$ and $\Delta z^{\rm Far}$ with best fit models of $\chi^2=35.3, \ 24.8, \ 34.4$ with 36 dof, respectively. We clearly see baroynic acoustic signatures in both $\xi_{\perp}$ and $\xi_{||}$ of all three redshift ranges. The reason that there is no apparent gap as in the pre-reconstruction case, is that the reconstruction procedure corrects for the Kaiser-effect (cite Kaiser) by adding a line-of-sight term correction to $\vec{\psi}$, which envolves   estimating the rate of growth of structure $f$ and linear bias $b$ in Equation 3 of \cite{Kazin_2014}.