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Eyal Kazin edited 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.
\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. In practice we estimated the linear displacement vectors $\vec{\psi}$ of the galaxies in grid-cells of length 5 $h^{-1}$Mpc, and
shift shifted 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.