All Figures

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{3939_f01.eps} \end{figure}$ Figure 1: Acoustic oscillations in the CMB ( upper panel) and linear matter power spectrum ( lower panel) for the "concordance'' cosmological model. Here, as we have plotted the spectra against spatial wavenumber k, we have changed the standard notation of $C_\ell$ to C_k. Due to the k³ factor the first CMB acoustic peak is barely visible. Density fluctuations in matter at smaller scales, being mostly induced by the velocity fields, are out of phase with respect to the fluctuations in the CMB component. The fluctuation period is also twice as large.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3939_f02.eps} \end{figure}$ Figure 2: Comoving number density of galaxies as a function of comoving distance. Smooth solid line shows a cubic spline fit to the number density estimated for 50 discrete radial bins.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3939_f03.eps} \end{figure}$ Figure 3: Angular distribution of galaxies given in the SDSS survey coordinates $(\lambda ,\eta )$ . The survey mask is shown with solid lines. The vertical dashed lines show the division of the sample into 22 separate regions each containing $\sim$ 2350 galaxies. This division will be exploited in the "jackknife'' error analysis of the correlation function.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3939_f04.eps} \end{figure}$ Figure 4: Power spectrum of the SDSS LRG sample with the bin width $\Delta k \simeq 0.005 ~h~{\rm Mpc}^{-1}$ . The upper solid line shows the best fitting model spectrum and the lower one corresponds to the linearly evolved matter power spectrum of the "concordance'' cosmological model multiplied by the square of the bias parameter b=1.95. Both of the spectra are convolved with a survey window. The dashed lines represent the corresponding unconvolved spectra.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3939_f05.eps} \end{figure}$ Figure 5: Power spectrum of the SDSS LRG sample with the bin width $\Delta k \simeq 0.02 ~h~{\rm Mpc}^{-1}$ . The upper solid line shows the best fitting model spectrum and the lower one corresponds to the linearly evolved matter power spectrum of the "concordance'' cosmological model multiplied by the square of the bias parameter b=1.95. Both of the spectra are convolved with a survey window. The dashed lines represent the "smoothed'' versions of the above model spectra. The dotted line is the cubic spline fit to the data points.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3939_f06.eps}\end{figure}$ Figure 6: The comparison of the different power spectrum error estimates. For clarity slight relative shifts of the data points have been applied. The errorbars resulting from the 1st method are the rightmost ones and the ones from the 3rd method are displayed in the middle. The lines show cubic spline fits to the data points. The solid line corresponds to the case when all the available galaxy data is used to find the angular mask of the survey, while the dashed line represents the case when LRGs only are used for this purpose.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=16.5cm,clip]{3939_f07.eps} \end{figure}$ Figure 7: Covariance ( left column) and correlation matrices ( right column). Top row represents the results from the FKP prescription (see Eq. (18)) and the middle row the ones from 1000 mock catalogs. The last row displays the nonlinear contribution due to the 1-halo term.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3939_f08.eps} \end{figure}$ Figure 8: Isotropized survey window. Here the normalization is taken such that |W(0)|=1. The light gray stripe marks the region where the window is above $1\%$ of its maximum value of 1. Dashed lines show approximations discussed in the text.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=90,width=7.5cm,clip]{3939_f09.ps}\end{figure}$ Figure 9: 3D survey window embedded in a box with a side length of $0.04~h~{\rm Mpc}^{-1}$ . Here the isosurface corresponding to $1\%$ of the maximum value of the window is shown. Note the symmetry of the window, $\vert W(\vec{k})\vert^2=\vert W(-\vec{k})\vert^2$ , as expected when taking a modulus of the Fourier transform of a real 3D scalar function.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{3939_f10.eps} \end{figure}$ Figure 10: Coupling kernels $K_i(k)\equiv K(k_i,k)$ for the power spectrum bins k_i shown in Fig. 5. Numerically evaluated kernels are shown with solid lines. The dashed lines correspond to the fitting functions given in Appendix D.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{3939_f11.eps} \end{figure}$ Figure 11: $1\sigma$ error contours for the free model parameters. Best fit parameter values are marked with crosses.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3939_f12.eps} \end{figure}$ Figure 12: Upper panel: power spectrum from Fig. 5 divided by the best fitting "smoothed'' spectrum. Solid line shows a cubic spline fit to the data points and long-dashed line corresponds to the best "wiggly'' model. The short-dashed line represents the most favorable fit from the parametric family of Eq. (28). Lower panel: various input power spectra used to calculate the two-point correlation function. The dashed line is the cubic spline fit from the upper panel. The solid lines represent a transition sequence from the best fitting "wiggly'' model to the best "smoothed'' model. In each step we have erased more oscillatory features. For clarity slight vertical shifts have been introduced.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3939_f13.eps} \end{figure}$ Figure 13: Left panel: two-point correlation functions as determined in this paper (circles with solid lines) and by Eisenstein et al. (2005). Right panel: correlation functions corresponding to the models shown in the lower panel of Fig. 12 in comparison to the one obtained directly from the data. Here all the data points have been lowered by 0.0035.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3939_f14.eps} \end{figure}$ Figure 14: The comparison of spectra from different surveys.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3939_f15.eps} \end{figure}$ Figure 15: The same as Fig. 14 with the errorbars omitted.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{3939_f16.eps} \end{figure}$ Figure A.1: Power spectra of galaxy clusters from the z=0 Hubble Volume simulation box. The solid line represents the spectrum for the full sample of 1 560 995 clusters. The circles with errorbars denote the recovered spectrum from the 50 mock catalogs having similar selection effects as the analyzed SDSS LRG sample. The dotted lines demonstrate the convolution effect of the survey window on the best fitting model spectrum.

In the text

$\begin{figure} \par\includegraphics[width=11cm,clip]{3939_f17.ps} \end{figure}$ Figure B.1: A $25~h^{-1}~{\rm Mpc}$ thick slice through a $1280~h^{-1}~{\rm Mpc}$ computational box. The gray scale image represents the underlying density field obtained by the optimized 2LPT approach. White dots mark the positions of the "galaxies'' generated by the Poisson sampler.

In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3939_f18.eps}\end{figure}$ Figure B.2: The power spectrum of $\sim$ 350 000 "galaxies'' from the simulation box shown in Fig. B.1. The solid line shows the linearly evolved input spectrum multiplied by the square of the bias parameter b=2.0.

In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3939_f02.eps} \end{figure}$	Figure 2: Comoving number density of galaxies as a function of comoving distance. Smooth solid line shows a cubic spline fit to the number density estimated for 50 discrete radial bins.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3939_f03.eps} \end{figure}$	Figure 3: Angular distribution of galaxies given in the SDSS survey coordinates $(\lambda ,\eta )$ . The survey mask is shown with solid lines. The vertical dashed lines show the division of the sample into 22 separate regions each containing $\sim$ 2350 galaxies. This division will be exploited in the "jackknife'' error analysis of the correlation function.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=16.5cm,clip]{3939_f07.eps} \end{figure}$	Figure 7: Covariance ( left column) and correlation matrices ( right column). Top row represents the results from the FKP prescription (see Eq. (18)) and the middle row the ones from 1000 mock catalogs. The last row displays the nonlinear contribution due to the 1-halo term.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3939_f08.eps} \end{figure}$	Figure 8: Isotropized survey window. Here the normalization is taken such that \|W(0)\|=1. The light gray stripe marks the region where the window is above $1\%$ of its maximum value of 1. Dashed lines show approximations discussed in the text.
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=90,width=7.5cm,clip]{3939_f09.ps}\end{figure}$	Figure 9: 3D survey window embedded in a box with a side length of $0.04~h~{\rm Mpc}^{-1}$ . Here the isosurface corresponding to $1\%$ of the maximum value of the window is shown. Note the symmetry of the window, $\vert W(\vec{k})\vert^2=\vert W(-\vec{k})\vert^2$ , as expected when taking a modulus of the Fourier transform of a real 3D scalar function.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8cm,clip]{3939_f10.eps} \end{figure}$	Figure 10: Coupling kernels $K_i(k)\equiv K(k_i,k)$ for the power spectrum bins k_i shown in Fig. 5. Numerically evaluated kernels are shown with solid lines. The dashed lines correspond to the fitting functions given in Appendix D.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7cm,clip]{3939_f11.eps} \end{figure}$	Figure 11: $1\sigma$ error contours for the free model parameters. Best fit parameter values are marked with crosses.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3939_f13.eps} \end{figure}$	Figure 13: Left panel: two-point correlation functions as determined in this paper (circles with solid lines) and by Eisenstein et al. (2005). Right panel: correlation functions corresponding to the models shown in the lower panel of Fig. 12 in comparison to the one obtained directly from the data. Here all the data points have been lowered by 0.0035.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3939_f14.eps} \end{figure}$	Figure 14: The comparison of spectra from different surveys.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3939_f15.eps} \end{figure}$	Figure 15: The same as Fig. 14 with the errorbars omitted.
Open with DEXTER