All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{3879fig1.eps} \end{figure}$ Figure 1: Sensitivity of the $\theta_\circ \longleftrightarrow z_{\rm c}$ relation to $\Omega _{m\circ }$ and $\Omega _{\Lambda \circ }$ .
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{3879fig2.eps} \end{figure}$ Figure 2: Histogram of the distribution of projected separations for the 3239 pairs in the 2dFGRS selected by: i) redshifts from emission lines and greater than 0.001, ii) angular separation less than 10 $^\prime$ . The concordance model is assumed.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{3879fig3.eps}\end{figure}$ Figure 3: Selection of the sub-sample of interactivated galaxies candidates in the 2dFGRS. The zone of the 45 retained pairs with $PS < 300 \ (0.7/h_\circ )$ kpc is hashed. The white case in the first bin is for the rejected pair in the arms of NGC 4517. The solid line displays the Poissonian distribution used for simulations.
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In the text

$\begin{figure} \par\includegraphics[width=4cm,height=8cm,angle=-90,clip]{3879fig4.eps} \end{figure}$ Figure 4: Redshifts of QSOs in the 2QZ survey. We selected the 22 122 objects with only the label "QSO''. This distribution of redshifts has been applied to the synthetic samples of interactivating galaxies.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3879fig5.eps} \end{figure}$ Figure 5: Normalized probability densities of retrieved cosmological parameters with 1000 pairs of interactivated galaxies. The 68% and 95% confidence levels appear in shaded and darker shaded areas for the four sets of ( $\Omega _{m\circ }$ , $\Omega _{\Lambda \circ }$ ): (1.0, 0.0), (0.3, 0.0), (0.3, 0.7), and (0.1, 0.9).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.4cm,clip]{3879fig6.eps} \end{figure}$ Figure 6: Internal precision ( $\sigma$ ) on $\Omega _{m\circ }$ and $\Omega _{\Lambda \circ }$ versus number of pairs and for the "concordance'' model, also shown with $\Omega _{f\circ }$ the precision with the flat space external condition $\Omega _{m\circ } + \Omega _{\Lambda \circ } =1$ .
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{3879fig1.eps} \end{figure}$	Figure 1: Sensitivity of the $\theta_\circ \longleftrightarrow z_{\rm c}$ relation to $\Omega _{m\circ }$ and $\Omega _{\Lambda \circ }$ .
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{3879fig2.eps} \end{figure}$	Figure 2: Histogram of the distribution of projected separations for the 3239 pairs in the 2dFGRS selected by: i) redshifts from emission lines and greater than 0.001, ii) angular separation less than 10 $^\prime$ . The concordance model is assumed.
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{3879fig3.eps}\end{figure}$	Figure 3: Selection of the sub-sample of interactivated galaxies candidates in the 2dFGRS. The zone of the 45 retained pairs with $PS < 300 \ (0.7/h_\circ )$ kpc is hashed. The white case in the first bin is for the rejected pair in the arms of NGC 4517. The solid line displays the Poissonian distribution used for simulations.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=4cm,height=8cm,angle=-90,clip]{3879fig4.eps} \end{figure}$	Figure 4: Redshifts of QSOs in the 2QZ survey. We selected the 22 122 objects with only the label "QSO''. This distribution of redshifts has been applied to the synthetic samples of interactivating galaxies.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3879fig5.eps} \end{figure}$	Figure 5: Normalized probability densities of retrieved cosmological parameters with 1000 pairs of interactivated galaxies. The 68% and 95% confidence levels appear in shaded and darker shaded areas for the four sets of ( $\Omega _{m\circ }$ , $\Omega _{\Lambda \circ }$ ): (1.0, 0.0), (0.3, 0.0), (0.3, 0.7), and (0.1, 0.9).
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$\begin{figure} \par\includegraphics[angle=-90,width=8.4cm,clip]{3879fig6.eps} \end{figure}$	Figure 6: Internal precision ( $\sigma$ ) on $\Omega _{m\circ }$ and $\Omega _{\Lambda \circ }$ versus number of pairs and for the "concordance'' model, also shown with $\Omega _{f\circ }$ the precision with the flat space external condition $\Omega _{m\circ } + \Omega _{\Lambda \circ } =1$ .
Open with DEXTER