Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3998f1.eps} . \end{figure}$ Figure 1: Comparison of cz distributions of group and field galaxies (solid and dashed lines, respectively). The error bars are 1 $\sigma$ Poissonian errors. The dotted line indicates the simulated field (S-FIELD, see text).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3998f2.eps} \end{figure}$ Figure 2: Comparison between magnitude distribution of all NOG galaxies with that of matched 2MASS-NOG galaxies (solid and dashed lines, respectively). The error bars are 1 $\sigma$ Poissonian errors.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3998f3.eps} \end{figure}$ Figure 3: Comparison between absolute magnitude distributions of group and field galaxies in B and K bands (left and right panels, respectively) for GROUP and S-FIELD samples (solid and dashed lines, respectively). The error bars in the top-panels are 1 $~\sigma$ Poissonian errors. The corresponding cumulative distributions are shown in the bottom panels: there, the dotted lines indicate the distributions for the simulated field ST-S-FIELD, which mimics morphological-type distribution of group galaxies (see text).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3998f4.eps} \end{figure}$ Figure 4: Comparison between absolute magnitude distributions of group and field galaxies in B and K bands (left and right panels, respectively) for VLGROUP and VLFIELD samples (solid and dashed lines, respectively). The error bars in the top-panels are 1 $\sigma$ Poissonian errors. The respective cumulative distributions are shown in the bottom panels: there, the dotted lines indicate the distributions for the simulated field ST-VLFIELD, which mimics morphological-type distribution of group galaxies (see text).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3998f5.eps} \end{figure}$ Figure 5: Comparison between morphological-type distribution of GROUP and FIELD galaxies (solid and dashed lines, respectively). The error bars are 1 $\sigma$ Poissonian errors.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3998f6.eps} \end{figure}$ Figure 6: Top panels: B-band absolute-magnitude as a function of morphological type for GROUP and S-FIELD (left panels) and VLGROUP and VLFIELD (right panels). Points are biweight mean values for galaxies in groups (filled circles) and field (open circles). Error bars are $68\%$ bootstrap estimates. Only bins containing more than three galaxies both for group and field samples are plotted. Solid, dashed, and dotted lines indicate the median values of magnitude distributions of group, field, and simulated field galaxies, respectively; see also left-lower panels of Figs. 3 and 4. Bottom panels show the magnitude difference between group and field as recovered from the top panels.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3998f7.eps} \end{figure}$ Figure 7: Top panels: K-band absolute-magnitude as a function of morphological type for GROUP and S-FIELD (left panels) and VLGROUP and VLFIELD (right panels). Points are biweight mean values for galaxies in groups (filled circles) and field (open circles). Error bars are 68% bootstrap estimates. Only bins containing more than three galaxies both for group and field samples are plotted. Solid, dashed, and dotted lines indicate the median values of magnitude distributions of group, field, and simulated field galaxies, respectively; see also right-lower panels of Figs. 3 and 4. Bottom panels show the magnitude difference between group and field as recovered from the top panels.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3998f8.eps} \end{figure}$ Figure 8: Absolute magnitude as function of cz for B and K bands (top and bottom panels, respectively). Points are biweight mean values for galaxies in GROUP sample (filled circles) and S-FIELD sample (open circles). Error bars are 68% bootstrap estimates. The results for the real (not simulated) field are also shown (stars). Solid and dashed lines show the trend for the two alternative cz estimates, recovered by using two different corrections for the peculiar velocity field (corrections 1 and 2, respectively, see text) for group and field galaxies (thick and thin lines, respectively).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3998f9.eps} \end{figure}$ Figure 9: Comparison between B-K distributions of group and field galaxies (solid and dashed lines, respectively) for GROUP and S-FIELD (left panels) and VLGROUP and VLFIELD (right panels). The error bars in the top-panels are 1 $\sigma$ Poissonian errors. The corresponding cumulative distributions are shown in the bottom panels: there, the dotted lines indicate distributions of the simulated fields, ST-S-FIELD and ST-VLFIELD, which mimic morphological-type distribution of group galaxies (see text).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3998f10.eps} \end{figure}$ Figure 10: Top panels: B-K color as a function of morphological type for GROUP and S-FIELD (left panels) and VLGROUP and VLFIELD (right panels). Points are biweight mean values for galaxies in groups (filled circles) and field (open circles). Error bars are $68\%$ bootstrap estimates. Only bins containing more than three galaxies both for group and field samples are plotted. Bottom panels show the color difference between group and field as recovered from the top panels.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3998f1.eps} . \end{figure}$	Figure 1: Comparison of cz distributions of group and field galaxies (solid and dashed lines, respectively). The error bars are 1 $\sigma$ Poissonian errors. The dotted line indicates the simulated field (S-FIELD, see text).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3998f2.eps} \end{figure}$	Figure 2: Comparison between magnitude distribution of all NOG galaxies with that of matched 2MASS-NOG galaxies (solid and dashed lines, respectively). The error bars are 1 $\sigma$ Poissonian errors.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3998f5.eps} \end{figure}$	Figure 5: Comparison between morphological-type distribution of GROUP and FIELD galaxies (solid and dashed lines, respectively). The error bars are 1 $\sigma$ Poissonian errors.
Open with DEXTER