Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{2280fig1.eps}\end{figure}$ Figure 1: Histogram of the morphological types of the full CIG sample obtained from NED ( bottom) and LEDA ( top).
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{2280fig2.eps}\end{figure}$ Figure 2: Aitoff projection in right ascension and declination coordinates showing the distribution on the sky of CIG galaxies in the following velocity ranges. Galaxies in the 0-3000 km s^-1 velocity interval are shown in a), 3000-6000 km s^-1 in b), 6000-9000 km s^-1 in c) and 9000-12 000 km s^-1 in d). The core of the Virgo cluster is indicated by a circle with $D= 12^\circ$ . Other Abell clusters in the same redshift range and with richness classes 1 or 2 are indicated by filled circles corresponding to their core radius.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2280fig3.eps}\end{figure}$ Figure 3: Histogram of the optical heliocentric velocities of the 956 CIG galaxies with redshift data. Only CIG 402 is out of the plot, with V = 40 658 km s^-1. The solid line corresponds to a homogeneous redshift distribution of the same sample size, velocity distribution and Schechter function. The dashed line has been obtained by scaling down the previous distribution by a factor of 0.6.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2280fig4.eps}\end{figure}$ Figure 4: a) Zwicky-corrected magnitudes versus $B_{\rm T}^0$ from RC3 for the 507 CIG galaxies in common. The solid line is a fit to the plotted data and the parameters of the fit are given in the text (Sect. 4.2). b) Residuals from the previous fit in magnitudes versus $B_{\rm T}^0$ .
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8cm,clip]{2280fig5.eps}\end{figure}$ Figure 5: Distribution of the corrected apparent magnitudes (n = 1050).
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8cm,clip]{2280fig6.eps}\end{figure}$ Figure 6: The $\langle V/V_{\rm m} \rangle$ test for the CIG sample excluding galaxies brighter than 11 mag. The open squares indicate the whole sample (n = 1031), and the filled square the subsample for which recession velocities are available (n = 937) and which are used in the following to construct the OLF. The error bars are given for the latter subsamples and are the statistical errors in the mean $\langle V/V_{\rm m} \rangle$ .
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{2280fig7.eps}\end{figure}$ Figure 7: The $\langle V/V_{\rm m} \rangle$ test for our CIG sample with available distances (n=956) and for XS91 (n=450) sample are shown respectively with filled and open squares. Our sample has been shifted by 0.5 mag toward fainter values in order to match the uncorrected optical magnitudes used by XS91.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2280fig8.eps}\end{figure}$ Figure 8: Optical luminosity function for CIG galaxies for which velocity information exists and with apparent magnitudes between 11 and 15 (n = 725). The Schechter fit to this sample is plotted as a solid line. The dashed line corresponds to a fit to the same sample when galaxies with $V_{\rm r}$ < 1500 km s^-1 are removed.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{2280fig9.eps}\end{figure}$ Figure 9: All three OLF estimations for the CIG involving n=725 galaxies (our sample, filled triangles), 450 galaxies (CIG sample of XS91, open circles) and 294 galaxies (AIG sample of XS91, crosses). The CIG data are given in corrected magnitudes while the data of XS91 refer to uncorrected magnitudes.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{2280fig10.eps}\end{figure}$ Figure 10: The same as in Fig. 9 but calculated using uncorrected magnitudes for the CIG galaxies, as was done for the other two samples by XS91.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2280fig11.eps}\end{figure}$ Figure 11: The Schechter function M^* parameter as a function of the environment, ordered in an approximate way. The label "all'' indicates that the M^* value has been obtained for all galaxies in the sample independently of the environment.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{2280fig12.eps}\end{figure}$ Figure 12: The same as in Fig. 11 for the $\alpha$ parameter.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{2280fig1.eps}\end{figure}$	Figure 1: Histogram of the morphological types of the full CIG sample obtained from NED ( bottom) and LEDA ( top).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2280fig3.eps}\end{figure}$	Figure 3: Histogram of the optical heliocentric velocities of the 956 CIG galaxies with redshift data. Only CIG 402 is out of the plot, with V = 40 658 km s^-1. The solid line corresponds to a homogeneous redshift distribution of the same sample size, velocity distribution and Schechter function. The dashed line has been obtained by scaling down the previous distribution by a factor of 0.6.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2280fig4.eps}\end{figure}$	Figure 4: a) Zwicky-corrected magnitudes versus $B_{\rm T}^0$ from RC3 for the 507 CIG galaxies in common. The solid line is a fit to the plotted data and the parameters of the fit are given in the text (Sect. 4.2). b) Residuals from the previous fit in magnitudes versus $B_{\rm T}^0$ .
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$\begin{figure} \par\includegraphics[angle=270,width=8cm,clip]{2280fig5.eps}\end{figure}$	Figure 5: Distribution of the corrected apparent magnitudes (n = 1050).
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$\begin{figure} \par\includegraphics[width=8cm,clip]{2280fig7.eps}\end{figure}$	Figure 7: The $\langle V/V_{\rm m} \rangle$ test for our CIG sample with available distances (n=956) and for XS91 (n=450) sample are shown respectively with filled and open squares. Our sample has been shifted by 0.5 mag toward fainter values in order to match the uncorrected optical magnitudes used by XS91.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2280fig8.eps}\end{figure}$	Figure 8: Optical luminosity function for CIG galaxies for which velocity information exists and with apparent magnitudes between 11 and 15 (n = 725). The Schechter fit to this sample is plotted as a solid line. The dashed line corresponds to a fit to the same sample when galaxies with $V_{\rm r}$ < 1500 km s^-1 are removed.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{2280fig9.eps}\end{figure}$	Figure 9: All three OLF estimations for the CIG involving n=725 galaxies (our sample, filled triangles), 450 galaxies (CIG sample of XS91, open circles) and 294 galaxies (AIG sample of XS91, crosses). The CIG data are given in corrected magnitudes while the data of XS91 refer to uncorrected magnitudes.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{2280fig10.eps}\end{figure}$	Figure 10: The same as in Fig. 9 but calculated using uncorrected magnitudes for the CIG galaxies, as was done for the other two samples by XS91.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2280fig11.eps}\end{figure}$	Figure 11: The Schechter function M^* parameter as a function of the environment, ordered in an approximate way. The label "all'' indicates that the M^* value has been obtained for all galaxies in the sample independently of the environment.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{2280fig12.eps}\end{figure}$	Figure 12: The same as in Fig. 11 for the $\alpha$ parameter.
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