All Figures

$\begin{figure} \par\includegraphics[width=16.3cm,clip]{0140fg01.ps} \end{figure}$ Figure 1: The ESO-Sculptor Gaussian+Schechter composite luminosity functions for the early-type ( top panels), intermediate-type ( middle panels), and late-type galaxies ( bottom panels) in the 3 samples: $R_{\rm c}\le 21.5$ ( left panels), $V\le 21.0$ ( central panels) and $B\le 22.0$ ( right panels). Symbols indicate the SWML solution, and lines the composite fits; all were obtained with H₀ = 100 h km s^-1 Mpc^-1, $\Omega _{\rm m}=1.0$ , and $\Omega _\Lambda =0.0$ . The shape parameters of the composite functions converted to $\Omega _{\rm m}=0.3$ and $\Omega _\Lambda =0.7$ are listed in Table 1.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{0140fg02.ps} \end{figure}$ Figure 2: Absolute $R_{\rm c}$ magnitudes as a function of redshift z for the ESS galaxies with $R_{\rm c}\le 21.5$ , using H₀ = 100 h km s^-1 Mpc^-1, $\Omega _{\rm m}=0.3$ , and $\Omega _\Lambda =0.7$ . This graph shows how the apparent limiting magnitude biases the range of absolute magnitudes detected at increasing redshift, and how the varying K-corrections per spectral type affect the faintest absolute magnitude reached at a given redshift.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{0140fg03.ps} \end{figure}$ Figure 3: Same as Fig. 2 for $V\le 21.0$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{0140fg04.ps} \end{figure}$ Figure 4: Same as Fig. 2 for $B\le 22.0$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{0140fg05.ps} \end{figure}$ Figure 5: The amplitude $\phi _0$ of the Gaussian component of the composite luminosity functions measured for the ESO-Sculptor $R_{\rm c}\le 21.5$ sample, using the estimators n₁ (red solid line), n₂ (green dotted line), n₃ (blue dashed line), and $n_{\rm EEP}$ (black dot-dashed line) defined in Eqs. (10)-(15), as a function of redshift (denoted $z_{\rm max}$ in the text). Each panel corresponds to a spectral-type. For clarity, only the random errors for the n₁ estimator, calculated using Eq. (16) are shown (see text for details). The error bars for the other curves have similar amplitude, except for n₂, for which they are 50% wider.
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In the text

$\begin{figure} \par\includegraphics[width=8.7cm,clip]{0140fg06.ps} \end{figure}$ Figure 6: The amplitude $\phi _0$ of the Gaussian component of the composite luminosity functions measured for the ESO-Sculptor $R_{\rm c}\le 21.5$ sample, using the estimator n₁ defined in Eq. (10), as a function of redshift $z_{\rm max}$ ; early-type, intermediate-type, late-type galaxies correspond to the red dotted, green dashed, and blue solid lines respectively. For clarity, the random errors for the intermediate-type galaxies are not shown; they are comparable to those for the early-type and late-type galaxies (see Eq. (16)). The linear fit of Eq. (19) is also plotted (magenta solid straight line).
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0140fg07.ps} \end{figure}$ Figure 7: The amplitude $\phi _0(z_{\rm max})$ of the Gaussian component of the composite luminosity functions measured from the ESO-Sculptor $R_{\rm c}\le 21.5$ sample for the intermediate-type (green dashed line) and late-type galaxies (blue solid line), both normalized to $\phi _0(z_{\rm max})$ for the early-type galaxies. All values of $\phi _0$ are derived using the n₁ estimator defined in Eq. (10). The linear fit to the relative late-type density given in Eq. (20) is also shown (magenta solid straight line).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0140fg08.ps} \end{figure}$ Figure 8: The amplitude $\phi _0(z_{\rm max})$ of the Gaussian component of the composite luminosity functions measured from the ESO-Sculptor $V\le 21.0$ sample ( top panel) and the $B\le 22.0$ sample ( bottom panel) for the intermediate-type (green dashed line) and late-type galaxies (blue solid line), both normalized to $\phi _0(z_{\rm max})$ for the early-type galaxies. All values of $\phi _0$ are derived using the n₁ estimator defined in Eq. (10). The linear fits to the relative late-type density and the corresponding parameterization are also shown in each panel (magenta solid straight line).
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{0140fg09.ps} \end{figure}$ Figure 9: K-corrections in the $R_{\rm c}$ band ( top panel), V band ( middle panel), and B band ( bottom panel) derived from Coleman et al. (1980, labeled "CWW extrap'' in graph; see text for details) which are used for predicting the ESO-Sculptor galaxy number counts in Figs. 10-12: Elliptical, Sbc and Magellanic Irregular types are plotted as dashed lines (running from top to bottom), and are used to model the ESO-Sculptor K-corrections for the early-type, intermediate-type, and late-type galaxies respectively; K-corrections for "CWW extrap'' type Scd are shown as dotted lines, for comparison. The polynomial K-corrections calculated for the 3 ESO-Sculptor spectral classes and valid only for z<0.6 are shown as heavy solid lines, with early-type, intermediate-type and late-type galaxies plotted from top to bottom.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0140fg10.ps} \end{figure}$ Figure 10: Comparison of the ESO-Sculptor magnitude number-counts in the $R_{\rm c}$ band per 0.25 $^{\rm mag}$ interval (open and filled circles) with the modeled counts defined as the sum of the predicted number counts for the 3 considered spectral classes: early-type (red dotted line), intermediate-type (green dashed line), late-type with no-evolution (blue dot-dashed line), late-type with the best-fit evolution rate (blue solid line). The Gaussian+Schechter composite luminosity functions listed in Table 1 are used for the 3 classes. The amplitude $\phi _0$ of the Gaussian component of the luminosity function used for each galaxy class is identical to that used in Fig. 13. The black heavy dot-dashed line show the predicted total counts with no-evolution, and the black heavy solid line the adjusted total counts with evolution in the late-type galaxies (see text for details). Only the data points with more than 100 galaxies per bin (filled circles) are used for the adjustment of the total evolving counts. The plotted error bars in the observed counts are estimated as $\sqrt {n}$ . The inset shows the predicted redshift distributions for the 3 spectral classes, with the same line coding as for the number-counts.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0140fg11.ps} \end{figure}$ Figure 11: Same as Fig. 10 for the ESS number-counts per 0.25 mag interval in the V band. The amplitude $\phi _0$ of the Gaussian component of the luminosity function used for each galaxy class is identical to that used in Fig. 14.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0140fg12.ps} \end{figure}$ Figure 12: Same as Fig. 10 for the ESS number-counts per 0.25 mag interval in the B band. The amplitude $\phi _0$ of the Gaussian component of the luminosity function used for each galaxy class is identical to that used in Fig. 15.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{0140fg13.ps} \end{figure}$ Figure 13: The observed redshift distribution for the early-type (top graph), intermediate-type (middle graph), and late-type galaxies (bottom graph) in the ESS $R_{\rm c}\le 21.5$ sample. In order to allow for the noise in the observed histograms, these are plotted for 2 binnings of $\Delta z=0.08$ , offset by 0.04 in redshift (first bin starting at z=0, z=0.04 for the dotted, resp. solid histogram). The expected distribution for a uniform galaxy distribution with the ESS incompleteness and the composite luminosity function listed in Table 1 is over-plotted as a solid line for the 3 spectral classes. For the late-type galaxies, we also plot as a dashed line the expected distribution with an evolution factor P_0.15=2.2, as derived from the $R_{\rm c}$ number counts (see Sect. 6). All expected curves are normalized so that they match the observed number of galaxies in the interval $0.01\le z\le 0.81$ ; the resulting amplitudes $\phi _0$ and $\phi ^*$ for the Gaussian and Schechter components are indicated inside each panel.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0140fg14.ps} \end{figure}$ Figure 14: Same as Fig. 13 for the ESS $V\le 21.0$ sample, with P_0.15=4.3 as derived from the V number counts (see Sect. 6).
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0140fg15.ps} \end{figure}$ Figure 15: Same as Fig. 13 for the ESS $B\le 22.0$ sample, with P_0.15=3.3 as derived from the B number counts (see Sect. 6).
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In the text

$\begin{figure} \par\includegraphics[width=8.7cm,clip]{0140fg16.ps} \end{figure}$ Figure 16: The observed redshift distribution for the bright and faint galaxies in the ESO-Sculptor late-type class ( $M(R_{\rm c})\le-19.0+5\log h$ in top panel, $M(R_{\rm c})\ge-19.0+5\log h$ in bottom panel). In order to allow for the noise in the observed histograms, they are plotted for 2 binnings of $\Delta z=0.08$ , offset by 0.04 in redshift (first bin starting at z=0, z=0.04 for the dotted, resp. solid histogram). The expected distribution for a uniform galaxy distribution with the ESS incompleteness and the composite late-type LF listed in Table 1 and truncated at $M(R_{\rm c})=-19.0+5\log h$ is plotted as a solid line in both panels. The expected distribution with an evolution factor P_0.15=3.0 is plotted as a dashed line in both panels; the expected curve with P_0.15=6.0 is also shown as a dash-dotted line in the top panel. The expected curves are normalized so that they match the observed number of galaxies in the interval $0.01\le z\le 0.81$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{0140fg03.ps} \end{figure}$	Figure 3: Same as Fig. 2 for $V\le 21.0$ .
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{0140fg04.ps} \end{figure}$	Figure 4: Same as Fig. 2 for $B\le 22.0$ .
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0140fg11.ps} \end{figure}$	Figure 11: Same as Fig. 10 for the ESS number-counts per 0.25 mag interval in the V band. The amplitude $\phi _0$ of the Gaussian component of the luminosity function used for each galaxy class is identical to that used in Fig. 14.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0140fg12.ps} \end{figure}$	Figure 12: Same as Fig. 10 for the ESS number-counts per 0.25 mag interval in the B band. The amplitude $\phi _0$ of the Gaussian component of the luminosity function used for each galaxy class is identical to that used in Fig. 15.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0140fg14.ps} \end{figure}$	Figure 14: Same as Fig. 13 for the ESS $V\le 21.0$ sample, with P_0.15=4.3 as derived from the V number counts (see Sect. 6).
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0140fg15.ps} \end{figure}$	Figure 15: Same as Fig. 13 for the ESS $B\le 22.0$ sample, with P_0.15=3.3 as derived from the B number counts (see Sect. 6).
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