Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{MS3483fig01.ps}\end{figure}$ Figure 1: Fractional and cumulative completeness for the ESO-Sculptor spectroscopic catalog, as a function of apparent magnitude, in the Johnson B, V and Cousins $R_{\rm c}$ bands.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{MS3483fig02.ps}\end{figure}$ Figure 2: a) Top panel: spectral classification parameters $\delta$ and $\theta$ for the 603 ESO-Sculptor spectra with $R_{\rm c}\le 20.5$ and a PCA defined spectral class $\delta _1-\theta _1$ (see Sect. 2.2 for details). Spectra are getting bluer toward larger values of $\delta$ . Galaxies with EW[OII] < 30 Å are shown as black open circles, those with EW[OII] $\ge$ 30 Å as magenta filled circles. The vertical lines at $\delta =-5$ and $\delta =3$ indicate the limits between the 3 spectral classes used for the calculation of the luminosity functions (see Sect. 2.5). b) Bottom panel: $\delta$ and $\theta$ parameters obtained by projection of 26 Kennicutt spectra Kennicutt (1992) onto the ESS PCs used in a). To correct for the systematic color shift in the ESS spectra, a constant offset of $-2.5^\circ$ is applied to the $\delta$ values for the Kennicutt spectra (see Sect. 2.4). The morphological types for the Kennicutt galaxies provides indications on the type content of the ESS spectral classes.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{MS3483fig03.ps}\end{figure}$ Figure 3: Spectral classification parameter $\delta$ as a function of redshift for the ESO-Sculptor galaxies with $R_{\rm c}\le 20.5$ sample. Galaxies with EW[OII] < 10 Å are shown as black open circles, those with EW[OII] $\ge$ 10 Å as magenta filled circles. The vertical lines at $\delta =-5^\circ$ and $\delta =3^\circ$ indicate the limits between the 3 spectral classes used for the calculation of the luminosity functions (see Sect. 2.5).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{MS3483fig04.ps}\end{figure}$ Figure 4: K-corrections obtained from the PEGASE templates (Fioc & Rocca-Volmerange 1997, red filled circles with error-bars) in the $R_{\rm c}$ and B band, compared with the K-corrections from Coleman et al. (1980, blue solid lines), Kinney et al. (1996, black dotted lines), Pence (1976, green short-dashed lines), and Poggianti (1997, magenta long-dashed line); for the B K-corrections by Kinney et al. (1996), the K-corrections for type SB4 are used in panel "Irr''.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{MS3483fig05.ps}\end{figure}$ Figure 5: The mean absolute and apparent colors for galaxies with $R_{\rm c}\le 20.5$ in each of the 3 ESO-Sculptor spectral classes used for calculation of the LFs, and in the 4 redshifts intervals bounded by 0.1, 0.2, 0.3, 0.4, and 0.5; red solid, green dotted, blue dashed lines connect the points for the early, intermediate, and late-type classes respectively. The left panels show the apparent colors and the right panels the absolute colors. The upper panels show the $B-R_{\rm c}$ colors, and the lower panels, the $V-R_{\rm c}$ colors. The error bars indicate the rms dispersion measured in the corresponding redshift interval. For clarity, the points for early and late-type galaxies are offset along the redshift axis by -0.007 and 0.007, respectively.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{MS3483fig06.ps}\end{figure}$ Figure 6: Spectral classification parameter $\delta$ as a function of absolute magnitude $M(R_{\rm c})$ for the ESO-Sculptor galaxies with $R_{\rm c}\le 20.5$ . Galaxies with EW[OII] < 10 Å are shown as black open circles, those with EW[OII] $\ge$ 10 Å as magenta filled circles. The vertical lines at $\delta =-5^\circ$ and $\delta =3^\circ$ indicate the limits between the 3 spectral classes used for the calculation of the luminosity functions (see Sect. 2.5).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=16.3cm,clip]{MS3483fig07.ps}\end{figure}$ Figure 7: The ESO-Sculptor luminosity functions for the early-type, intermediate-type, and late-type galaxies at the nominal limits in the 3 filters: $R_{\rm c}\le 20.5$ , $V\le 21.0$ and $B\le 22.0$ . Symbols indicate the SWML solution, and lines the STY solution: early-type are shown as red filled circles and red solid lines; intermediate-type as green open circles and green dotted lines; late-type as blue open triangles and blue dashed lines. The flatter curve for the late-type galaxies in the $R_{\rm c}\le 20.5$ sample has $\alpha =-1.3$ (see text for details). The Schechter parameters of the STY solutions are listed in Tables 2 and 3. The amplitudes of the SWML points are adjusted by least-square fits to the STY solutions. The histograms show for each filter the number of galaxies used in the calculation of the corresponding LFs as a function of absolute magnitude (with the same line coding as for the STY solutions).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{MS3483fig08.ps}\end{figure}$ Figure 8: The best-fit parameters (filled circles) and the 1- $\sigma$ error ellipses for M^* and $\alpha$ as derived from the STY fit of the LFs to $R_{\rm c}\le 20.5$ for the 3 galaxy classes in the ESO-Sculptor Survey: early-type (red solid line); intermediate-type (green dotted line); late-type (blue dashed line).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{MS3483fig09.ps}\end{figure}$ Figure 9: Absolute $R_{\rm c}$ magnitudes as a function of redshift z for the ESO-Sculptor Survey galaxies with $R_{\rm c}\le 20.5$ . This graph shows how the limit in apparent 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.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{MS3483fig10.ps}\end{figure}$ Figure 10: Comparison of the Schechter parameters M^* and $\alpha$ for theESO-Sculptor Survey in the $R_{\rm c}$ , V, and B bands with those from theCNOC2 (Lin et al. 1999). Galaxies of later spectral type are in the direction of steeper slopes $\alpha$ .
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=17.6cm,clip]{MS3483fig11.ps}\end{figure}$ Figure 11: Comparison of the ESO-Sculptor spectral-type luminosity functions for $R_{\rm c}\le 20.5$ (top panels) and $R_{\rm c}\le 21.5$ (bottom panels) with the composite LFs modeling the intrinsic LFs (see Sandage et al. 1985 and Jerjen & Tammann 1997). Left, center, and right panels show the LFs for the early-type, intermediate-type, and late-type galaxies respectively. Dotted and dot-dashed lines show the adjusted Spiral LFs, and dashed lines show the adjusted dwarf galaxy LFs; solid lines show the composite LFs resulting from the sum of the individual components, excluding the Sd/Sm component, only shown as indicative (see text for details). The respective LF parameters are listed in Table 7 (those for which the "Type of LF'' is written in boldface).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{MS3483fig12.ps}\end{figure}$ Figure 12: Other composite fits of the ESO-Sculptor late-type luminosity functions for the $R_{\rm c}\le 20.5$ and $R_{\rm c}\le 21.5$ samples. Dotted and dot-dashed lines show the Spiral LFs, dashed lines show the dwarf galaxy LFs (dI). Solid lines show the composite LFs resulting from the sum of the individual components, except for the Sd/Sm component only shown as indicative (see text for details). Here, the Schechter slope $\alpha$ of the dI component is fixed to -0.3, as measured from the Virgo cluster (see Tables 6 and 7). The other LF parameters are listed in Table 7.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{MS3483fig13.ps}\end{figure}$ Figure 13: Comparison of the ESO-Sculptor rest-frame peak surface brightness at $R_{\rm c}\le 20.5$ (3 left panels) and $R_{\rm c}\le 21.5$ (3 right panels), for the early-type (red solid line), intermediate-type (green dotted line), and late-type (blue dashed line) galaxies, using redshift increments $\Delta z=0.04$ . The 3 spectral classes are separated according to the physical radius $r_{{\rm peak}}$ of the peak pixel over which is calculated the surface brightness: top, middle, and bottom panels correspond to $r_{{\rm peak}}\le 0.6$ h^-1 kpc, $0.6< r_{{\rm peak}}\le 0.8$ h^-1 kpc, and $r_{{\rm peak}}> 0.8$ h^-1 kpc respectively.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{MS3483fig01.ps}\end{figure}$	Figure 1: Fractional and cumulative completeness for the ESO-Sculptor spectroscopic catalog, as a function of apparent magnitude, in the Johnson B, V and Cousins $R_{\rm c}$ bands.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{MS3483fig08.ps}\end{figure}$	Figure 8: The best-fit parameters (filled circles) and the 1- $\sigma$ error ellipses for M^* and $\alpha$ as derived from the STY fit of the LFs to $R_{\rm c}\le 20.5$ for the 3 galaxy classes in the ESO-Sculptor Survey: early-type (red solid line); intermediate-type (green dotted line); late-type (blue dashed line).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{MS3483fig09.ps}\end{figure}$	Figure 9: Absolute $R_{\rm c}$ magnitudes as a function of redshift z for the ESO-Sculptor Survey galaxies with $R_{\rm c}\le 20.5$ . This graph shows how the limit in apparent 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.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{MS3483fig10.ps}\end{figure}$	Figure 10: Comparison of the Schechter parameters M^* and $\alpha$ for theESO-Sculptor Survey in the $R_{\rm c}$ , V, and B bands with those from theCNOC2 (Lin et al. 1999). Galaxies of later spectral type are in the direction of steeper slopes $\alpha$ .
Open with DEXTER