Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0909f01.eps} \end{figure}$ Figure 1: $I_{814}-K_{\rm s}$ versus $K_{\rm s}$ color-magnitude relation for $K_{\rm s}$ -selected objects of the HDF-S as given by Labbé et al. (2003). Following Labbé et al. (2003) only sources with a minimum of 20% of the total exposure time in all bands are included and shown as filled symbols. Colors are plotted with $1 \sigma$ error bars. The solid line corresponds to the limiting magnitude of the FDF (I=26.8). Only the objects to the right of the solid line are beyond our I-band limit.
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In the text

$\begin{figure} \par\includegraphics[width=12.1cm,clip]{0909f02.eps} \end{figure}$ Figure 2: Comparison of spectroscopic (Böhm et al. 2003; Noll et al. 2004) and photometric redshifts for different galaxy types and quasars in the FDF (362 objects).
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0909f03a.eps}\hspace*{1cm} \includegraphics[width=8.7cm,clip]{0909f03b.eps} \end{figure}$ Figure 3: Left panel: histogram of the reduced $\chi ^2$ for all galaxies in the FDF as obtained for the best fitting template and redshift. The dotted vertical line indicates the median reduced $\chi ^2$ . Right panel: histogram of the photometric redshift errors. The error distribution can be approximated by a Gaussian centered at 0.006 with an rms of 0.028 (dotted line).
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{0909f04a.eps}\hspace*{8mm} \includegraphics[width=8.6cm,clip]{0909f04b.eps}\par \par\end{figure}$ Figure 4: Left panel: absolute B magnitudes of galaxies in the FDF against redshift. Colors indicate spectral types (red to blue: old to young). The two lines indicate the 50% completeness limit for a red and a blue spectral energy distribution corresponding to an I-band limiting magnitude of 26.8. Right panel: redshift number distribution of all galaxies in the FDF sample. The clustering observed in photometric redshift space ( both panels) is probably mostly real, as we see clustered spectroscopic redshifts at z=0.22, z=0.33, z=0.39, z=0.45, z=0.77, z=2.35 and possibly at z=0.95, z=3.15, and z=3.4.
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In the text

$\begin{figure} \par\includegraphics[width=5.6cm,clip]{0909f05a.eps}\hspace*{2mm}... ....eps}\hspace*{2mm} \includegraphics[width=5.6cm,clip]{0909f05i.eps} \end{figure}$ Figure 5: Luminosity functions at 2800 Å from low redshift ( $\langle z\rangle=0.3$ , upper left panel) to high redshift ( $\langle z\rangle=5.5$ , lower right panel). The filled (open) symbols show the luminosity function corrected (uncorrected) for $V/V_{\rm max}$ . The fitted Schechter functions for a fixed slope $\alpha$ are shown as solid lines. Note that we only fit the luminosity functions from $\langle z\rangle=0.6$ to $\langle z\rangle=4.5$ . The parameters of the Schechter functions are given in Table A.2. The Schechter fit for redshift $\langle z\rangle=0.6$ is indicated as a dashed line in all panels.
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In the text

$\begin{figure} \par\includegraphics[width=5.6cm,clip]{0909f06a.eps}\hspace*{2mm}... ....eps}\hspace*{2mm} \includegraphics[width=5.6cm,clip]{0909f06i.eps} \end{figure}$ Figure 6: Luminosity functions in the g'-band from low redshift ( $\langle z\rangle=0.3$ , upper left panel) to high redshift ( $\langle z\rangle=5.5$ , lower right panel). The filled (open) symbols show the luminosity function corrected (uncorrected) for $V/V_{\rm max}$ . The fitted Schechter functions for a fixed slope $\alpha$ are shown as solid lines. Note that we only fit the luminosity functions from $\langle z\rangle=0.6$ to $\langle z\rangle=4.5$ . The parameters of the Schechter functions can be found in Table A.4. The dotted line represents the local g'-band luminosity function derived from the SDSS (Blanton et al. 2001). The Schechter fit for redshift $\langle z\rangle=0.6$ is indicated as a dashed line in all panels.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0909f07a.eps}\hspace*{4mm} \... ...7c.eps}\hspace*{4mm} \includegraphics[width=8cm,clip]{0909f07d.eps} \end{figure}$ Figure 7: $1 \sigma$ and $2\sigma$ confidence levels in Schechter parameter space for the different redshift bins, labeled by their mean redshift. A Schechter function with a fixed slope (see Table 3) has been fitted to the luminosity function at 1500 Å (upper left panel), 2800 Å (upper right panel), in the u'-band (lower left panel) and in the g'-band (lower right panel). The parameters of the Schechter function can be found in Tables A.1-A.4.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{0909f08.eps} \end{figure}$ Figure 8: $1 \sigma$ and $2\sigma$ confidence levels of the parameters a and b in different bands (1500 Å, 2800 Å, u', g' and B) for the evolutionary model described in the text. The values for a and b can be found in Table 4.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0909f09a.eps}\hspace*{4mm} \includegraphics[width=8.5cm,clip]{0909f09b.eps} \end{figure}$ Figure 9: Redshift evolution of $M^\ast$ ( left panel) and $\phi ^\ast$ ( right panel) for the filters g' (filled squares), u' (open triangles) and the two UV bands at 2800 Å and 1500 Å (filled circles). The arrows mark the values for $M^\ast$ and $\phi ^\ast$ as derived in the SDSS (Blanton et al. 2001).
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In the text

$\begin{figure} \par\includegraphics[width=5.7cm,clip]{0909f10a.eps}\hspace*{2mm}... ....eps}\hspace*{2mm} \includegraphics[width=5.7cm,clip]{0909f10c.eps} \end{figure}$ Figure 10: Comparison of the luminosity function at 1700 Å of the FDF with the Schechter function derived in Steidel et al. (1999): $\langle z \rangle\sim 3.04$ ( left panel) and $\langle z \rangle\sim 4.13$ ( middle panel). The filled (open) symbols show the luminosity function corrected (uncorrected) for $V/V_{\rm max}$ . The shaded region in all plots is based only on $\Delta$ $M^\ast$ , and $\Delta \alpha$ (a detailed discussion concerning the errors $\Delta$ $M^\ast$ , and $\Delta \alpha$ can be found in Sect. 7), where the cut-off at low luminosity indicates the limiting magnitude of the sample. In the right panel the $1 \sigma$ and $2\sigma$ confidence levels for $M^\ast$ and $\alpha$ for a 3 parameter Schechter fit as derived in the FDF in the redshift interval $2.54 <z\le 3.54$ (solid contours) and $3.70 <z\le 4.56$ (dotted contours) are shown. The horizontal dashed line marks the slope $\alpha =-1.6$ as derived in Steidel et al. (1999).
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In the text

$\begin{figure} \par\includegraphics[width=5.8cm,clip]{0909f11a.eps}\hspace*{2mm}... ....eps}\hspace*{2mm} \includegraphics[width=5.6cm,clip]{0909f11c.eps} \end{figure}$ Figure 11: Comparison of the luminosity function at 2500 Å of the FDF with the Schechter function derived in Wilson et al. (2002): $0.2 <z\le 0.5$ ( left panel), $0.6 <z\le 1.0$ ( middle panel), and $1.0 <z\le 1.5$ ( right panel). Wilson et al. (2002) fixed the slope to $\alpha =-1.0$ (thick line) and $\alpha =-1.5$ (thin line) and used only $M^\ast$ and $\phi ^\ast$ as free parameters to determine the Schechter functions.
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In the text

$\begin{figure} \par\includegraphics[width=5.6cm,clip]{0909f12a.eps}\hspace*{2mm}... ....eps}\hspace*{2mm} \includegraphics[width=5.6cm,clip]{0909f12f.eps} \end{figure}$ Figure 12: Comparison of the B-band luminosity function of the FDF with predictions based on Kauffmann et al. (1999) (solid line): $\langle z \rangle\sim 0.20$ , $\langle z \rangle\sim 0.62$ , $\langle z \rangle\sim 1.05$ , $\langle z \rangle\sim 1.46$ , $\langle z \rangle\sim 2.12$ , and $\langle z \rangle\sim 2.97$ (from upper left to lower right panel). The filled (open) symbols show the luminosity function corrected (uncorrected) for $V/V_{\rm max}$ . The drops of the theoretical curves towards the faint end is caused by the limited mass resolution of the models, see Kauffmann et al. (1999) for details.
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In the text

$\begin{figure} \par\includegraphics[width=5.8cm,clip]{0909f13a.eps}\hspace*{2mm}... ...phics[width=5.8cm,clip]{0909f13h.eps}\hspace*{2mm} \hspace*{5.8cm}\end{figure}$ Figure 13: Comparison of the B-band luminosity function of the FDF with predictions based on the CDM model of Menci et al. (2002) (private communication; solid line): $\langle z \rangle\sim 0.3$ , $\langle z \rangle\sim 0.6$ , $\langle z \rangle\sim 0.9$ , $\langle z \rangle\sim 1.4$ , $\langle z \rangle\sim 1.9$ , $\langle z \rangle\sim 2.6$ , $\langle z \rangle\sim 3.4$ , and $\langle z \rangle\sim 4.3$ (from upper left to lower right panel). The filled (open) symbols show the luminosity function corrected (uncorrected) for $V/V_{\rm max}$ .
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In the text

$\begin{figure} \par\includegraphics[width=5.33cm,clip]{0909A01a.eps}\hspace*{4mm... ...eps}\hspace*{4mm} \includegraphics[width=5.33cm,clip]{0909A01i.eps} \end{figure}$ Figure A.1: Luminosity functions at 1500 Å from low redshift ( $\langle z\rangle=0.3$ , upper left panel) to high redshift ( $\langle z\rangle=5.5$ , lower right panel). The filled (open) symbols show the luminosity function corrected (uncorrected) for $V/V_{\rm max}$ . The fitted Schechter functions for a fixed slope $\alpha$ are shown as solid lines. Note that we only fit the luminosity functions from $\langle z\rangle=0.6$ to $\langle z\rangle=4.5$ . The parameters of the Schechter functions can be found in Table A.1. The Schechter fit for redshift $\langle z\rangle=0.6$ is indicated as a dashed line in all panels.

In the text

$\begin{figure} \par\includegraphics[width=5.33cm,clip]{0909A02a.eps}\hspace*{4mm... ...eps}\hspace*{4mm} \includegraphics[width=5.33cm,clip]{0909A02i.eps} \end{figure}$ Figure A.2: Luminosity functions in the u'-band from low redshift ( $\langle z\rangle=0.3$ , upper left panel) to high redshift ( $\langle z\rangle=5.5$ , lower right panel). The filled (open) symbols show the luminosity function corrected (uncorrected) for $V/V_{\rm max}$ . The fitted Schechter functions for a fixed slope $\alpha$ are shown as solid lines. Note that we only fit the luminosity functions from $\langle z\rangle=0.6$ to $\langle z\rangle=4.5$ . The parameters of the Schechter functions can be found in Table A.3. The dotted line represents the local u'-band luminosity function derived from the SDSS (Blanton et al. 2001). The Schechter fit for redshift $\langle z\rangle=0.6$ is indicated as a dashed line in all panels.

In the text

$\begin{figure} \par\includegraphics[width=5.5cm,clip]{0909A03a.eps}\hspace*{4mm}... ....eps}\hspace*{4mm} \includegraphics[width=5.5cm,clip]{0909A03i.eps} \end{figure}$ Figure A.3: Luminosity functions in the B-band from low redshift ( $\langle z\rangle=0.3$ , upper left panel) to high redshift ( $\langle z\rangle=5.5$ , lower right panel). The filled (open) symbols show the luminosity function corrected (uncorrected) for $V/V_{\rm max}$ . The fitted Schechter functions for a fixed slope $\alpha$ are shown as solid lines. Note that we only fit the luminosity functions from $\langle z\rangle=0.6$ to $\langle z\rangle=4.5$ . The parameters of the Schechter functions can be found in Table A.5. The Schechter fit for redshift $\langle z\rangle=0.6$ is indicated as a dashed line in all panels.

In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0909B01.eps} \end{figure}$ Figure B.1: Comparison of the luminosity function at 2000 Å of the FDF with the Schechter function derived in Sullivan et al. (2000) ( $z\simeq 0{-}0.4$ ). The shaded region is based on $\Delta$ $M^\ast$ , $\Delta \phi ^\ast$ , and $\Delta \alpha$ , where the cut-off at low luminosity indicates the limiting magnitude of the sample.

In the text

$\begin{figure} \par\mbox{\includegraphics[width=7.6cm,clip]{0909B02a.eps}\hspace... ...\hspace*{2.5cm} \includegraphics[width=7.6cm,clip]{0909B02d.eps} }\end{figure}$ Figure B.2: Comparison of the luminosity function at 2800 Å of the FDF with the Schechter function derived in Wolf et al. (2003): $0.2 <z\le 0.4$ ( upper left panel, light gray), $0.4 <z\le 0.6$ ( upper left panel, dark grey), $0.6 <z\le 0.8$ ( upper right panel), $0.8 <z\le 1.0$ ( lower left panel), $1.0 <z\le 1.2$ ( lower right panel). The shaded regions of all plots are based on $\Delta$ $M^\ast$ , $\Delta \phi ^\ast$ , and $\Delta \alpha$ , where the cut-off at low luminosity indicates the limiting magnitude of the sample.

In the text

$\begin{figure} \par\mbox{\includegraphics[width=7.7cm,clip]{0909B03a.eps}\hspace... ...s}\hspace*{2.5cm} \includegraphics[width=8cm,clip]{0909B03d.eps} }\end{figure}$ Figure B.3: Comparison of the luminosity function at 2000 Å of the FDF with the Schechter function derived in Kashikawa et al. (2003): $0.6 <z\le 1.0$ ( upper left panel), $1.0 <z\le 1.5$ ( upper right panel), $1.5 <z\le 2.5$ ( lower left panel), $2.5 <z\le 3.5$ ( lower right panel). The shaded regions of all plots are based on $\Delta$ $M^\ast$ , $\Delta \phi ^\ast$ , and $\Delta \alpha$ , where the cut-off at low luminosity indicates the limiting magnitude of the sample.

In the text

$\begin{figure} \par\includegraphics[width=11cm,clip]{0909B04.eps} \end{figure}$ Figure B.4: Comparison of the luminosity function at 1700 Å of the FDF with the Schechter function derived in Poli et al. (2001) ( $2.50 <z\le 3.50$ ). The shaded region is based only on $\Delta$ $M^\ast$ , and $\Delta \alpha$ , where the cut-off at low luminosity indicates the limiting magnitude of the sample.

In the text

$\begin{figure} \par\mbox{\includegraphics[width=8cm,clip]{0909B05a.eps}\hspace*{2cm} \includegraphics[width=8cm,clip]{0909B05b.eps} }\end{figure}$ Figure B.5: Left panel: comparison of the luminosity function at 1700 Å of the FDF with the Schechter function derived in Iwata et al. (2003) ( $z\sim 5$ ). The shaded region is based only on $\Delta$ $M^\ast$ , and $\Delta \phi ^\ast$ . Right panel: comparison of the luminosity function at 1700 Å of the FDF with the Schechter functions derived in Ouchi et al. (2003b): $z=4.0 \pm 0.5$ (dark shaded), $z=4.7 \pm 0.5$ (light shaded), and $z=4.9 \pm 0.3$ (not shaded; dashed line). Both shaded regions are based only on $\Delta$ $M^\ast$ , and $\Delta \phi ^\ast$ , where the cut-off at low luminosity indicates the limiting magnitude of the sample.

In the text

$\begin{figure} \par\mbox{\includegraphics[width=8cm,clip]{0909B06a.eps}\hspace*{2.2cm} \includegraphics[width=8cm,clip]{0909B06b.eps} }\end{figure}$ Figure B.6: Left panel: comparison of the u'-band luminosity function of the FDF with the Schechter function derived in Blanton et al. (2001) at $z\sim 0.1$ (light shaded). The dark shaded region shows the Schechter function of Blanton et al. (2001) evolved according to our evolutionary model described in Sect. 6 to redshift $z\sim 0.3$ . The shaded regions are based on $\Delta$ $M^\ast$ , $\Delta \phi ^\ast$ , and $\Delta \alpha$ . Right panel: comparison of the ^0.1u-band luminosity function of the FDF with the Schechter function derived in Blanton et al. (2003) at $z\sim 0.1$ (light shaded). The dark shaded region shows the Schechter function of Blanton et al. (2003) evolved according to our evolutionary model described in Sect. 6 to redshift $z\sim 0.3$ . The shaded regions are based on $\Delta$ $M^\ast$ , $\Delta \phi ^\ast$ , and $\Delta \alpha$ , where the cut-off at low luminosity indicates the limiting magnitude of the sample.

In the text

$\begin{figure} \par\mbox{\includegraphics[width=8cm,clip]{0909B07a.eps}\hspace*{2.2cm} \includegraphics[width=8cm,clip]{0909B07b.eps} }\end{figure}$ Figure B.7: Left panel: comparison of the g'-band luminosity function of the FDF with the Schechter function derived in Blanton et al. (2001) at $z\sim 0.1$ (light shaded). The dark shaded region shows the Schechter function of Blanton et al. (2001) evolved according to our evolutionary model described in Sect. 6 to redshift $z\sim 0.3$ . The shaded regions are based on $\Delta$ $M^\ast$ , $\Delta \phi ^\ast$ , and $\Delta \alpha$ . Right panel: comparison of the ^0.1g-band luminosity function of the FDF with the Schechter function derived in Blanton et al. (2003) at $z\sim 0.1$ (light shaded). The dark shaded region shows the Schechter function of Blanton et al. (2003) evolved according to our evolutionary model described in Sect. 6 to redshift $z\sim 0.3$ . The shaded regions are based on $\Delta$ $M^\ast$ , $\Delta \phi ^\ast$ , and $\Delta \alpha$ , where the cut-off at low luminosity indicates the limiting magnitude of the sample.

In the text

$\begin{figure} \par\mbox{\includegraphics[width=7.7cm,clip]{0909B08a.eps}\hspace... ...\hspace*{2.2cm} \includegraphics[width=7.7cm,clip]{0909B08d.eps} }\end{figure}$ Figure B.8: comparison of the B-band luminosity function of the FDF with the Schechter function derived in Poli et al. (2003): $0.4 <z\le 0.7$ ( upper left panel), $0.7 <z\le 1.0$ ( upper right panel), $1.3 <z\le 2.5$ ( lower left panel), and $2.5 <z\le 3.5$ ( lower right panel). The shaded region is based only on $\Delta$ $M^\ast$ , and $\Delta \alpha$ for $0.4 <z\le 0.7$ , and $0.7 <z\le 1.0$ , whereas for the $1.3 <z\le 2.5$ , and $1.3 <z\le 2.5$ the shaded region is based only on $\Delta$ $M^\ast$ , where the cut-off at low luminosity indicates the limiting magnitude of the sample.

In the text

$\begin{figure}\par\mbox{\includegraphics[width=8.5cm,clip]{0909C01a.eps}\hspace*... ...\hspace*{1.2cm} \includegraphics[width=8.5cm,clip]{0909C01d.eps} }\end{figure}$ Figure C.1: $1 \sigma$ and $2\sigma$ confidence levels in Schechter parameter space. A Schechter function with three free parameters $M^\ast$ , $\phi ^\ast$ , and $\alpha$ has been fitted to the luminosity function at 1500 Å (upper left panel), 2800 Å (upper right panel), u' (lower left panel) and g'-band (lower right panel) and projected to the $M^\ast$ - $\alpha$ plane. The various contours in each panel correspond to the different redshift bins, ranging from $\langle z\rangle=0.6$ (low luminosity) to $\langle z \rangle = 3.5$ (high luminosity). We alternate continuous and dotted lines for clarity. The dashed line marks the fixed slope ( $\alpha (z)={\rm const.}$ ) used to derive the luminosity functions in the different wavebands (see Table 3 lower part).

In the text

$\begin{figure} \par\includegraphics[width=12.1cm,clip]{0909f02.eps} \end{figure}$	Figure 2: Comparison of spectroscopic (Böhm et al. 2003; Noll et al. 2004) and photometric redshifts for different galaxy types and quasars in the FDF (362 objects).
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{0909f03a.eps}\hspace*{1cm} \includegraphics[width=8.7cm,clip]{0909f03b.eps} \end{figure}$	Figure 3: Left panel: histogram of the reduced $\chi ^2$ for all galaxies in the FDF as obtained for the best fitting template and redshift. The dotted vertical line indicates the median reduced $\chi ^2$ . Right panel: histogram of the photometric redshift errors. The error distribution can be approximated by a Gaussian centered at 0.006 with an rms of 0.028 (dotted line).
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{0909f08.eps} \end{figure}$	Figure 8: $1 \sigma$ and $2\sigma$ confidence levels of the parameters a and b in different bands (1500 Å, 2800 Å, u', g' and B) for the evolutionary model described in the text. The values for a and b can be found in Table 4.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0909f09a.eps}\hspace*{4mm} \includegraphics[width=8.5cm,clip]{0909f09b.eps} \end{figure}$	Figure 9: Redshift evolution of $M^\ast$ ( left panel) and $\phi ^\ast$ ( right panel) for the filters g' (filled squares), u' (open triangles) and the two UV bands at 2800 Å and 1500 Å (filled circles). The arrows mark the values for $M^\ast$ and $\phi ^\ast$ as derived in the SDSS (Blanton et al. 2001).
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