Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{Gb042_f1.ps} \end{figure}$ Figure 1: ( ${\rm UV}-g$ ) vs. (g-r) color-color diagram for the FOCA sources. The filled circles and stars represent the spectroscopically confirmed galaxies and stars, respectively. Dots are the UV detections with a DPOSS counterpart. The line is: $(m_{\rm UV}-g) = 1.92*(g-r) + 2.92$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{Gb042_f2.ps} \end{figure}$ Figure 2: The normalized redshift distributions for spectroscopically confirmed galaxies. The dotted and dashed lines are the observed N(z) in Q030 and Q089, respectively; the solid line is the modeled N(z) (see Sect. 2.2 for details).
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{Gb042_f3.ps} \end{figure}$ Figure 3: Top panel: the measured autocorrelation function of our UV-selected sample (filled circles). The errors are as described in Sect. 3.2. The solid line shows the best power-law fit to the measurements, while the dashed line shows the best fit using $\delta =0.8$ . Bottom panel: comparison of Poissonian errors (filled circles) and cosmic uncertainties computed using Eq. (38) of Bernstein (1994).
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{Gb042_f4.ps} \end{figure}$ Figure 4: Contours of constant $\chi ^2$ in the ( $A_\omega$ , $\delta$ ) parameter space: the inner and outer solid lines correspond to the 68.3% and 95.4% confidence levels, respectively. The dashed line corresponds to the $(\chi ^2_{\rm min}+1)$ level. The + sign shows the best fit amplitude and slope; the cross indicates the best fit amplitude assuming $\delta =0.8$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{Gb042_f5.ps} \end{figure}$ Figure 5: The correlation lengths derived for the present UV-selected sample (filled circle), the local blue galaxies (star and pentagon symbols), the local active galaxies from 2dFGRS (open square), and the rest-frame UV-selected galaxies at z=3 (filled triangle). The dashed line shows the clustering evolution of the dark matter, following Moustakas & Somerville (2002).
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{Gb042_f1.ps} \end{figure}$	Figure 1: ( ${\rm UV}-g$ ) vs. (g-r) color-color diagram for the FOCA sources. The filled circles and stars represent the spectroscopically confirmed galaxies and stars, respectively. Dots are the UV detections with a DPOSS counterpart. The line is: $(m_{\rm UV}-g) = 1.92*(g-r) + 2.92$ .
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{Gb042_f2.ps} \end{figure}$	Figure 2: The normalized redshift distributions for spectroscopically confirmed galaxies. The dotted and dashed lines are the observed N(z) in Q030 and Q089, respectively; the solid line is the modeled N(z) (see Sect. 2.2 for details).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{Gb042_f4.ps} \end{figure}$	Figure 4: Contours of constant $\chi ^2$ in the ( $A_\omega$ , $\delta$ ) parameter space: the inner and outer solid lines correspond to the 68.3% and 95.4% confidence levels, respectively. The dashed line corresponds to the $(\chi ^2_{\rm min}+1)$ level. The + sign shows the best fit amplitude and slope; the cross indicates the best fit amplitude assuming $\delta =0.8$ .
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$\begin{figure} \par\includegraphics[width=7.3cm,clip]{Gb042_f5.ps} \end{figure}$	Figure 5: The correlation lengths derived for the present UV-selected sample (filled circle), the local blue galaxies (star and pentagon symbols), the local active galaxies from 2dFGRS (open square), and the rest-frame UV-selected galaxies at z=3 (filled triangle). The dashed line shows the clustering evolution of the dark matter, following Moustakas & Somerville (2002).
Open with DEXTER