Astronomy & Astrophysics

All Figures

$\begin{figure} \par\resizebox{7.8cm}{!}{\includegraphics[clip]{fig1_ms3644.ps}} \end{figure}$ Figure 1: An outline of all CCD frames contained in the I-band stack. Shown in this figure are four separate pointings of the CFH12K camera. At each pointing there are 7-8 individual exposures comprising 12 CCDs in each. At the scale of this plot, it is not possible to see the displacement caused by the dither pattern offsets.
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In the text

$\begin{figure} \par\resizebox{7.9cm}{!}{\includegraphics[clip]{fig2_ms3644.ps}} \par\end{figure}$ Figure 2: Seeing distribution for CCD images used in the F02 mosaic for each of the four filters. The dashed line shows the median seeing; note that in all cases this is less than 1''. All images with a seeing higher than 1.2'' were discarded and are not shown in this figure.
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In the text

$\begin{figure} \par\resizebox{7.6cm}{!}{\includegraphics[clip]{fig3_ms3644.ps}} \end{figure}$ Figure 3: Positions of USNO sources compared to point-like sources with $17.5<I_{\rm AB}<22.0$ in the final 1.2 deg² stacked image. The inner and outer circles (at $0.5\hbox {$^{\prime \prime }$ }$ and $1.0\hbox {$^{\prime \prime }$ }$ ) enclose 68% and 90% of all objects respectively. The dotted lines cross each other at the position of the centroid, which is at $(\Delta \alpha ,\Delta \delta )=(-0.03\hbox {$^{\prime \prime }$ },0.00\hbox {$^{\prime \prime }$ })$ .
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In the text

$\begin{figure} \par\resizebox{7.3cm}{!}{\includegraphics[angle=-90,clip]{fig4_ms3644.ps}} \end{figure}$ Figure 4: Positions of USNO sources compared to point-like objects in the I-stack as a function of right ascension and declination, displaying the uncertainty per co-ordinate. The inner dashed lines enclose $68\%$ of all sources and are at $\vert\Delta\alpha\vert\sim0.38\hbox{$^{\prime\prime}$ }$ and $\vert\Delta\delta\vert\sim0.32\hbox{$^{\prime\prime}$ }$ ; the outer dot-dashed lines enclosing $90\%$ of all sources are at $\vert\Delta\alpha\vert\sim0.80\hbox{$^{\prime\prime}$ }$ and $\vert\Delta\delta\vert\sim0.70\hbox{$^{\prime\prime}$ }$ .
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In the text

$\begin{figure} \par\resizebox{7.6cm}{!}{\includegraphics[clip]{fig5_ms3644.ps}} \end{figure}$ Figure 5: Positions of unsaturated point-like sources in the I-stack image compared with objects extracted from the B stacked image. For clarity only one point in ten is shown. The circles at $0.11\hbox {$^{\prime \prime }$ }$ and $0.26\hbox {$^{\prime \prime }$ }$ enclose $68\%$ and $90\%$ of all sources respectively. The dotted lines cross each other at the position of the centroid, which is at $(\Delta \alpha ,\Delta \delta )=(-0.01\hbox {$^{\prime \prime }$ },-0.01\hbox {$^{\prime \prime }$ })$ .
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In the text

$\begin{figure} \par\resizebox{7.6cm}{!}{\includegraphics[angle=-90,clip]{fig6_ms3644.ps}} \end{figure}$ Figure 6: Residuals between I and B stacks as a function of right ascension and declination. The inner dashed lines enclose $68\%$ of all sources and are at $\vert\Delta\alpha\vert\sim0.08\hbox{$^{\prime\prime}$ }$ and $\vert\Delta\delta\vert\sim0.08\hbox{$^{\prime\prime}$ }$ ; the outer dot-dashed lines enclosing $90\%$ of all sources are at $\vert\Delta\alpha\vert\sim0.18\hbox{$^{\prime\prime}$ }$ and $\vert\Delta\delta\vert\sim0.18\hbox{$^{\prime\prime}$ }$ .
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In the text

$\begin{figure} \par\resizebox{6.2cm}{!}{\includegraphics[clip]{fig7_ms3644.ps}} \end{figure}$ Figure 7: Object half-light radius as a function of $I_{\rm AB}$ magnitude. In the upper panel, we show the half-light radius in pixels (normalised by full-field mean of 2.5 pixels) over the full mosaic both for point-like (solid points) and extended sources (light points). In the lower panel each object's half-light radius has been normalised by the local mode, computed using the adaptive classifier (in both panels, for clarity, only a fraction of all objects are shown).
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In the text

$\begin{figure} \par\resizebox{7.8cm}{!}{\includegraphics[clip]{fig8_ms3644.ps}} \end{figure}$ Figure 8: Distribution of bright galaxies. The points show galaxies (extended sources) with $18.0<I_{\rm AB}<21.0$ . Masked regions are also indicated.
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In the text

$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics[clip]{fig9_ms3644.ps}} \end{figure}$ Figure 9: Peak surface brightness as a function of $I_{\rm AB}$ total magnitude. Detected galaxies are shown as the black dots, the open circles show the spurious detections. The stellar locus is represented by the solid line. Most galaxies lie nearby to this locus. The contour lines indicate the $50\%$ , $70\%$ and $90\%$ completeness limits. The numbers represent the fraction of objects recovered at each combination of total magnitude and peak surface brightness.
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In the text

$\begin{figure} \par\resizebox{8cm}{!}{\includegraphics[clip]{fig10_ms3644.ps}} \end{figure}$ Figure 10: Measured incompleteness as a function of position (decimal declination and right ascension) for the I-band mosaic. The grey-scale contours indicate, at each position, the fraction of stellar objects which were recovered. Input magnitudes were distributed uniformly in the range $23.75<I_{\rm AB}<24.25$ . The thick lines show the location of the masked regions.
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In the text

$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics[clip]{fig11_ms3644.ps}} \end{figure}$ Figure 11: $B_{\rm AB}$ -selected galaxy counts (filled symbols), compared to a selection of recent results from the literature. The dotted lines shows the best fitting slope computed in the magnitude ranges $20.0<B_{\rm AB}<24.0$ and $24.0<B_{\rm AB}<25.5$ . Error bars are smaller than our symbols and are not shown.
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In the text

$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics[clip]{fig12_ms3644.ps}} \end{figure}$ Figure 12: $V_{\rm AB}$ -selected galaxy counts (filled symbols), compared to a selection of recent results from the literature. Error bars are smaller than our symbols and are not shown.
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In the text

$\begin{figure} \par\resizebox{8.3cm}{!}{\includegraphics[clip]{fig13_ms3644.ps}} \end{figure}$ Figure 13: $R_{\rm AB}$ -selected galaxy counts (filled symbols), compared to a selection of recent results from the literature. Error bars are smaller than our symbols and are not shown.
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In the text

$\begin{figure} \par\resizebox{8.3cm}{!}{\includegraphics[clip]{fig14_ms3644.ps}} \end{figure}$ Figure 14: $I_{\rm AB}-$ selected galaxy and star counts (filled circles and squares respectively), compared to a selection of recent results from the literature (open symbols). For the galaxy counts, in all cases our (Poisson) error bars are smaller than the symbols and are not plotted. The dotted line shows the best fitting slope computed in the magnitude range $20<I_{\rm AB}<24$ . The solid line shows the predictions of the galactic model of Robin et al., computed at the galactic latitude of our survey.
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In the text

$\begin{figure} \par\resizebox{8.4cm}{!}{\includegraphics[clip]{fig15_ms3644.ps}}\end{figure}$ Figure 15: $(B-V)_{\rm AB}$ vs. $(V-I)_{\rm AB}$ colours for (filled points) compared to synthetic colours computed from library of Pickles (open circles).
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In the text

$\begin{figure} \par\resizebox{6.1cm}{!}{\includegraphics[clip]{fig16_ms3644.ps}}\end{figure}$ Figure 16: Stellar colours as a function of position for each of the four pointings. In each pointing we compute the median $(B-V)_{\rm AB}$ and $(R-I)_{\rm AB}$ colours in bins of $(V-I)_{\rm AB}$ (upper and lower panels respectively). This is represented as the four different line styles. The regions are defined as follows: solid line: south-west, dotted line: north-east; dashed line: south-east, dot-dashed line: north-west.
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In the text

$\begin{figure} \par\resizebox{6.3cm}{!}{\includegraphics[clip]{fig17_ms3644.ps}} \end{figure}$ Figure 17: Field galaxy colours from our catalogues. In the upper panel, the solid line shows the median $(B-V)_{\rm AB}$ galaxy colour computed in half-magnitude bins as a function of $B_{\rm AB}$ limiting magnitude; in the lower panel, we show the median $(V-I)_{\rm AB}$ colour as a function of $I_{\rm AB}$ magnitude. In both cases we compare with colours from the CFDF survey (symbols).
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In the text

$\begin{figure} \par\resizebox{8.4cm}{!}{\includegraphics[clip]{fig18_ms3644.ps}} \end{figure}$ Figure 18: $(B-V)_{\rm AB}$ vs. $(V-I)_{\rm AB}$ colour-colour diagram for galaxies with $18<I_{\rm AB}<20$ . The greyscale levels are proportional to the numbers of galaxies at each combination of $(V-I)_{\rm AB}$ and $(B-V)_{\rm AB}$ colour. The lines shows model tracks for five galaxy types (two early types, shown by the dotted lines, and three late-types, represented by the solid lines). Tracks are computed in the redshift range 0.0<z<0.4 in intervals of 0.1. Solid symbols show the location of the z=0 point for each track.
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In the text

$\begin{figure} \par\resizebox{8.3cm}{!}{\includegraphics[clip]{fig19_ms3644.ps}} \end{figure}$ Figure 19: Colour-colour diagram for galaxies with $20<I_{\rm AB}<22$ . For this figure, model tracks span the redshifts range 0.0<z<1.0.
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In the text

$\begin{figure} \par\resizebox{8.3cm}{!}{\includegraphics[clip]{fig20_ms3644.ps}} \end{figure}$ Figure 20: Colour-colour diagram for galaxies with $22<I_{\rm AB}<24$ . Model tracks are computed from 0.0<z<3.0.
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In the text

$\begin{figure} \par\resizebox{8.4cm}{!}{\includegraphics[clip]{fig21.eps}}\end{figure}$ Figure 21: Angular clustering of stellar sources, $\omega (\theta )$ as a function of the logarithm of the angular separation in degrees. Filled squares represent objects with $18.0<I_{\rm AB}<20$ ; open circles show sources with $20.0<I_{\rm AB}<21.5$ . For clarity, the fainter magnitude slice has been slightly offset in $\log~(\theta)$ from the brighter one.
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In the text

$\begin{figure} \par\resizebox{8.4cm}{!}{\includegraphics[clip]{fig21_ms3644.ps}}\end{figure}$ Figure 22: $I_{\rm AB}$ -selected galaxy clustering. For each magnitude slice, we show the amplitude of the angular correlation function, $\omega (\theta )$ as a function of the logarithm of the angular separation in degrees, $\log~(\theta)$ . At each magnitude slice, we show the fitted correlation amplitude, including a correction for the integral constraint term.
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In the text

$\begin{figure} \par\resizebox{8.3cm}{!}{\includegraphics[clip]{fig22_ms3644.ps}}\end{figure}$ Figure 23: The amplitude of the angular correlation function at arcminute scales. The filled symbols show $\log A_\omega(1\hbox{$^\prime$ })$ as a function of $I_{\rm AB}$ limiting magnitude as measured in the CFH12K-VIRMOS deep field, assuming a power-law form for the galaxy angular correlation function $\omega (\theta )$ with slope of $\delta =-0.8$ (error bars shown represent only the error bars from the fitting program and do not indicate the true cosmic errors, which are likely to be larger). The open circles and stars show measurements from other recent wide-field surveys.
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In the text

$\begin{figure} \par\resizebox{7.8cm}{!}{\includegraphics[clip]{fig1_ms3644.ps}} \end{figure}$	Figure 1: An outline of all CCD frames contained in the I-band stack. Shown in this figure are four separate pointings of the CFH12K camera. At each pointing there are 7-8 individual exposures comprising 12 CCDs in each. At the scale of this plot, it is not possible to see the displacement caused by the dither pattern offsets.
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$\begin{figure} \par\resizebox{7.9cm}{!}{\includegraphics[clip]{fig2_ms3644.ps}} \par\end{figure}$	Figure 2: Seeing distribution for CCD images used in the F02 mosaic for each of the four filters. The dashed line shows the median seeing; note that in all cases this is less than 1''. All images with a seeing higher than 1.2'' were discarded and are not shown in this figure.
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$\begin{figure} \par\resizebox{7.8cm}{!}{\includegraphics[clip]{fig8_ms3644.ps}} \end{figure}$	Figure 8: Distribution of bright galaxies. The points show galaxies (extended sources) with $18.0<I_{\rm AB}<21.0$ . Masked regions are also indicated.
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$\begin{figure} \par\resizebox{8cm}{!}{\includegraphics[clip]{fig10_ms3644.ps}} \end{figure}$	Figure 10: Measured incompleteness as a function of position (decimal declination and right ascension) for the I-band mosaic. The grey-scale contours indicate, at each position, the fraction of stellar objects which were recovered. Input magnitudes were distributed uniformly in the range $23.75<I_{\rm AB}<24.25$ . The thick lines show the location of the masked regions.
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$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics[clip]{fig11_ms3644.ps}} \end{figure}$	Figure 11: $B_{\rm AB}$ -selected galaxy counts (filled symbols), compared to a selection of recent results from the literature. The dotted lines shows the best fitting slope computed in the magnitude ranges $20.0<B_{\rm AB}<24.0$ and $24.0<B_{\rm AB}<25.5$ . Error bars are smaller than our symbols and are not shown.
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$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics[clip]{fig12_ms3644.ps}} \end{figure}$	Figure 12: $V_{\rm AB}$ -selected galaxy counts (filled symbols), compared to a selection of recent results from the literature. Error bars are smaller than our symbols and are not shown.
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$\begin{figure} \par\resizebox{8.3cm}{!}{\includegraphics[clip]{fig13_ms3644.ps}} \end{figure}$	Figure 13: $R_{\rm AB}$ -selected galaxy counts (filled symbols), compared to a selection of recent results from the literature. Error bars are smaller than our symbols and are not shown.
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$\begin{figure} \par\resizebox{8.4cm}{!}{\includegraphics[clip]{fig15_ms3644.ps}}\end{figure}$	Figure 15: $(B-V)_{\rm AB}$ vs. $(V-I)_{\rm AB}$ colours for (filled points) compared to synthetic colours computed from library of Pickles (open circles).
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$\begin{figure} \par\resizebox{6.3cm}{!}{\includegraphics[clip]{fig17_ms3644.ps}} \end{figure}$	Figure 17: Field galaxy colours from our catalogues. In the upper panel, the solid line shows the median $(B-V)_{\rm AB}$ galaxy colour computed in half-magnitude bins as a function of $B_{\rm AB}$ limiting magnitude; in the lower panel, we show the median $(V-I)_{\rm AB}$ colour as a function of $I_{\rm AB}$ magnitude. In both cases we compare with colours from the CFDF survey (symbols).
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$\begin{figure} \par\resizebox{8.3cm}{!}{\includegraphics[clip]{fig19_ms3644.ps}} \end{figure}$	Figure 19: Colour-colour diagram for galaxies with $20<I_{\rm AB}<22$ . For this figure, model tracks span the redshifts range 0.0<z<1.0.
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$\begin{figure} \par\resizebox{8.3cm}{!}{\includegraphics[clip]{fig20_ms3644.ps}} \end{figure}$	Figure 20: Colour-colour diagram for galaxies with $22<I_{\rm AB}<24$ . Model tracks are computed from 0.0<z<3.0.
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$\begin{figure} \par\resizebox{8.4cm}{!}{\includegraphics[clip]{fig21.eps}}\end{figure}$	Figure 21: Angular clustering of stellar sources, $\omega (\theta )$ as a function of the logarithm of the angular separation in degrees. Filled squares represent objects with $18.0<I_{\rm AB}<20$ ; open circles show sources with $20.0<I_{\rm AB}<21.5$ . For clarity, the fainter magnitude slice has been slightly offset in $\log~(\theta)$ from the brighter one.
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$\begin{figure} \par\resizebox{8.4cm}{!}{\includegraphics[clip]{fig21_ms3644.ps}}\end{figure}$	Figure 22: $I_{\rm AB}$ -selected galaxy clustering. For each magnitude slice, we show the amplitude of the angular correlation function, $\omega (\theta )$ as a function of the logarithm of the angular separation in degrees, $\log~(\theta)$ . At each magnitude slice, we show the fitted correlation amplitude, including a correction for the integral constraint term.
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