Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{2993fg1.ps}\end{figure}$ Figure 1: Layout of the observed K-band pointings for field 0226-04. The raster configuration chosen in order to secure a non-negligible overlap between adjacent pointings is clearly visible. Each pointing is is turn observed through a series of jittered exposures, with jitter box size of 30 $^{\prime \prime }$ (see text for more details).
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2993fg2.ps}\end{figure}$ Figure 2: FWHM seeing distribution of the coadded images for each field observed in K-band. The dashed line shows the median seeing measured in the final mosaicked image. Note that in all cases this value is below $1\hbox {$^{\prime \prime }$ }$ . All images with seeing higher than $1\hbox{$.\!\!^{\prime\prime}$ }3$ were discarded, and are not shown in this plot.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{2993fg3.ps}\end{figure}$ Figure 3: Radial residuals between K-band and I-band positions for unsaturated, point-like sources for each of the four fields. The inner and outer circles enclose 68% and 90% of all objects respectively. The dashed lines cross each other at the position of the centroid of the residuals distribution.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{2993fg4.ps}\end{figure}$ Figure 4: Comparison between the magnitude of corresponding objects in two different K-band coadded images of the same pointing. The sequence of images n4 81-120 was observed during the run of November 1998, while n4 121-160 was observed during the run of November 2002. The agreement for the photometry of these two coadded images is quite good (the mean value of the magnitude difference is only $\Delta {\rm mag} = -0.015$ ).
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{2993fg5.ps}\end{figure}$ Figure 5: Root-mean-square magnitude errors as a function of K-band magnitude. See text for more details.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{2993fg6.ps}\end{figure}$ Figure 6: Half-light radius (r_1/2) as a function of K-band magnitudes for each of our four fields. Heavy dots show point like sources. The histogram on the right hand side shows clearly the locus of point-like sources for objects brighter than the classification limit. Fainter than this magnitude ( $K\sim 17$ ) the star-galaxy separation becomes unreliable.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{2993fg7.ps}\end{figure}$ Figure 7: Ratio of detected input sources as a function of input magnitude for J-band. The input catalogue consists of a flat distribution of simulated point-like sources. The dotted lines show the adopted 50% and 90% completeness magnitudes for each field.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{2993fg8.ps}\end{figure}$ Figure 8: Ratio of detected input sources as a function of input magnitude for K-band. The input catalogue consists of a flat distribution of simulated point-like sources. The dotted lines show the adopted 50% and 90% completeness magnitudes for each field.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2993fg9.ps}\end{figure}$ Figure 9: Differential number counts of stars in J-band for our fields. The continuous lines are the prediction of the model of Robin et al. (2003) for each field.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2993fg10.ps}\end{figure}$ Figure 10: Differential number counts of stars in K-band for our fields. The continuous lines are the prediction of the model of Robin et al. (2003) for each field.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2993fg11.ps}\end{figure}$ Figure 11: Differential J-band number counts in our four fields. Error bars are Poissonian and no correction for stellar contamination has been applied to the points plotted. The dotted line shows the final total raw number densities, obtained by simply adding up raw densities from the four fields, while the heavy line shows the total galaxy densities obtained after correcting for star contamination. On the right of each points, slightly offset for sake of clarity, are shown $+/-1~\sigma$ error bars for total galaxy densities in each bin. See text for more details.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{2993fg12.ps}\end{figure}$ Figure 12: As in Fig. 11, but for K-band.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{2993fg13.ps}\end{figure}$ Figure 13: Our J-band galaxy number counts, in units of number0.5 mag^-1 deg^-2 compared to a literature compilation, including counts from Teplitz et al. (1999), Saracco et al. (2001), Maihara et al. (2001) and Martini (2001).
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{2993fg14.ps}\end{figure}$ Figure 14: The K-band galaxy number counts, in units of number0.5 mag^-1 deg^-2, obtained in this paper are compared to a compilation of those from the literature, including counts from Gardner et al. (1996), Djorgovski et al. (1995), McLeod et al. (1995), Huang et al. (2001), Minezaki et al. (1998), McCracken et al. (2000a), Kümmel & Wagner (2001), Saracco et al. (2001), Totani et al. (2001), Maihara et al. (2001) and Cristóbal-Hornillos et al. (2003).
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{2993fg15.ps}\end{figure}$ Figure 15: Colour-magnitude diagrams for the K-selected samples in each of our fields. The star symbols indicate objects classified as point-like using our star/galaxy classifier. See text for more details.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{2993fg16.ps}\end{figure}$ Figure 16: (J-K) colour distribution for the total K-selected sample in different slices of K-band magnitude. There is a trend towards redder colors at fainter magnitudes, probably reflecting an increasing fraction of high redshift, red, galaxies.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{2993fg17.ps}\end{figure}$ Figure 17: Plot of the correlation function $\omega (\theta )$ for the total sample of stars in the K-band stacks as a function of the logarithm of the angular pair separation in degrees. At all scales displayed the measured correlation values are consistent with zero.
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In the text

$\begin{figure} \par\includegraphics[width=7cm]{2993fg18.ps}\end{figure}$ Figure 18: Results obtained for the amplitude $A_{\omega }$ at $1\deg$ of each of our fields on galaxy sub-samples of different K-band limiting magnitudes. No correction for stellar contamination is applied and the error bars on the amplitude are $1\sigma$ error bars obtained from rms of the fit. The different fields show a good agreement, within the error bars. On the right of each point, slightly offset for sake of clarity, filled circles show our final estimate, from the total sample, of the amplitude of the angular correlation function.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{2993fg19.ps}\end{figure}$ Figure 19: We compare our total sample estimate of the amplitude, $A_{\omega }$ at $1\deg$ , of the angular correlation function with a compilation of results from the literature. We include mesurements from: Daddi et al. (2000), Kümmel & Wagner (2001), McCracken et al. (2000b), Daddi et al. (2003) and Roche et al. (2003). The continous, dotted and dashed lines show, for reference, the models of PLE from Roche et al. (1998), with scaling from local galaxy clustering.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{2993fg1.ps}\end{figure}$	Figure 1: Layout of the observed K-band pointings for field 0226-04. The raster configuration chosen in order to secure a non-negligible overlap between adjacent pointings is clearly visible. Each pointing is is turn observed through a series of jittered exposures, with jitter box size of 30 $^{\prime \prime }$ (see text for more details).
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2993fg2.ps}\end{figure}$	Figure 2: FWHM seeing distribution of the coadded images for each field observed in K-band. The dashed line shows the median seeing measured in the final mosaicked image. Note that in all cases this value is below $1\hbox {$^{\prime \prime }$ }$ . All images with seeing higher than $1\hbox{$.\!\!^{\prime\prime}$ }3$ were discarded, and are not shown in this plot.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{2993fg3.ps}\end{figure}$	Figure 3: Radial residuals between K-band and I-band positions for unsaturated, point-like sources for each of the four fields. The inner and outer circles enclose 68% and 90% of all objects respectively. The dashed lines cross each other at the position of the centroid of the residuals distribution.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{2993fg5.ps}\end{figure}$	Figure 5: Root-mean-square magnitude errors as a function of K-band magnitude. See text for more details.
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$\begin{figure} \par\includegraphics[width=8.8cm]{2993fg6.ps}\end{figure}$	Figure 6: Half-light radius (r_1/2) as a function of K-band magnitudes for each of our four fields. Heavy dots show point like sources. The histogram on the right hand side shows clearly the locus of point-like sources for objects brighter than the classification limit. Fainter than this magnitude ( $K\sim 17$ ) the star-galaxy separation becomes unreliable.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{2993fg7.ps}\end{figure}$	Figure 7: Ratio of detected input sources as a function of input magnitude for J-band. The input catalogue consists of a flat distribution of simulated point-like sources. The dotted lines show the adopted 50% and 90% completeness magnitudes for each field.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{2993fg8.ps}\end{figure}$	Figure 8: Ratio of detected input sources as a function of input magnitude for K-band. The input catalogue consists of a flat distribution of simulated point-like sources. The dotted lines show the adopted 50% and 90% completeness magnitudes for each field.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2993fg9.ps}\end{figure}$	Figure 9: Differential number counts of stars in J-band for our fields. The continuous lines are the prediction of the model of Robin et al. (2003) for each field.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2993fg10.ps}\end{figure}$	Figure 10: Differential number counts of stars in K-band for our fields. The continuous lines are the prediction of the model of Robin et al. (2003) for each field.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{2993fg12.ps}\end{figure}$	Figure 12: As in Fig. 11, but for K-band.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{2993fg13.ps}\end{figure}$	Figure 13: Our J-band galaxy number counts, in units of number0.5 mag^-1 deg^-2 compared to a literature compilation, including counts from Teplitz et al. (1999), Saracco et al. (2001), Maihara et al. (2001) and Martini (2001).
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$\begin{figure} \par\includegraphics[width=7.3cm,clip]{2993fg15.ps}\end{figure}$	Figure 15: Colour-magnitude diagrams for the K-selected samples in each of our fields. The star symbols indicate objects classified as point-like using our star/galaxy classifier. See text for more details.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{2993fg16.ps}\end{figure}$	Figure 16: (J-K) colour distribution for the total K-selected sample in different slices of K-band magnitude. There is a trend towards redder colors at fainter magnitudes, probably reflecting an increasing fraction of high redshift, red, galaxies.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{2993fg17.ps}\end{figure}$	Figure 17: Plot of the correlation function $\omega (\theta )$ for the total sample of stars in the K-band stacks as a function of the logarithm of the angular pair separation in degrees. At all scales displayed the measured correlation values are consistent with zero.
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