All Figures

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{1252fig3.ps}\end{figure}$ Figure 3: 115 sources with three independent detections have been used to compute the photometric bias caused by the mosaicing of repeated rasters. The ratio between the 14.3 $\mu$ m mean fluxes and the corresponding mosaic fluxes are plotted as a function of their signal to noise ratio on the mosaic. The horizontal line indicates the median ratio ( $bias\_mos =$ 0.915) that we will use to correct the total fluxes extracted from the mosaic.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{1252fig4.ps}\end{figure}$ Figure 4: Correlation of 14.3 $\mu$ m total fluxes for the sources in common in the Shallow and in the Deep catalogues. Fluxes in the Deep have been corrected for the effect of the combination of repeated rasters ( $bias\_mos$ = 0.915) and for the same flux bias as in the Shallow catalogue ( $q_{{\rm med}}$ = 0.84). For sources above 0.25 mJy (crosses) the correlation follows the unitary relation (dashed line).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.7cm,clip]{1252fig5.ps}\end{figure}$ Figure 5: The LW3 measured fluxes are compared with the corresponding ratio of the measured over predicted fluxes. This makes sense for sources with reliable K and J magnitudes (see text for details). As expected, the ratio is close to 1 for stars (asterisks), and greater for galaxies (diamonds). The intermediate objects (squares) should correspond to elliptical galaxies.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{1252fig6.ps}\end{figure}$ Figure 6: We have calibrated the LW2-6.7 $\mu$ m fluxes against model predictions (Aussel & Alexander 2002). The figure shows that for the stars with J and K counterparts, the 6.7 $\mu$ m total fluxes are derived by multiplying for a factor 3.77 the corresponding peak fluxes.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1252fig7.ps}\end{figure}$ Figure 7: For the 63 sources with both LW2 and LW3 detections, the 14.3 $\mu$ m fluxes are plotted against the ratio of the 6.7 and 14.3 $\mu$ m fluxes. As a first approximation, this ratio can be used as a star/galaxy indicator. Sources with high LW2/LW3 should correspond to stars (asterisks in the figure).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1252fig8.ps}\end{figure}$ Figure 8: LW3 fluxes as a function of the optical r' magnitudes for the Lockman Deep ISOCAM sources. The lines indicate the relations where the infrared to optical ratio is constant ( $S(15_{\mu {\rm m}})/S_R=-$ 1, 0, +1, +2). The brightest objects are stars (marked as asterisks): the two exceptions correspond to stars blended with galaxies.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{1252fig29.ps}\vspace*{5mm} \includegraphics[width=6cm,clip]{1252fig30.ps}\end{figure}$ Figure 12: Distribution of the difference in RA (top) and Dec (bottom) between the infrared coordinates and the positions of the optical identifications. In these graphics only sources with highly reliable optical counterparts (stars and isolated objects) have been considered. The distributions have been fitted with Gaussian functions, with dispersion of respectively 0.99'' and 1.24'' for RA and Dec.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{1252fig31.ps}\end{figure}$ Figure 13: Histogram Flux Distributions of the Lockman Deep sources (solid line) compared to that in the Lockman Shallow (dotted line).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{1252fig32.ps}\end{figure}$ Figure 14: Sky coverage as a function of the peak flux in the Lockman Deep and in the Lockman Shallow surveys. Above $\sim$ 0.1 mJy the areal correction does not affect the two samples.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.45cm,clip]{1252fig33.ps}\end{figure}$ Figure 15: Integral source counts for extragalactic ISOCAM sources detected at 14.3 $\mu$ m in the Deep and Shallow survey, without areal and completeness correction. The dotted line refers to the Deep sample, the dashed line to the Shallow one.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{1252fig34.ps}\end{figure}$ Figure 16: 14.3 $\mu$ m differential counts normalized to the Euclidean law ( $N \propto S^{-2.5}$ ). Our estimates (Lockman Deep - grey filled circles, Lockman Shallow - black filled squares) are compared with those from other ISOCAM surveys (A2390 from Altieri et al. 1999 - hexagon; ISO Hubble Deep Field North (HDF-N) from Aussel et al. 1999 - filled circles; ISO Hubble Deep Field South (HDF-S) - open circles, Marano Firback - thin open squares, Marano Ultra-Deep - crosses, Marano Deep - asterisks, and Lockman Deep - triangles from Elbaz et al. 1999; ELAIS S1 from Gruppioni et al. 2002 - thick empty squares). The data are compared with model predictions: Franceschini et al. (2001, dotted line), Franceschini et al. (2004 in preparation, solid line), Pozzi et al. (2004, dot-dashed line). The dashed line represents the expectations from a no-evolution model normalized to the IRAS 12 $\mu$ m local luminosity function (Fang et al. 1998).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{1252fig1.ps}\end{figure}$ Figure 1: Lockman Deep 14.3 $\mu$ m sky coverage. Black regions correspond to $\sim$ 2000 s of exposure time, grey regions to $\sim$ 700 s.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{1252fig2.ps}\end{figure}$ Figure 2: Signal to noise map of the total field observed by ISOCAM in the direction of the Lockman Hole.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=3.9cm,clip]{1252fig9.ps}\hspace*{1.5mm... ....ps}\hspace*{1.5mm} \includegraphics[width=3.9cm,clip]{1252fig12.ps}\end{figure}$ Figure 9: Examples of few STARS in the 14.3 $\mu$ m Lockman catalogue. We report the postage stamps of the R optical image overlayed with the 14.3 $\mu$ m contours (starting from 5- $\sigma$ at increasing signal-to-noise levels). Each map is $\sim$ $1\times 1$ square arcminutes. North is upward, East leftward.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=3.9cm,clip]{1252fig13.ps}\hspace*{1.5m... ...ps}\hspace*{1.5mm} \includegraphics[width=3.9cm,clip]{1252fig20.ps}\end{figure}$ Figure 10: Examples of few ISOLATED OBJECTS in the 14.3 $\mu$ m Lockman catalogue. For this class of sources the optical identification is generally straightforward. The reference for the maps legend is the same as in Fig. 9.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=3.9cm,clip]{1252fig21.ps}\hspace*{1.5m... ....ps}\hspace*{1.5mm} \includegraphics[width=3.9cm,clip]{1252fig28.ps}\end{figure}$ Figure 11: Examples of a few BLENDED OBJECTS: as can be seen in the figure, they look like mergers or small groups. For these sources in the catalogue list we report the main optical associations within a search radius of 10 arcsec (from the major component to those with decreasing significance). The reference for the maps legend is the same as in Fig. 9.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.7cm,clip]{1252fig5.ps}\end{figure}$	Figure 5: The LW3 measured fluxes are compared with the corresponding ratio of the measured over predicted fluxes. This makes sense for sources with reliable K and J magnitudes (see text for details). As expected, the ratio is close to 1 for stars (asterisks), and greater for galaxies (diamonds). The intermediate objects (squares) should correspond to elliptical galaxies.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{1252fig6.ps}\end{figure}$	Figure 6: We have calibrated the LW2-6.7 $\mu$ m fluxes against model predictions (Aussel & Alexander 2002). The figure shows that for the stars with J and K counterparts, the 6.7 $\mu$ m total fluxes are derived by multiplying for a factor 3.77 the corresponding peak fluxes.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1252fig7.ps}\end{figure}$	Figure 7: For the 63 sources with both LW2 and LW3 detections, the 14.3 $\mu$ m fluxes are plotted against the ratio of the 6.7 and 14.3 $\mu$ m fluxes. As a first approximation, this ratio can be used as a star/galaxy indicator. Sources with high LW2/LW3 should correspond to stars (asterisks in the figure).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1252fig8.ps}\end{figure}$	Figure 8: LW3 fluxes as a function of the optical r' magnitudes for the Lockman Deep ISOCAM sources. The lines indicate the relations where the infrared to optical ratio is constant ( $S(15_{\mu {\rm m}})/S_R=-$ 1, 0, +1, +2). The brightest objects are stars (marked as asterisks): the two exceptions correspond to stars blended with galaxies.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{1252fig31.ps}\end{figure}$	Figure 13: Histogram Flux Distributions of the Lockman Deep sources (solid line) compared to that in the Lockman Shallow (dotted line).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{1252fig32.ps}\end{figure}$	Figure 14: Sky coverage as a function of the peak flux in the Lockman Deep and in the Lockman Shallow surveys. Above $\sim$ 0.1 mJy the areal correction does not affect the two samples.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.45cm,clip]{1252fig33.ps}\end{figure}$	Figure 15: Integral source counts for extragalactic ISOCAM sources detected at 14.3 $\mu$ m in the Deep and Shallow survey, without areal and completeness correction. The dotted line refers to the Deep sample, the dashed line to the Shallow one.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{1252fig1.ps}\end{figure}$	Figure 1: Lockman Deep 14.3 $\mu$ m sky coverage. Black regions correspond to $\sim$ 2000 s of exposure time, grey regions to $\sim$ 700 s.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=12cm,clip]{1252fig2.ps}\end{figure}$	Figure 2: Signal to noise map of the total field observed by ISOCAM in the direction of the Lockman Hole.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=3.9cm,clip]{1252fig9.ps}\hspace{1.5mm... ....ps}\hspace{1.5mm} \includegraphics[width=3.9cm,clip]{1252fig12.ps}\end{figure}$	Figure 9: Examples of few STARS in the 14.3 $\mu$ m Lockman catalogue. We report the postage stamps of the R optical image overlayed with the 14.3 $\mu$ m contours (starting from 5- $\sigma$ at increasing signal-to-noise levels). Each map is $\sim$ $1\times 1$ square arcminutes. North is upward, East leftward.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=3.9cm,clip]{1252fig13.ps}\hspace{1.5m... ...ps}\hspace{1.5mm} \includegraphics[width=3.9cm,clip]{1252fig20.ps}\end{figure}$	Figure 10: Examples of few ISOLATED OBJECTS in the 14.3 $\mu$ m Lockman catalogue. For this class of sources the optical identification is generally straightforward. The reference for the maps legend is the same as in Fig. 9.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=3.9cm,clip]{1252fig21.ps}\hspace{1.5m... ....ps}\hspace{1.5mm} \includegraphics[width=3.9cm,clip]{1252fig28.ps}\end{figure}$	Figure 11: Examples of a few BLENDED OBJECTS: as can be seen in the figure, they look like mergers or small groups. For these sources in the catalogue list we report the main optical associations within a search radius of 10 arcsec (from the major component to those with decreasing significance). The reference for the maps legend is the same as in Fig. 9.
Open with DEXTER