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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 ![]() ![]() |
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Figure 4:
Correlation of 14.3 ![]() ![]() ![]() |
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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. |
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Figure 6:
We have calibrated the LW2-6.7 ![]() ![]() |
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Figure 7:
For the 63 sources with both LW2 and LW3 detections, the 14.3 ![]() ![]() |
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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 (
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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. |
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Figure 13: Histogram Flux Distributions of the Lockman Deep sources (solid line) compared to that in the Lockman Shallow (dotted line). |
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Figure 14:
Sky coverage as a function of the peak flux in the Lockman Deep
and in the Lockman Shallow surveys. Above ![]() |
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Figure 15:
Integral source counts for extragalactic ISOCAM sources detected at 14.3 ![]() |
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Figure 16:
14.3 ![]() ![]() ![]() |
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Figure 1:
Lockman Deep 14.3 ![]() ![]() ![]() |
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Figure 2: Signal to noise map of the total field observed by ISOCAM in the direction of the Lockman Hole. |
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Figure 9:
Examples of few STARS in the 14.3 ![]() ![]() ![]() ![]() ![]() |
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Figure 10:
Examples of few ISOLATED OBJECTS in the 14.3 ![]() |
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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. |
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