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Figure 1:
Distribution of ELAIS-S1 type-1 and -2 AGN in the
z-R-magnitude plane. Best fit linear solutions (![]() ![]() |
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Figure 2: Adopted mid-IR spectral energy distributions (SEDs) for type-2 sources ( top panel) and the corresponding k-corrections as a function of redshift computed for the ISOCAM-LW3 filter ( bottom panel). |
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Figure 3: Distribution in the L15- z space of the total sample of mid-IR type-1 and 2 AGN. The mid-IR luminosity for type-2 sources has been computed applying the Circinus k-correction (see text, Sect. 3.1). The dotted, dashed and dot-dashed lines represent the flux limits at 0.1, 1.0 and 300 mJy respectively. |
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Figure 4:
Type-1 AGN local (z=0.1, continuous line) and
high redshift (z=1.2, dash-dotted line) best fits to the 15![]() ![]() ![]() |
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Figure 5:
Left: mid-IR integral counts for type-1 AGN.
Shaded areas show the RMS and ELAIS observed counts, while symbols (triangle,
star and diamonds) represent the ISO-Deep surveys. The thick solid
line gives the predicted counts from the variable slope fit model ("B'').
Expectations from the fixed faint slope model ("A'') are plotted as a
dashed line. All errors in the observed distributions are quoted at the
1![]() ![]() |
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Figure 6:
Observed and best fit LF for type-2 AGN at
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Figure 7: Left: observed and predicted integral counts for type-2 sources using the the two representative SED: NGC 1068 (thin dashed for the "C'' model and thin continuous for the "D'' model) and Circinus (thick dashed for the "E'' model and thick continuous for the "F'' model). Right: observed and predicted type-2 AGN redshift distribution for the different models mentioned before. Lines as in left panel. Symbols and shaded area in both panels as in Fig. 5. Errors reported in the lower section of both panels have been computed and plotted as described in Fig. 5. |
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Figure 8:
Luminosity-redshift distribution of the type-1
( top) and type-2 ( bottom) AGN. Shaded areas represents
the fraction of incompleteness due to the optical spectroscopic limits.
Contours range from 75% (black) to 95% (light-gray) of the total
area lost and have a 5% step between them. For type-1 AGN ![]() ![]() ![]() |
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Figure 9:
Comparison of LFs at 25![]() ![]() ![]() |
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Figure 10:
The expected Spitzer MIPS integral counts
for AGN at 24![]() ![]() ![]() |
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