All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2426f1} \end{figure}$ Figure 1: Sky distribution of the observed ICRF quasars in equatorial coordinates. Each quasar is identified by an internal identification number listed in Col. 11 of Table 2. The dotted line indicates the Galactic equator.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2426f2} \end{figure}$ Figure 2: $\rm O{-}C$ values for reference stars as a function of their image position in pixel units. No correction for the FDP was applied. Stars that were eliminated during the reduction process are not plotted.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{2426f3} \end{figure}$ Figure 3: Relative positions of the 9 mosaic images used for the FDP analysis. Each image is identified with a number. The total area is $10'\times 10'$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2426f4} \end{figure}$ Figure 4: $\rm O{-}C$ values for reference stars as a function of their image position, in pixel units. Correction for the FDP was applied. Stars that were eliminated during the reduction process are not plotted.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2426f5} \end{figure}$ Figure 5: Distribution of the observed quasar magnitudes in the three near-IR bands (full line: J, dotted line: H, dashed line: $K_{\rm s}$ ).
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2426f6} \end{figure}$ Figure 6: Precision of the J, H, and $K_{\rm s}$ magnitudes as a function of the quasar magnitude.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2426f7} \end{figure}$ Figure 7: Comparison of near-IR and radio spectral indices.
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{2426f8a}\hspace*{4mm} \includegraphics[width=6.5cm,clip]{2426f8b} \end{figure}$ Figure 8: Differences in the sense near-IR minus ICRF, before ( left panel) and after ( right panel) correcting for the FDP. The near-IR positions are the mean of the J, H, and $K_{\rm s}$ positions, with errors as in Cols. 4 and 6 of Table 3. In the right panel, the four largest differences have the internal identification numbers of their corresponding objects indicated. Note that the difference for Field 3 falls outside the limits of the figure.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2426f9} \end{figure}$ Figure 9: Distance moduli between the near-IR and ICRF positions as a function of the $K_{\rm s}$ magnitude.
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{2426f10a}\hspace*{4mm} \includegraphics[width=6.5cm,clip]{2426f10b} \end{figure}$ Figure 10: Comparison between the astrometric results from single-image (horizontal axes) and mosaic (vertical axes) modes in the F filter. In the left panel, the two largest differences have the internal identification numbers of their corresponding objects indicated. These were not considered for calculating the rms values printed in each panel.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{2426f11a}\hspace*{2mm} \includegraphics[width=8cm,clip]{2426f11b} \end{figure}$ Figure 11: Comparison of the uncorrected and FDP-corrected positional scatter from the single-image treatment. The reference (UCAC2) star positions were modified according to improvements provided by the global reduction technique. Left panel: without correction for the FDP. Right panel: with correction for the FDP.
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In the text

$\begin{figure}{\resizebox{14.1cm}{!}{\includegraphics{2426f12a}\includegraphics{2426f12b}} }\end{figure}$ Figure 12: SED. Left: 0312-770 (01a). Right: 0431-512 (03p).
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In the text

$\begin{figure}{\resizebox{14.1cm}{!}{\includegraphics{2426f13a}\includegraphics{2426f13b}} }\end{figure}$ Figure 13: SED. Left: 0511-220 (04p). Right: 0521-365 (07p).
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In the text

$\begin{figure}{\resizebox{14.1cm}{!}{\includegraphics{2426f14a}\includegraphics{2426f14b}} }\end{figure}$ Figure 14: SED. Left: 0530-727 (08p). Right: 0528-250 (09a).
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In the text

$\begin{figure}{\resizebox{14.1cm}{!}{\includegraphics{2426f15a}\includegraphics{2426f15b}} }\end{figure}$ Figure 15: SED. Left: 0537-286 (10a). Right: 0614-349 (11p).
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In the text

$\begin{figure}{\resizebox{14.1cm}{!}{\includegraphics{2426f16a}\includegraphics{2426f16b}} }\end{figure}$ Figure 16: SED. Left: 0622-441 (13p). Right: 0629-418 (14a).
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In the text

$\begin{figure}{\resizebox{14.1cm}{!}{\includegraphics{2426f17a}\includegraphics{2426f17b}} }\end{figure}$ Figure 17: SED. Left: 0637-752 (15p). Right: 0646-306 (17a).
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In the text

$\begin{figure}{\resizebox{14.1cm}{!}{\includegraphics{2426f18a}\includegraphics{2426f18b}} }\end{figure}$ Figure 18: SED. Left: 0700-465 (19a). Right: 0743-673 (23a).
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In the text

$\begin{figure}{\resizebox{14.1cm}{!}{\includegraphics{2426f19a}\includegraphics{2426f19b}} }\end{figure}$ Figure 19: SED. Left: 0809-493 (24p). Right: 0823-500 (25p).
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In the text

$\begin{figure}{\resizebox{14.1cm}{!}{\includegraphics{2426f20a}\includegraphics{2426f20b}} }\end{figure}$ Figure 20: SED. Left: 0823-223 (26a). Right: 0834-201 (30p).
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In the text

$\begin{figure}{\resizebox{14.1cm}{!}{\includegraphics{2426f21a}\includegraphics{2426f21b}} }\end{figure}$ Figure 21: SED. Left: 0842-754 (31p). Right: 0919-260 (32p).
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In the text

$\begin{figure}{\resizebox{14.1cm}{!}{\includegraphics{2426f22a}\includegraphics{2426f22b}} }\end{figure}$ Figure 22: SED. Left: 0920-397 (33p). Right: 0925-203 (34p).
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In the text

$\begin{figure}{\resizebox{14.1cm}{!}{\includegraphics{2426f23a}\includegraphics{2426f23b}} }\end{figure}$ Figure 23: SED. Left: 1048-313 (38p). Right: 1101-325 (39p).
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In the text

$\begin{figure}{\resizebox{14.1cm}{!}{\includegraphics{2426f24a}\includegraphics{2426f24b}} }\end{figure}$ Figure 24: SED. Left: 1101-536 (40a). Right: 1104-445 (41a).
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In the text

$\begin{figure}{\resizebox{14.1cm}{!}{\includegraphics{2426f25a}\includegraphics{2426f25b}} }\end{figure}$ Figure 25: SED. Left: 1105-680 (42a). Right:1116-462 (43a).
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In the text

$\begin{figure}{\resizebox{14.1cm}{!}{\includegraphics{2426f26a}\includegraphics{2426f26b}} }\end{figure}$ Figure 26: SED. Left: 1129-580 (44a). Right: 1144-379 (46a).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2426f1} \end{figure}$	Figure 1: Sky distribution of the observed ICRF quasars in equatorial coordinates. Each quasar is identified by an internal identification number listed in Col. 11 of Table 2. The dotted line indicates the Galactic equator.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2426f2} \end{figure}$	Figure 2: $\rm O{-}C$ values for reference stars as a function of their image position in pixel units. No correction for the FDP was applied. Stars that were eliminated during the reduction process are not plotted.
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$\begin{figure} \par\includegraphics[width=6cm,clip]{2426f3} \end{figure}$	Figure 3: Relative positions of the 9 mosaic images used for the FDP analysis. Each image is identified with a number. The total area is $10'\times 10'$ .
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2426f4} \end{figure}$	Figure 4: $\rm O{-}C$ values for reference stars as a function of their image position, in pixel units. Correction for the FDP was applied. Stars that were eliminated during the reduction process are not plotted.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2426f5} \end{figure}$	Figure 5: Distribution of the observed quasar magnitudes in the three near-IR bands (full line: J, dotted line: H, dashed line: $K_{\rm s}$ ).
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2426f6} \end{figure}$	Figure 6: Precision of the J, H, and $K_{\rm s}$ magnitudes as a function of the quasar magnitude.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2426f7} \end{figure}$	Figure 7: Comparison of near-IR and radio spectral indices.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2426f9} \end{figure}$	Figure 9: Distance moduli between the near-IR and ICRF positions as a function of the $K_{\rm s}$ magnitude.
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$\begin{figure} \par\includegraphics[width=6.5cm,clip]{2426f10a}\hspace*{4mm} \includegraphics[width=6.5cm,clip]{2426f10b} \end{figure}$	Figure 10: Comparison between the astrometric results from single-image (horizontal axes) and mosaic (vertical axes) modes in the F filter. In the left panel, the two largest differences have the internal identification numbers of their corresponding objects indicated. These were not considered for calculating the rms values printed in each panel.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{2426f11a}\hspace*{2mm} \includegraphics[width=8cm,clip]{2426f11b} \end{figure}$	Figure 11: Comparison of the uncorrected and FDP-corrected positional scatter from the single-image treatment. The reference (UCAC2) star positions were modified according to improvements provided by the global reduction technique. Left panel: without correction for the FDP. Right panel: with correction for the FDP.
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$\begin{figure}{\resizebox{14.1cm}{!}{\includegraphics{2426f12a}\includegraphics{2426f12b}} }\end{figure}$	Figure 12: SED. Left: 0312-770 (01a). Right: 0431-512 (03p).
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$\begin{figure}{\resizebox{14.1cm}{!}{\includegraphics{2426f13a}\includegraphics{2426f13b}} }\end{figure}$	Figure 13: SED. Left: 0511-220 (04p). Right: 0521-365 (07p).
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$\begin{figure}{\resizebox{14.1cm}{!}{\includegraphics{2426f14a}\includegraphics{2426f14b}} }\end{figure}$	Figure 14: SED. Left: 0530-727 (08p). Right: 0528-250 (09a).
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$\begin{figure}{\resizebox{14.1cm}{!}{\includegraphics{2426f15a}\includegraphics{2426f15b}} }\end{figure}$	Figure 15: SED. Left: 0537-286 (10a). Right: 0614-349 (11p).
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$\begin{figure}{\resizebox{14.1cm}{!}{\includegraphics{2426f16a}\includegraphics{2426f16b}} }\end{figure}$	Figure 16: SED. Left: 0622-441 (13p). Right: 0629-418 (14a).
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$\begin{figure}{\resizebox{14.1cm}{!}{\includegraphics{2426f17a}\includegraphics{2426f17b}} }\end{figure}$	Figure 17: SED. Left: 0637-752 (15p). Right: 0646-306 (17a).
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$\begin{figure}{\resizebox{14.1cm}{!}{\includegraphics{2426f18a}\includegraphics{2426f18b}} }\end{figure}$	Figure 18: SED. Left: 0700-465 (19a). Right: 0743-673 (23a).
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$\begin{figure}{\resizebox{14.1cm}{!}{\includegraphics{2426f19a}\includegraphics{2426f19b}} }\end{figure}$	Figure 19: SED. Left: 0809-493 (24p). Right: 0823-500 (25p).
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$\begin{figure}{\resizebox{14.1cm}{!}{\includegraphics{2426f20a}\includegraphics{2426f20b}} }\end{figure}$	Figure 20: SED. Left: 0823-223 (26a). Right: 0834-201 (30p).
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$\begin{figure}{\resizebox{14.1cm}{!}{\includegraphics{2426f21a}\includegraphics{2426f21b}} }\end{figure}$	Figure 21: SED. Left: 0842-754 (31p). Right: 0919-260 (32p).
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$\begin{figure}{\resizebox{14.1cm}{!}{\includegraphics{2426f22a}\includegraphics{2426f22b}} }\end{figure}$	Figure 22: SED. Left: 0920-397 (33p). Right: 0925-203 (34p).
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$\begin{figure}{\resizebox{14.1cm}{!}{\includegraphics{2426f23a}\includegraphics{2426f23b}} }\end{figure}$	Figure 23: SED. Left: 1048-313 (38p). Right: 1101-325 (39p).
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$\begin{figure}{\resizebox{14.1cm}{!}{\includegraphics{2426f24a}\includegraphics{2426f24b}} }\end{figure}$	Figure 24: SED. Left: 1101-536 (40a). Right: 1104-445 (41a).
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$\begin{figure}{\resizebox{14.1cm}{!}{\includegraphics{2426f25a}\includegraphics{2426f25b}} }\end{figure}$	Figure 25: SED. Left: 1105-680 (42a). Right:1116-462 (43a).
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$\begin{figure}{\resizebox{14.1cm}{!}{\includegraphics{2426f26a}\includegraphics{2426f26b}} }\end{figure}$	Figure 26: SED. Left: 1129-580 (44a). Right: 1144-379 (46a).
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