All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=7.8cm,clip]{0460fg1a.ps}\hsp... ...ace*{4mm} \includegraphics[angle=-90,width=7.8cm,clip]{0460fg1d.ps} \end{figure}$ Figure 1: $S_{\rm P}^{\rm s}$ vs. $S_{\rm P}^{\rm v}~$ for components of resolved sources (top) and for the whole source ( bottom), at 8.5 GHz ( left) and 4.9 GHz ( right). Note that, for clarity, the source 2311+269 has not been included since it has a polarized flux $\protect\ga$ 25 mJy. The dotted line is for $S^{\rm v}_{\rm P} = S^{\rm s}_{\rm P}$ . The crosses represent the 1- $\sigma$ error bars.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{0460fg2a.ps}\par... ...ace*{2mm} \includegraphics[angle=-90,width=8.5cm,clip]{0460fg2c.ps} \end{figure}$ Figure 2: Depolarization versus S/N: at low resolution on top (4.9/8.5 GHz) and central (1.4/8.5 GHz) panels; at high resolution (4.9/8.5 GHz) on bottom panel. In all figures the two lines show the upper and lower bounds of the 95% ( $2\sigma$ ) confidence interval of statistical fluctuations in the absence of depolarization (DP=1).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.05cm,clip]{0460fg3a.ps}\hspace*{4mm} \includegraphics[angle=-90,width=7.6cm,clip]{0460fg3b.ps} \end{figure}$ Figure 3: Distribution of the $\vert\Delta \chi \vert^{4.9}_{8.5}$ at low resolution ( left) and at high resolution ( right), corrected for Galactic rotation, for sources and components with errors on $\Delta \chi \le 12 ^\circ$ .
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In the text

$\begin{figure} \par$\chi^\circ(\lambda)$\includegraphics[angle=-90,width=7.2cm,c... ...$^2$ )]{\includegraphics[angle=-90,width=7.2cm,clip]{0460fg4h.ps} } \end{figure}$ Figure 4: Examples of $\chi (\lambda )$ vs. $\lambda ^2$ fits discussed in the text. A + mark our own data, an $\times$ those from Klein et al (2003). The continuous and the long dashed lines correspond to the RM₃given in Table 3 and to the RM of Klein et al. (2003), respectively. Other lines are alternative fits. $n_{1.4}\times 180^\circ$ ambiguities at 1.4 GHz are also marked. Note the role of the datapoint at 2.7 GHz ( $\lambda^2 = 0.0123 {\rm~ m}^2$ ).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7cm,clip]{0460fg5a.ps}\hspace*{4mm} \includegraphics[angle=-90,width=7cm,clip]{0460fg5b.ps} \end{figure}$ Figure 5: Distribution of three-frequency |RM₃|. Left panel is for the observer frame (Galaxy corrected). Note that RM₃ = 100 rad/m² corresponds to $\Delta \chi ^{4.9}_{8.5}\sim 14^\circ$ . Right panel is for the source frame. Dark bars indicate sources without red-shift for which z=1.05 has been assumed.
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In the text

$\begin{figure} \par\includegraphics[height=8.0cm,angle=-90,clip]{0460fg6a.ps}\hspace*{4mm} \includegraphics[height=8.0cm,angle=-90,clip]{0460fg6a.ps} \end{figure}$ Figure 6: Depolarization ratio vs. rotation angle (4.9/8.5 GHz) (Galaxy corrected) at high ( left) and low ( right) resolutions.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{0460fg7.ps} \end{figure}$ Figure 7: Depolarization (1.4/8.5 GHz) vs. rotation angle (4.9/8.5 GHz). The line represents the effect of bandwidth depolarization at 1.4 GHz (Fig. 23 in Condon et al. 1998).
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In the text

$\begin{figure} \par\includegraphics[height=8.4cm,angle=-90,clip]{0460fg8a.ps}\pa... ...ce*{2mm} \includegraphics[height=8.4cm,angle=-90,clip]{0460fg8c.ps} \end{figure}$ Figure 8: Distribution of $m_{\rm v}$ as a function of LS, at 1.4, 4.9 and 8.5 GHz (from top to bottom). Median values are shown by horizontal segments. Two models, discussed in Sect. 5.4, are shown: the lower curve is for uniform brightness over the whole source extent; the upper curve is for a brightness distribution concentrated in the outermost thirds of the source extent.
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In the text

$\begin{figure} \par\includegraphics[height=8cm,angle=-90,clip]{0460fg9a.ps}\par\vspace*{2mm} \includegraphics[height=8cm,angle=-90,clip]{0460fg9b.ps} \end{figure}$ Figure 9: Distribution of DP as a function of LS with the two models of Fig. 8. Top: 4.9-8.5 GHz; bottom: 1.4-8.5 GHz.
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In the text

$\begin{figure} \par$m_{\rm v}$ (\%)\includegraphics[height=7.2cm,angle=-90,clip]... ...degraphics[height=7.4cm,width=5.2cm,angle=-90,clip]{0460f10h.ps} }\end{figure}$ Figure 10: Fits with the Burn and/or Tribble models for some of the sources discussed in the text. The data points at $\lambda =0.11$ m ( $\nu =2.7$ GHz) are from Klein et al. (2003). The two values of $m_{\rm v}^{1.4}$ (e.g. 0137+401) are the one given in the NVSS catalogue and the one corrected for bandwidth depolarization.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{0460f11a.ps}\hspace*{2mm} \includegraphics[angle=-90,width=8.1cm,clip]{0460f11b.ps} \end{figure}$ Figure 11: Distribution of the Faraday Dispersions in the observer frame ( left) and in the source frame ( right). Dark bars indicate sources without red-shift for which z=1.05 has been assumed.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm,clip]{0460fg12.ps} \end{figure}$ Figure 12: Distribution of the intrinsic fractional polarisation m₀ ( low resolution).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{0460fg13.ps} \end{figure}$ Figure 13: Distribution of intrinsic RM₃ vs. red-shift; data-points in squares represent photometric red-shifts. See Sect. 4.3 for a discussion of uncertainties in RM₃.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{0460f14a.ps}\hspace*{2mm} \includegraphics[angle=-90,width=8.8cm,clip]{0460f14b.ps} \end{figure}$ Figure 14: Distribution vs. red-shift of the intrinsic ( left) and of the observed ( right) Faraday Dispersion. In both figures a circle marks the objects from Table 6; a plus sources with a more uncertain Faraday Dispersion (see text); a square photometric red-shifts. The curve on the right panel represents the expected $\sigma _{\rm obs}$ as a function of z for $\sigma _{\rm sf}=900$ rad/m².
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In the text