All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{1204fg4a.ps}\hspace*{5mm} \includegraphics[width=8cm,clip]{1204fg4b.ps}\end{figure}$ Figure 4: Polarization images of the Southern lobe of the source B3-1343+386 at 5.0 GHz ( left) and 8.4 GHz ( right). The vectors superimposed on the I contours show the percentage polarization and the position angle of the $\vec{E}$ vector. The restoring beam is given by the ellipse in the bottom left corner of each image. The image at 8.4 GHz was produced using maxima uv-ranges and restoring beam identical to those at 5.0 GHz.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{aa1204f5.eps}\end{figure}$ Figure 5: Polarization image of the Westernmost region of the source B3-2304+377 at 5.0 GHz. The vectors superimposed on the I contours show the percentage polarization and the position angle of the $\vec{E}$ vector. The restoring beam is given by the ellipse in the bottom left corner.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=16.4cm,clip]{aa1204f6.eps}\end{figure}$ Figure 6: Examples of spectral fits in the lobes (JP model), hot spot (power law) and core (inverted spectrum) of B3-0147+400 ( left) and B3-2358+406 ( right). The values of the local spectral indices are reported in the spectrum of each component. The green line connects the flux density measurements, while the blue line represents the best fit to the spectrum. No fit has been attempted for the core region in both sources.
Open with DEXTER

In the text

$\begin{figure*}\special{psfile=1204fg1a.ps voffset=-270 hoffset=-20 hscale=40 vs... ...204fg1f.ps voffset=-400 hoffset=220 hscale=40 vscale=40 angle=270} \end{figure*}$ Figure 1: VLBA images at 5.0 (left) and 8.4 (right) GHz. For each image we give the following information on the plot itself: a) Peak flux density in mJy/beam; b) First contour intensity ( f.c., again in mJy/beam), which is generally = 3 r.m.s. of the noise; contour levels increase by a factor of 2; c) The restoring beam is plotted on the bottom left corner of each image.
Open with DEXTER

In the text

$\begin{figure*}\special{psfile=1204fg1g.ps voffset=-250 hoffset=-20 hscale=33 vs... ...{psfile=1204fg1l.ps voffset=-720 hoffset=240 hscale=40 vscale=40 } \end{figure*}$ Figure 1: Continued.
Open with DEXTER

In the text

$\begin{figure*}\special{psfile=1204fg1m.ps voffset=-260 hoffset=-20 hscale=35 vs... ...04fg1r.ps voffset=-425 hoffset=220 hscale=40 vscale=40 angle=270} \end{figure*}$ Figure 1: Continued.
Open with DEXTER

In the text

$\begin{figure*}\special{psfile=1204fg1s.ps voffset=-260 hoffset=-20 hscale=40 vs... ...l{psfile=1204fg1t.ps voffset=-260 hoffset=260 hscale=40 vscale=35} \end{figure*}$ Figure 1: Continued.
Open with DEXTER

In the text

$\begin{figure*}\special{psfile=1204fg2a.ps voffset=-260 hoffset=-20 hscale=35 vs... ...fg2f.ps voffset=-450 hoffset=230 hscale=35 vscale=35 angle=270 } \end{figure*}$ Figure 2: VLBA images of the sources observed at 5.0 GHz only. For each image we give the following information on the plot itself: a) Peak flux density in mJy/beam; b) First contour intensity (f.c., in mJy/beam), which is generally 3 times the r.m.s. noise on the image plane; contour levels increase by a factor of 2; c) The restoring beam is plotted on the bottom left corner of each image.
Open with DEXTER

In the text

$\begin{figure*}\special{psfile=1204fg2g.ps voffset=10 hoffset=-50 hscale=40 vsca... ...file=1204fg2h.ps voffset=-280 hoffset=260 hscale=40 vscale=40} \par\end{figure*}$ Figure 2: Continued.
Open with DEXTER

In the text

$\begin{figure*}\special{psfile=1204fg3a.ps voffset=-285 hoffset=-20 hscale=40 v... ...{psfile=1204fg3f.ps voffset=-730 hoffset=260 hscale=40 vscale=40} \end{figure*}$ Figure 3: VLBA spectral images between 1.67 and 5.0 GHz. For each spectral index distribution image we provide the following information on the plot itself: a) Peak flux density and first contour (f.c.), in mJy/beam at 5 GHz, corresponding to 3 times the off-source noise on the image plane; contours increase by a factor 2; b) Beam size, represented by the ellipse in the lower left corner; c) Grey-scale range of the spectral index 1.5> $\alpha$ > -1, in the convention $S(\nu )\propto \nu ^{-\alpha }$ . The grey scale is shown by the wedge at the top of each spectral index image. Contours shows the images at 5.0 GHz obtained by using the same uv-range as the 1.67 GHz, and the same restoring beam. Local spectral indices are marked.
Open with DEXTER

In the text

$\begin{figure*}\special{psfile=1204fg3g.ps voffset=10 hoffset=-25 hscale=40 vsc... ...l{psfile=1204fg3l.ps voffset=-710 hoffset=260 hscale=40 vscale=35} \end{figure*}$ Figure 3: Continued.
Open with DEXTER

In the text

$\begin{figure*}\special{psfile=1204fg3m.ps voffset=-270 hoffset=-20 hscale=40 vs... ...l{psfile=1204fg3r.ps voffset=-710 hoffset=260 hscale=40 vscale=35} \end{figure*}$ Figure 3: Continued.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{aa1204f5.eps}\end{figure}$	Figure 5: Polarization image of the Westernmost region of the source B3-2304+377 at 5.0 GHz. The vectors superimposed on the I contours show the percentage polarization and the position angle of the $\vec{E}$ vector. The restoring beam is given by the ellipse in the bottom left corner.
Open with DEXTER

$\begin{figure}\special{psfile=1204fg1a.ps voffset=-270 hoffset=-20 hscale=40 vs... ...204fg1f.ps voffset=-400 hoffset=220 hscale=40 vscale=40 angle=270} \end{figure}$	Figure 1: VLBA images at 5.0 (left) and 8.4 (right) GHz. For each image we give the following information on the plot itself: a) Peak flux density in mJy/beam; b) First contour intensity ( f.c., again in mJy/beam), which is generally = 3 r.m.s. of the noise; contour levels increase by a factor of 2; c) The restoring beam is plotted on the bottom left corner of each image.
Open with DEXTER

$\begin{figure}\special{psfile=1204fg1g.ps voffset=-250 hoffset=-20 hscale=33 vs... ...{psfile=1204fg1l.ps voffset=-720 hoffset=240 hscale=40 vscale=40 } \end{figure}$	Figure 1: Continued.
Open with DEXTER

$\begin{figure}\special{psfile=1204fg2a.ps voffset=-260 hoffset=-20 hscale=35 vs... ...fg2f.ps voffset=-450 hoffset=230 hscale=35 vscale=35 angle=270 } \end{figure}$	Figure 2: VLBA images of the sources observed at 5.0 GHz only. For each image we give the following information on the plot itself: a) Peak flux density in mJy/beam; b) First contour intensity (f.c., in mJy/beam), which is generally 3 times the r.m.s. noise on the image plane; contour levels increase by a factor of 2; c) The restoring beam is plotted on the bottom left corner of each image.
Open with DEXTER

$\begin{figure}\special{psfile=1204fg2g.ps voffset=10 hoffset=-50 hscale=40 vsca... ...file=1204fg2h.ps voffset=-280 hoffset=260 hscale=40 vscale=40} \par\end{figure}$	Figure 2: Continued.
Open with DEXTER

$\begin{figure}\special{psfile=1204fg3g.ps voffset=10 hoffset=-25 hscale=40 vsc... ...l{psfile=1204fg3l.ps voffset=-710 hoffset=260 hscale=40 vscale=35} \end{figure}$	Figure 3: Continued.
Open with DEXTER