Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{4137fg1.eps} \end{figure}$ Figure 1: VLBI 6 cm images at four epochs ( left panels), from which we placed an upper limit on the proper motion of the B1 component, relative to B0, in NGC 5506. The proper motion of the B2 component is unreliable due to limited image fidelity. The 6 cm 1994.16 epoch is repeated as the top right panel. The lower three right panels show the 18 cm images. All images are naturally weighted. The VLBA observations were restored with common beams of $7.4~{\rm mas}\times4.3~{\rm mas}$ (6 cm) and $18.5~{\rm mas}\times11.3~{\rm mas}$ (18 cm).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{4137fg2.eps} \end{figure}$ Figure 2: Diagram illustrating the apparent motions in NGC 5506. The peak positions of B1 and B2 from 6 cm global VLBI, EVN and VLBA are plotted relative to B0. Errors are $1~\sigma$ .
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{4137fg3.eps} \end{figure}$ Figure 3: Combined EVN and MERLIN 6 cm image of NGC 5506. Offsets are relative to RA 14:13:14.87953, Dec -03:12:27.6799 (J2000), peak flux density is 37.3 mJy/beam, contours are 1 mJy/beam $~\times$ (2,4,8,16,32), beam size is $16.5~{\rm mas}~\times$ 8.0 mas and natural weighting was used.
Open with DEXTER

In the text

$\begin{figure} \par\subfigure[{NGC~7674} at 18~cm (MERLIN). Offsets are relative... ...]{\includegraphics[angle=270,width=8.1cm,clip]{4137fg5.ps} } \par\end{figure}$ Figure 4: NGC 7674 images.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{4137fg6.eps} \end{figure}$ Figure 5: NGC 2110 at 18 cm (MERLIN). Offsets are relative to RA 05:52:11.38254, Dec -07:27:22.5262 (J2000), peak flux density is 31.4 mJy/beam, contours are 1 mJy/beam $\times$ (-3, 3, 6, 9, $\ldots$ , 30), beam size is 318.0 mas $\times$ 193.4 mas and natural weighting was used. The (u,v) range was $80~{\rm k}\lambda$ to $1000~{\rm k}\lambda$ .
Open with DEXTER

In the text

$\begin{figure} \par\subfigure[MERLIN 6~cm image of~{Mrk~1210}. Offsets are relat... ... was used.]{\includegraphics[width=7.2cm,clip]{4137fg10.eps} }\\ \end{figure}$ Figure 6: Mrk 1210 images.
Open with DEXTER

In the text

$\begin{figure} \par\subfigure[]{ \includegraphics[angle=270,width=7.8cm,clip]{4... ...e[]{ \includegraphics[angle=270,width=7.8cm,clip]{4137fg12.ps} } \end{figure}$ Figure 7: Upper panel: histogram of spectral indices between 18 cm and 6 cm for the Seyfert sample in Table 4. Upper and lower limits are indicated by arrows. Lower panel: distribution of angles between pc- and kpc-scale structure. For comparison with data from radio galaxies, the data from Table 6 have been reflected onto the range $0^{\circ }$ to $90^{\circ }$ .
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{4137fg2.eps} \end{figure}$	Figure 2: Diagram illustrating the apparent motions in NGC 5506. The peak positions of B1 and B2 from 6 cm global VLBI, EVN and VLBA are plotted relative to B0. Errors are $1~\sigma$ .
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{4137fg3.eps} \end{figure}$	Figure 3: Combined EVN and MERLIN 6 cm image of NGC 5506. Offsets are relative to RA 14:13:14.87953, Dec -03:12:27.6799 (J2000), peak flux density is 37.3 mJy/beam, contours are 1 mJy/beam $~\times$ (2,4,8,16,32), beam size is $16.5~{\rm mas}~\times$ 8.0 mas and natural weighting was used.
Open with DEXTER

$\begin{figure} \par\subfigure[{NGC~7674} at 18~cm (MERLIN). Offsets are relative... ...]{\includegraphics[angle=270,width=8.1cm,clip]{4137fg5.ps} } \par\end{figure}$	Figure 4: NGC 7674 images.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{4137fg6.eps} \end{figure}$	Figure 5: NGC 2110 at 18 cm (MERLIN). Offsets are relative to RA 05:52:11.38254, Dec -07:27:22.5262 (J2000), peak flux density is 31.4 mJy/beam, contours are 1 mJy/beam $\times$ (-3, 3, 6, 9, $\ldots$ , 30), beam size is 318.0 mas $\times$ 193.4 mas and natural weighting was used. The (u,v) range was $80~{\rm k}\lambda$ to $1000~{\rm k}\lambda$ .
Open with DEXTER

$\begin{figure} \par\subfigure[MERLIN 6~cm image of~{Mrk~1210}. Offsets are relat... ... was used.]{\includegraphics[width=7.2cm,clip]{4137fg10.eps} }\\ \end{figure}$	Figure 6: Mrk 1210 images.
Open with DEXTER

$\begin{figure} \par\subfigure[]{ \includegraphics[angle=270,width=7.8cm,clip]{4... ...e[]{ \includegraphics[angle=270,width=7.8cm,clip]{4137fg12.ps} } \end{figure}$	Figure 7: Upper panel: histogram of spectral indices between 18 cm and 6 cm for the Seyfert sample in Table 4. Upper and lower limits are indicated by arrows. Lower panel: distribution of angles between pc- and kpc-scale structure. For comparison with data from radio galaxies, the data from Table 6 have been reflected onto the range $0^{\circ }$ to $90^{\circ }$ .
Open with DEXTER