![\begin{figure}
\par\includegraphics[width=8.2cm,clip]{5820fig1} \end{figure}](/articles/aa/full/2006/38/aa5820-06/img66.gif) |
Figure 1:
The MIR SEDs of our sample of galaxies. Early- and late-type
Seyferts are shown in the left- and right-hand panel respectively.
Horizontal error bars show the band width of the used filters.
The flux densities of NGC 7314 have been offset by
 erg s-1 cm-2 for clarity. |
| Open with DEXTER | |
In the text
![\begin{figure}
\par\includegraphics[width=8.5cm,clip]{5820fig2} \end{figure}](/articles/aa/full/2006/38/aa5820-06/img67.gif){kind=small} |
Figure 2: Comparison of ISOPHOT-S spectra (dashed histograms) taken from Rigopoulou et al. (1999) and our VISIR photometry (filled circles). Horizontal error bars show the band width of the filters used. |
| Open with DEXTER | |
In the text
![\begin{figure}
\par\includegraphics[width=5cm,clip]{5820fig3} \end{figure}](/articles/aa/full/2006/38/aa5820-06/img72.gif) |
Figure 3: Correlation of MIR to absorption-corrected hard X-ray luminosities for our VISIR sample. Filled diamonds are early-type Seyferts (Type Sy 1.5 or smaller) while filled squares are late-type Seyferts. The power law displayed is the best fit obtained when omitting NGC 4579 (see Sect. 3 for details). |
| Open with DEXTER | |
In the text