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$\begin{figure} \par\includegraphics[angle=0,width=14cm]{9606fig1.eps} \end{figure}$ Figure 1: High-spatial resolution SED of the nucleus of NGC 1068, in comparison to thermal dust emission from a torus in the IR and non-thermal synchrotron emission in the radio. The blue line shows the clumpy torus model that was used in this study to model the single-dish IR photometry (diamonds) and interferometric observations by VLTI/MIDI (orange solid line; model: dashed-dotted blue line). The radio data (diamonds) are modeled by a spectrum $F_\nu \propto \nu^{1/3}\exp\left(-(\nu/\nu_{\rm ff})^{-2.1}\right)$ (Synchrotron emission + free-free absorption; green-dotted line) and extrapolated into the infrared. The dashed line shows the synchrotron spectrum attenuated by dust obscuration ( $\tau _V=16.8$ ) to reproduce the J-band data. regimes.
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=14cm]{9606fig2.eps} \end{figure}$ Figure 2: Same as Fig. 1, but with our free-free emission model in the radio. The free-free spectrum was attenuated by dust with $\tau _V=6$ to reproduce the J-band data.
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=13.5cm]{9606fig3.eps} \end{figure}$ Figure 3: Accretion disk contribution to the IR spectrum. A standard accretion disk spectrum $F_\nu \propto \nu^{1/3}\exp(\nu/\nu_{\rm max})$ was adjusted for the assumed parameters $L=2\times10^{45}~{\rm erg/s}$ and $M_{\rm BH}\approx10^7~{M_{\odot}}$ of NGC 1068 (green dotted line) and attenuated by dust obscuration (green dashed line) with $\tau _V=9.6$ to be consistent with the NIR measurements.
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=14cm]{9606fig2.eps} \end{figure}$	Figure 2: Same as Fig. 1, but with our free-free emission model in the radio. The free-free spectrum was attenuated by dust with $\tau _V=6$ to reproduce the J-band data.
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