All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{7911fig1.eps} \end{figure}$ Figure 1: The observed J-H and H-K colors for the nuclear point source in the HST/NICMOS images of the type 1 AGNs listed in Table 1 are shown as squares with error bars. The colors are presented as the spectral index $\alpha$ in $f_{\nu }$ ( $\propto$ $\nu ^{\alpha }$ ) from the fluxes measured with F110W and F160W filters for J-H color, and F160W and F222M filters for H-K color. The corresponding J-H and H-K colors in Vega magnitude are shown as second axes at the top and right (adopted zero points are 1848, 1084, 635 Jy for F110W, F160W, F222M, respectively). In the top small panel, the objects with only an H-K color are shown. The colors of type 2 (crosses) or intermediate-type objects (triangles) from Alonso-Hererro et al. (2001) have also been plotted for comparison with the type 1 objects. A foreground reddening vector for $A_{\rm V}=1$ is indicated in the upper-left.
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In the text

$\begin{figure} \includegraphics[width=7.7cm,clip]{7911fig2.eps} \end{figure}$ Figure 2: H-K color versus PSF flux fraction in F160W filter image, with synthetic aperture of 6 arcsec diameter (plus signs). Plotted in squares are the H-K colors of the PSF-only flux, i.e. after host galaxy light subtraction (and also after a K-correction; see text).
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{7911fig3.eps} \end{figure}$ Figure 3: The same J-H and H-K colors for the type 1 objects in Fig. 1 are shown but with a K-correction (see text; no-correction for the objects with only H-K color in the upper panel). A grid for J-H and H-K colors of a blackbody with temperature T of 1800, 1600, 1400, 1200, 1000, and 800 K, plus a blue power-law component with $f_{\nu } \propto \nu ^{+1/3}$ which has a fractional contribution $f_{\rm AD}$ at K-band from 0 with a 0.1 step, has also been plotted. The J-H and H-K spectral indices for each set of $(T, f_{\rm AD})$ are calculated using the transmission curves of F110W, F160W and F222M filters for the NIC2 camera. The small gray squares concentrated near the blackbody point of T $\sim$ 1400-1800 K are the colors of our clumpy torus models with type 1 inclinations, while the small gray crosses which are spread toward much redder colors are for intermediate or type 2 inclinations. The small flat grid overlayed on the small gray squares, labeled with inclinations (0-40 $^\circ$ ) and temperature (12-15, in units of 100 K), shows average colors for type 1 models. The tracks of colors for optically-thin graphite grains with different sizes are plotted in gray/blue curves for T = 1200 and 1500 K, where the colors for grain radii a = 0.01, 0.1, 0.3 $\mu$ m are marked with plus signs. The same colors for silicate grains with T = 1500 K and a = 0.01, 0.1, 0.3, 1, and 10 $\mu$ m are marked as triangles and connected with purple dashed lines.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{7911fig4.eps} \end{figure}$ Figure 4: Dust sublimation radius given by Barvainis (1987; solid line) for $T_{\rm sub}$ = 1500 K and grain size a = 0.05 $\mu$ m as a function of UV luminosity $L_{\rm UV}$ , as compared with K-band time-lag radii $R_{\tau _{K}}$ for various type 1 AGNs (Suganuma et al. 2006, and references therein). For the latter, $L_{\rm UV}=6 \ \nu L_{\nu }(V)$ is assumed, and a fit in $R_{\tau _{K}}\propto L^{1/2}$ given by Suganuma et al. is shown with the dotted line. The dashed line is a rough estimation of K-band emitting radii for an untruncated standard accretion disk. Also plotted are the interferometrically-measured radial sizes approximately perpendicular to the innermost linear radio structure for NGC 1068. The UV luminosity for NGC 1068 here is an unobscured (thus estimated) value.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{7911fig5.eps} \end{figure}$ Figure 5: The same comparison as in Fig. 4 but in angular radius versus V-band flux, with the solid and dotted line corresponding to Eqs. (2) and (4), respectively (i.e. $z \ll 1$ cases). The V-band flux for NGC 1068 here is an unobscured (thus estimated) value.
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In the text

$\begin{figure} \par\includegraphics[width=7.1cm,clip]{7911fig6.eps} \end{figure}$ Figure 6: Visibilities, or normalized amplitudes of the Fourier transform, for a model surface brightness image of a 1.2 mas radius ring plus a much more compact source at the center with various flux fractions $f_{\rm AD}$ of the latter. The baselines corresponding to the spatial frequencies in the bottom x-axis are shown in the top x-axis label for an observing wavelength of 2.2 $\mu$ m. The plausible case of $f_{\rm AD}$ = 0.2 is highlighted in red, and the corresponding model image is shown in the inset.
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In the text

$\begin{figure} \par\includegraphics[width=7.1cm,clip]{7911fig7.eps} \end{figure}$ Figure 7: The same as Fig. 6 but for a ring radius of 0.4 mas. The same symbols for each $f_{\rm AD}$ are used.
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In the text

$\begin{figure} \includegraphics[width=7.7cm,clip]{7911fig2.eps} \end{figure}$	Figure 2: H-K color versus PSF flux fraction in F160W filter image, with synthetic aperture of 6 arcsec diameter (plus signs). Plotted in squares are the H-K colors of the PSF-only flux, i.e. after host galaxy light subtraction (and also after a K-correction; see text).
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$\begin{figure} \par\includegraphics[width=7.2cm,clip]{7911fig5.eps} \end{figure}$	Figure 5: The same comparison as in Fig. 4 but in angular radius versus V-band flux, with the solid and dotted line corresponding to Eqs. (2) and (4), respectively (i.e. $z \ll 1$ cases). The V-band flux for NGC 1068 here is an unobscured (thus estimated) value.
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$\begin{figure} \par\includegraphics[width=7.1cm,clip]{7911fig7.eps} \end{figure}$	Figure 7: The same as Fig. 6 but for a ring radius of 0.4 mas. The same symbols for each $f_{\rm AD}$ are used.
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