All Figures

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{3013fig1.ps} \end{figure}$ Figure 1: The number of foreground galaxies as a function of 2MASS small aperture (7 $^{\prime \prime }$ ) magnitude from the Large Galaxy Atlas (Jarrett et al. 2003).
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{3013fig2.ps} \end{figure}$ Figure 2: The histogram of the Hubble types in this paper's sample. The HST Distance Scale Key project selected in favour of late-type spirals. However, most spiral galaxy types later then Sab are in our sample.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3013fig3.ps} \end{figure}$ Figure 3: Top: the number of field galaxies as a function of 2MASS surface brightness: the distant galaxies from the science field (solid) and the synthetic fields (shaded) without dimming (A = 0). Second from the top: the opacity in I (F814W), in magnitudes, as a function of H-band surface brightness in 2MASS (Kleinmann et al. 1994) images. The point at 17.5 mag arcsec^-2 is not based on sufficient statistics for a good comparison. Third from the top: the opacity in I as a function of H-band surface brightness, for those regions classified as "spiral arm''. Bottom: the opacity in I as a function of H-band surface brightness, for those regions classified as disk region, not part of a spiral arm.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{3013fig4.ps} \end{figure}$ Figure 4: Top: the number of field galaxies as a function of 2MASS surface brightness; the distant galaxies from the science field (solid) and the synthetic fields (shaded) without dimming (A = 0). Second from the top: the opacity in I ( F814W), in magnitudes, as a function of J-band surface brightness in 2MASS (Kleinmann et al. 1994) images. Third from the top: the opacity in I as a function of J-band surface brightness, for those regions classified as "spiral arm''. Bottom: the opacity in I as a function of J-band surface brightness, for those regions classified as disk region, not part of a spiral arm.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3013fig5.ps} \end{figure}$ Figure 5: Top: the number of field galaxies as a function of 2MASS surface brightness; the distant galaxies from the science field (solid) and the synthetic fields (shaded) without dimming (A = 0). Second from the top: the opacity in I ( F814W), in magnitudes, as a function of K-band surface brightness in 2MASS (Kleinmann et al. 1994) images. Third from the top: the opacity in I as a function of K-band surface brightness, for those regions classified as "spiral arm''. Bottom: the opacity in I as a function of K-band surface brightness, for those regions classified as disk region, not part of a spiral arm.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3013fig6.ps} \end{figure}$ Figure 6: Top panel: the number of field galaxies as a function of 2MASS surface brightness, but at a much smaller sampling scale than Fig. 5. The distant galaxies from the science field (solid) and the synthetic fields (shaded) without dimming (A = 0). Bottom: the opacity in I ( F814W) in magnitudes, as a function of K-band surface brightness in 2MASS (Kleinmann et al. 1994) images.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{3013fig7.ps} \end{figure}$ Figure 7: The relation between (H-K) color and I-band extinction ( bottom). Top panel shows the number of distant galaxies for each color bin.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3013fig8.ps} \end{figure}$ Figure 8: The relation between (J-K) color and I-band extinction ( bottom). Top panel shows the number of distant galaxies for each color bin.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{3013fig9.ps} \end{figure}$ Figure 9: The scalelengths of extinction and light in the I band for those galaxies in both our sample that of Macri et al. (2000). Most of scalelengths of the dust are much larger than those of the light, contrary to earlier results but a few are negative.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3013fig10.ps} \end{figure}$ Figure 10: The average extinction derived from the number of distant galaxies compared to the extinction derived from the Cepheid reddening (E(V-I)) from Freedman et al. (2001). There is no clear linear relation (dashed line). The Cepheid extinctions saturate at higher opacities as the Distance Scale project selected against high-extinction Cepheids. Note that cosmic variance in the number of background galaxies can produce a negative opacity value.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{3013fig1.ps} \end{figure}$	Figure 1: The number of foreground galaxies as a function of 2MASS small aperture (7 $^{\prime \prime }$ ) magnitude from the Large Galaxy Atlas (Jarrett et al. 2003).
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{3013fig2.ps} \end{figure}$	Figure 2: The histogram of the Hubble types in this paper's sample. The HST Distance Scale Key project selected in favour of late-type spirals. However, most spiral galaxy types later then Sab are in our sample.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3013fig6.ps} \end{figure}$	Figure 6: Top panel: the number of field galaxies as a function of 2MASS surface brightness, but at a much smaller sampling scale than Fig. 5. The distant galaxies from the science field (solid) and the synthetic fields (shaded) without dimming (A = 0). Bottom: the opacity in I ( F814W) in magnitudes, as a function of K-band surface brightness in 2MASS (Kleinmann et al. 1994) images.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{3013fig7.ps} \end{figure}$	Figure 7: The relation between (H-K) color and I-band extinction ( bottom). Top panel shows the number of distant galaxies for each color bin.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3013fig8.ps} \end{figure}$	Figure 8: The relation between (J-K) color and I-band extinction ( bottom). Top panel shows the number of distant galaxies for each color bin.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{3013fig9.ps} \end{figure}$	Figure 9: The scalelengths of extinction and light in the I band for those galaxies in both our sample that of Macri et al. (2000). Most of scalelengths of the dust are much larger than those of the light, contrary to earlier results but a few are negative.
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