All Figures

$\begin{figure} \par\includegraphics[width=12cm,clip]{1767f1.eps}\end{figure}$ Figure 1: Spatial distribution of the $1.5 \times 10^6$ 2MASS galaxies projected in rectangular coordinates. Milky Way objects have been removed. The Cartesian projection is in galactic coordinates and is centered at the anticenter direction. The absence of detected galaxies near the galactic center results from the confusion noise due to high stellar densities.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1767f2.eps}\end{figure}$ Figure 2: Magnitude distribution of galaxies at J ( upper panel) and $K_{\rm s}$ ( lower panel) for latitudes greater than 25 deg and lower than 5 deg. Only sources in the galactic anticenter hemisphere (longitude from 90 to 270 deg) are considered.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1767f3.eps}\end{figure}$ Figure 3: Density plot of the number of foreground stars from a Monte Carlo simulation. The contamination probability depends on the latitude, the longitude (from 90 to 270 deg) and the galaxy size which are taken from the XSC. The y-axis is in log scale and the bar scale indicates the normalized density color coding. As an example, for a galaxy at b=10 deg, the number of foreground stars is between 0.04 and 6 (depending on longitude and galaxy size) and the most common number is about 0.2 star (within the 50% iso-contour).
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In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{1767f4.eps}\end{figure}$ Figure 4: $J-K_{\rm s}$ color contamination ( upper panel) and $K_{\rm s}$ contamination ( lower panel) of a typical galaxy ( $K_{\rm s}=12.5$ , with a 12 $^{\prime \prime }$ diameter) by foreground stars in the galactic plane for l=90 deg ( left) and l=180 deg ( right). In all panels, the cross represents the reference galaxy and the diamonds the brightest foreground star. Solid lines show the contamination level versus the magnitude of the foreground stars. For the upper panels, dotted lines give the probability of reaching the corresponding contamination level.
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In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{1767f5.eps}\end{figure}$ Figure 5: Left panel: color-magnitude diagram for galaxies non-reddened by the ISM ( $I_{100~\mu {\rm m}}<1.5$ MJy sr^-1). The solid line indicates the magnitude-dependent reference for the extinction measurements. It is defined by the equation $J-K_{\rm s} = (16.5-K_{\rm s})^{-1}+0.81$ . Right panel: K-correction for $J-K_{\rm s}$ from Jarrett (2004). The color variation in our galaxy sample is consistent with a maximum redshift of about 0.1.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1767f6.eps}\end{figure}$ Figure 6: Latitude-dependent limiting magnitude used to correct the selection effect of galaxies reddened by the Milky Way disk dust. The curves represent the loss in sensitivity due to confusion noise.
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In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{1767f7.eps}\end{figure}$ Figure 7: Extinction map derived from the median color in adaptive cells containing 5 galaxies each. The scale is labeled in visual magnitude units. The statistical uncertainty is 0.3 mag. As for Fig. 1 no galaxy is detected near the galactic center due to high stellar density.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1767f8.eps}\end{figure}$ Figure 8: Figure from Cambrésy et al. (2001) representing the effective to total optical depth ratio as a function of the warm component fraction. Cold and warm components are described by the modified Planck function $P=B_\nu (T)$ $\times$ $(\lambda /\lambda _0)^{-2}$ with T_c=13.5 K and T_w=17.5 K.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1767f9.eps}\end{figure}$ Figure 9: ISM clumpiness bias derived from a synthetic molecular clouds (Padoan et al. 1998). The solid lines are the isocontours for $\overline {A_{\rm V}}/A_{\rm V}({\rm gal})$ and the dashed lines correspond to the $\sigma (A_{\rm V})/A_{\rm V}$ ratio isocontours labeled in percentage. For $\sigma (A_{\rm V})/A_{\rm V} \approx 25\%$ , the bias in the extinction determination $(\overline {A_{\rm V}}-A_{\rm V}({\rm gal}))/A_{\rm V}({\rm gal})$ is less than 10%.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1767f10a.eps}\vspace*{0.5cm} \includegraphics[width=8cm,clip]{1767f10b.eps}\end{figure}$ Figure 10: Upper panel: difference of extinction between SFD98 and 2MASS galaxies versus the galaxy extinction, restricted to SFD98 pixels not contaminated or corrected for point sources (=covered by the PSCz catalog). The deviation for $A_{\rm V}>1$ is fitted by the dashed line of equation $A_{\rm V}({\rm FIR})=1.31$ $\times$ $A_{\rm V}({\rm gal})- 0.24$ . Lower panel: same as upper panel but with all SFD98 pixels, including those for which the contamination cannot be assessed. The dashed line is $A_{\rm V}({\rm FIR})=1.58$ $\times$ $A_{\rm V}({\rm gal})- 0.66$ .
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1767f11a.eps}\vspace*{0.5cm} \includegraphics[width=8cm,clip]{1767f11b.eps}\end{figure}$ Figure 11: Extinction from 2MASS galaxies (solid line) and from SFD98 (dashed line) versus the galactic latitude cosecant for the northern ( upper panel) and the southern ( lower panel) part of the anticenter hemisphere. The sample is restricted to SFD98 pixels not contaminated or corrected for point sources (=covered by the PSCz catalog).
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{1767f1.eps}\end{figure}$	Figure 1: Spatial distribution of the $1.5 \times 10^6$ 2MASS galaxies projected in rectangular coordinates. Milky Way objects have been removed. The Cartesian projection is in galactic coordinates and is centered at the anticenter direction. The absence of detected galaxies near the galactic center results from the confusion noise due to high stellar densities.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{1767f2.eps}\end{figure}$	Figure 2: Magnitude distribution of galaxies at J ( upper panel) and $K_{\rm s}$ ( lower panel) for latitudes greater than 25 deg and lower than 5 deg. Only sources in the galactic anticenter hemisphere (longitude from 90 to 270 deg) are considered.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{1767f6.eps}\end{figure}$	Figure 6: Latitude-dependent limiting magnitude used to correct the selection effect of galaxies reddened by the Milky Way disk dust. The curves represent the loss in sensitivity due to confusion noise.
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$\begin{figure} \par\includegraphics[width=14cm,clip]{1767f7.eps}\end{figure}$	Figure 7: Extinction map derived from the median color in adaptive cells containing 5 galaxies each. The scale is labeled in visual magnitude units. The statistical uncertainty is 0.3 mag. As for Fig. 1 no galaxy is detected near the galactic center due to high stellar density.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{1767f8.eps}\end{figure}$	Figure 8: Figure from Cambrésy et al. (2001) representing the effective to total optical depth ratio as a function of the warm component fraction. Cold and warm components are described by the modified Planck function $P=B_\nu (T)$ $\times$ $(\lambda /\lambda _0)^{-2}$ with T_c=13.5 K and T_w=17.5 K.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{1767f11a.eps}\vspace*{0.5cm} \includegraphics[width=8cm,clip]{1767f11b.eps}\end{figure}$	Figure 11: Extinction from 2MASS galaxies (solid line) and from SFD98 (dashed line) versus the galactic latitude cosecant for the northern ( upper panel) and the southern ( lower panel) part of the anticenter hemisphere. The sample is restricted to SFD98 pixels not contaminated or corrected for point sources (=covered by the PSCz catalog).
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