All Figures

$\begin{figure} \par\includegraphics[width=16.5cm,keepaspectratio]{9901fig1.eps} \end{figure}$ Figure 1: Polarimetric images of CRL 2136. The top panels are the obtained intensity (Stokes I) images in the H ( left) and K ( right) bands with the polarization vector lines. The field of view is $19\hbox {$^{\prime \prime }$ }\times 19\hbox {$^{\prime \prime }$ }$ . The bottom panels show the degree of linear polarization images in the H ( left) and K ( right) bands. The position of the central star is indicated with the offset of (0 $.\!\!^{\prime\prime}$ 0, 0 $.\!\!^{\prime\prime}$ 0).
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{9901fig2.eps}} \end{figure}$ Figure 2: Cartoon of CRL 2136 illustrating the features detected in our data, the direction of the CO outflow, as well as our interpretation of a disk and envelope structure. The polarization disk on the northeastern side of IRS 1 is not visible in our data.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{9901fig3.eps}} \end{figure}$ Figure 3: The degree of polarization dependence on the grain size ( $a_{\rm max}$ ). The polarization is calculated by means of a single scattering modeling with a spherically symmetric dust shell. For simplicity, bare grains are assumed in this modeling. The minimum grain size $a_{\rm min}$ and the power index of the size distribution are fixed to be 0.005 $\mu$ m and -3.5, respectively.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{9901fig4.New.eps}} \end{figure}$ Figure 4: Comparison of the normalized optical depths of 3 $\mu$ m water ice absorption feature of the model result (filled triangles with dashed line) with an observational result (filled circles with solid line). The observational data was scanned from the paper by Holloway et al. (2002).
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{9901fig5.eps}} \end{figure}$ Figure 5: Cross sections of extinction (solid line), scattering (dashed line), and absorption (dotted line) of the modeled grains as a function of wavelength. Black, red, and blue lines denote the bare grains ( $0.005\le a\le0.45~\mu$ m), warm grains with a crystalline ice mantle ( $0.005\le a\le0.45~\mu$ m, $f_{\rm w}=300\%$ ) (multiplied by a factor of 5), and cold grains with an amorphous ice mantle ( $0.005\le a\le0.45~\mu$ m, $f_{\rm c}=5\%$ ) (multiplied by a factor of 0.1), respectively.
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In the text

$\begin{figure} \par\resizebox{18cm}{!}{\includegraphics{9901fig6.eps}} \end{figure}$ Figure 6: Mass density distribution ( top panels) and dust temperature distribution ( bottom panels). The results of three potential disk models of the SH, TO, and LA are shown in the left, middle, and right columns, respectively. The dust temperature distribution maps are generated with the standard full interacting mode and $3\times 10^8$ photon packets. Although the dust temperature in several cells in the polar direction still suffers from Monte Carlo noise, this does not affect the resulting SED significantly since the noise appears mainly in the low density region (cf. the corresponding mass density distribution maps).
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{9901fig7.eps}} \end{figure}$ Figure 7: Comparisons of SEDs of the acceptable, SH, TO, and LA disk models ( top panel) and the rejected, RB and SL disk models ( bottom panel) with observations. The results of these three disk models are indicated with violet, black, and blue curves, respectively. For the TO disk model, fluxes due to the thermal emission and dust scattering are also shown with a dotted-dashed line and dotted line, respectively. The attenuated stellar flux is not presented because it is less than 10^-14 Wm^-2. The observed data is obtained from Allen et al. (1977) for the JHK band photometry, Willner et al. (1982) for the spectrum from 2.0 $\mu$ m to 15 $\mu$ m, IRAS photometry at 12, 25, 60, and 100 $\mu$ m, and Kastner et al. (1994) for the photometry in sub-millimeter wavelength. An estimated interstellar extinction of 3.2 mag at V-band is dereddened in the observations.
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In the text

$\begin{figure} \par\resizebox{18cm}{!}{\includegraphics{9901fig8.eps}} \end{figure}$ Figure 8: Our model results for the intensity images, polarization vector lines, and the degree of polarization images. The top two rows represent the H band and the bottom two rows the K-band. The left, middle, and right columns are results of the SH, TO, and LA disk models, respectively. In these calculations, the scattering mode with the peeling-off technique and $1\times 10^8$ photon packets were applied. All images were convolved with a Gaussian function with a full width at half maximum of 0 $.\!\!^{\prime\prime}$ 35, which corresponds to the PSF size of our observations.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{9901fig2.eps}} \end{figure}$	Figure 2: Cartoon of CRL 2136 illustrating the features detected in our data, the direction of the CO outflow, as well as our interpretation of a disk and envelope structure. The polarization disk on the northeastern side of IRS 1 is not visible in our data.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{9901fig3.eps}} \end{figure}$	Figure 3: The degree of polarization dependence on the grain size ( $a_{\rm max}$ ). The polarization is calculated by means of a single scattering modeling with a spherically symmetric dust shell. For simplicity, bare grains are assumed in this modeling. The minimum grain size $a_{\rm min}$ and the power index of the size distribution are fixed to be 0.005 $\mu$ m and -3.5, respectively.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{9901fig4.New.eps}} \end{figure}$	Figure 4: Comparison of the normalized optical depths of 3 $\mu$ m water ice absorption feature of the model result (filled triangles with dashed line) with an observational result (filled circles with solid line). The observational data was scanned from the paper by Holloway et al. (2002).
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