All Figures

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{8249f01.eps} \end{figure}$ Figure 1: Reconstructed image of the continuum emission at the highest resolution (0.9 $'' \times$ 0.7''). The contours are linearly spaced with 1 $\sigma$ starting at 2 $\sigma$ and dashed lines are negative contour levels.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{8249f02a.eps}\par\vspace*{2mm} \includegraphics[width=8cm,clip]{8249f02b.eps} \end{figure}$ Figure 2: Zero and first moment plots of the HCO⁺ J = 3-2 emission toward L1489 IRS. Contours are linearly spaced by 2 $\sigma$ with a clip level of 2 $\sigma$ . $\sigma$ equals 1.1 and 2.0 Jy bm^-1 km s^-1 for the natural and uniform weighting schemes, respectively. Negative contours appear as dashed lines.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{8249f03-ONLINE.eps} % \end{figure}$ Figure 3: HCO⁺ emission (1 $\sigma$ ) contours superposed on the near-infrared scattered light image (Padgett et al. 1999).
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{8249f04.eps} \end{figure}$ Figure 4: Spectral map of L1489 IRS. The spectra are evenly spaced with 2''. The bandwidth in each panel is 20 km s^-1. The scale on the y-axis goes from 0 to 2 Jy bm^-1.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{8249f05.eps} \end{figure}$ Figure 5: PV-diagram. This plot shows that the emission on the scales measured by the SMA is entirely dominated by rotation. The black curves show the Keplerian velocity, calculated from the dynamic mass (1.35 $M_\odot$ ) obtained in Paper I. The curves have been inclination corrected with 74 $^\circ$ for the full lines and 40 $^\circ$ for the dashed lines. Contours start at 2 $\sigma$ and increase with 1 $\sigma = 0.12$ Jy beam^-1.
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In the text

$\begin{figure} \par\includegraphics[width=13.8cm,clip]{8249f06.eps} \end{figure}$ Figure 6: Three spectra from the SMA observations with model spectra superposed. The two off-positions are chosen in the direction along the long axis of the object. The offsets are chosen to be a resolution element. Three models are also shown: the dashed line shows the unmodified model from Paper I, the full line is the model from Paper I, but inclined at 40 $^\circ$ , and the dotted line shows a model where HCO⁺ is absent on scales smaller than 200 AU.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{8249f07.eps} \end{figure}$ Figure 7: A slice through the model of L1489 IRS: the top panels show the temperature on different scales and the bottom panels show the corresponding density profiles.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{8249f08.eps} \end{figure}$ Figure 8: The averaged (u,v)-amplitudes of the continuum at 1 mm in both compact and extended configurations. The full line show our model. The compact configuration visibilities cover the (u,v)-distance up to 60 k $\lambda$ . The black triangle marks the total flux at 1 mm (Moriarty-Schieven et al. 1994). The histogram indicates the zero-signal expectation values.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{8249f09.eps} \end{figure}$ Figure 9: The model spectral energy distribution assuming inclinations of 40 $^\circ$ (full line) and 50 $^\circ$ and 74 $^\circ$ (broken lines) plotted on top of flux measurements from the literature (marked by crosses) and the Spitzer/IRS spectrum from 2-40 microns (red line).
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{8249f10.eps} \par\end{figure}$ Figure 10: Three transitions of HCO⁺ observed by single-dish telescope (see Paper I for details) with our model superposed. The quality of the fit is comparable to the fit in Paper I although a disk model has now been included.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{8249f11.eps} \end{figure}$ Figure 11: The SMA spectrum towards the center of L1489 IRS with our model, consisting of a disk which is inclined with respect to the envelope, superposed. As in Fig. 6, the model has been imaged with the (u,v)-spacings from the observations.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{8249f12.eps} \end{figure}$ Figure 12: Similar to Fig. 8 but for the HCO⁺ J= 3-2 measurements. The triangle marks the total flux obtained from the single-dish observations. The amplitudes have been averaged over $\pm$ 5 km s^-1 relative to the systemic velocity. The histogram indicates the zero-signal expectation values. The insert is an enlargement of the longest baselines.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{8249f13.eps} \end{figure}$ Figure 13: An (exaggerated) illustration of the proposed model where the angular momentum axis is changing with radius. The line of sight is illustrated by the dashed line.
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{8249f01.eps} \end{figure}$	Figure 1: Reconstructed image of the continuum emission at the highest resolution (0.9 $'' \times$ 0.7''). The contours are linearly spaced with 1 $\sigma$ starting at 2 $\sigma$ and dashed lines are negative contour levels.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{8249f02a.eps}\par\vspace*{2mm} \includegraphics[width=8cm,clip]{8249f02b.eps} \end{figure}$	Figure 2: Zero and first moment plots of the HCO⁺ J = 3-2 emission toward L1489 IRS. Contours are linearly spaced by 2 $\sigma$ with a clip level of 2 $\sigma$ . $\sigma$ equals 1.1 and 2.0 Jy bm^-1 km s^-1 for the natural and uniform weighting schemes, respectively. Negative contours appear as dashed lines.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{8249f03-ONLINE.eps} % \end{figure}$	Figure 3: HCO⁺ emission (1 $\sigma$ ) contours superposed on the near-infrared scattered light image (Padgett et al. 1999).
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{8249f04.eps} \end{figure}$	Figure 4: Spectral map of L1489 IRS. The spectra are evenly spaced with 2''. The bandwidth in each panel is 20 km s^-1. The scale on the y-axis goes from 0 to 2 Jy bm^-1.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{8249f07.eps} \end{figure}$	Figure 7: A slice through the model of L1489 IRS: the top panels show the temperature on different scales and the bottom panels show the corresponding density profiles.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{8249f08.eps} \end{figure}$	Figure 8: The averaged (u,v)-amplitudes of the continuum at 1 mm in both compact and extended configurations. The full line show our model. The compact configuration visibilities cover the (u,v)-distance up to 60 k $\lambda$ . The black triangle marks the total flux at 1 mm (Moriarty-Schieven et al. 1994). The histogram indicates the zero-signal expectation values.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{8249f09.eps} \end{figure}$	Figure 9: The model spectral energy distribution assuming inclinations of 40 $^\circ$ (full line) and 50 $^\circ$ and 74 $^\circ$ (broken lines) plotted on top of flux measurements from the literature (marked by crosses) and the Spitzer/IRS spectrum from 2-40 microns (red line).
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{8249f10.eps} \par\end{figure}$	Figure 10: Three transitions of HCO⁺ observed by single-dish telescope (see Paper I for details) with our model superposed. The quality of the fit is comparable to the fit in Paper I although a disk model has now been included.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{8249f11.eps} \end{figure}$	Figure 11: The SMA spectrum towards the center of L1489 IRS with our model, consisting of a disk which is inclined with respect to the envelope, superposed. As in Fig. 6, the model has been imaged with the (u,v)-spacings from the observations.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{8249f12.eps} \end{figure}$	Figure 12: Similar to Fig. 8 but for the HCO⁺ J= 3-2 measurements. The triangle marks the total flux obtained from the single-dish observations. The amplitudes have been averaged over $\pm$ 5 km s^-1 relative to the systemic velocity. The histogram indicates the zero-signal expectation values. The insert is an enlargement of the longest baselines.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{8249f13.eps} \end{figure}$	Figure 13: An (exaggerated) illustration of the proposed model where the angular momentum axis is changing with radius. The line of sight is illustrated by the dashed line.
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