$\begin{figure} \par\includegraphics[width=16.15cm,clip]{5473f01.ps}\end{figure}$ Figure 1: The 24 single-dish molecular line spectra used for the model optimisation (histograms). The solid lines show the best-fit results for the model of L1489 IRS (see also Fig. 5).
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In the text

$\begin{figure} \par\includegraphics[width=8.05cm,clip]{5473f02.ps}\end{figure}$ Figure 2: Progression of flattening of the adopted density structure as f is increased from 0 (purely spherical) to 10 in Eq. (1).
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In the text

$\begin{figure} \par\includegraphics[width=7.65cm,clip]{5473f04.ps}\end{figure}$ Figure 4: The histograms show the $\chi ^2$ distributions of models around the best fit position where only one parameter is varied at each time. A Gaussian, centered on the best fit in each panel, is fitted to the distributions. The dispersion of the Gaussians is given in each panel.
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In the text

$\begin{figure} \par\includegraphics[width=16.35cm,clip]{5473f05.ps}\end{figure}$ Figure 5: The combined emission from the L1489 IRS model and the neighbour cloud core. Only spectra which are affected significantly by the cloud core emission are shown here.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{5473f06.eps}\end{figure}$ Figure 6: a) Best possible fit with a spherical model to the HCO⁺ J= 4-3 line. b) The best fit to the same line where the flattening f and the inclination i are kept as free parameters. Below, the residuals are shown with the mean and two standard deviations indicated.
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In the text

$\begin{figure} \par\includegraphics[height=7.1cm,width=7.4cm,clip]{5473f07.eps}\end{figure}$ Figure 7: a) Interferometer map in HCO⁺ J= 1-0; b) the corresponding synthesised map based on our best model; c) and d) models with f=1 and f=8 respectively. The white contour lines show the integrated intensity, starting at 0.25 Jy bm^-1 and increasing in steps of 0.5 Jy bm^-1. The colour scale shows the velocity centroid in units of km s^-1.
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In the text

$\begin{figure} \par\includegraphics[width=8.15cm,clip]{5473f08.eps}\end{figure}$ Figure 8: The top left panel shows the false colour NICMOS image of L1489 IRS from Padgett et al. (1999). In the three remaining panels are shown synthetic three-colour composite images based on our model.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{5473f09.ps}\end{figure}$ Figure 9: An average of the observed ¹²CO P(6)-P(15) lines with a similarly averaged model result over plotted.
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In the text

$\begin{figure} \par\includegraphics[width=16.15cm,clip]{5473f01.ps}\end{figure}$	Figure 1: The 24 single-dish molecular line spectra used for the model optimisation (histograms). The solid lines show the best-fit results for the model of L1489 IRS (see also Fig. 5).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.05cm,clip]{5473f02.ps}\end{figure}$	Figure 2: Progression of flattening of the adopted density structure as f is increased from 0 (purely spherical) to 10 in Eq. (1).
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$\begin{figure} \par\includegraphics[width=8.1cm,clip]{5473f03.eps}\end{figure}$	Figure 3: Layout of the grid cells for a model with f=3.8.
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$\begin{figure} \par\includegraphics[width=7.65cm,clip]{5473f04.ps}\end{figure}$	Figure 4: The histograms show the $\chi ^2$ distributions of models around the best fit position where only one parameter is varied at each time. A Gaussian, centered on the best fit in each panel, is fitted to the distributions. The dispersion of the Gaussians is given in each panel.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=16.35cm,clip]{5473f05.ps}\end{figure}$	Figure 5: The combined emission from the L1489 IRS model and the neighbour cloud core. Only spectra which are affected significantly by the cloud core emission are shown here.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{5473f06.eps}\end{figure}$	Figure 6: a) Best possible fit with a spherical model to the HCO⁺ J= 4-3 line. b) The best fit to the same line where the flattening f and the inclination i are kept as free parameters. Below, the residuals are shown with the mean and two standard deviations indicated.
Open with DEXTER

$\begin{figure} \par\includegraphics[height=7.1cm,width=7.4cm,clip]{5473f07.eps}\end{figure}$	Figure 7: a) Interferometer map in HCO⁺ J= 1-0; b) the corresponding synthesised map based on our best model; c) and d) models with f=1 and f=8 respectively. The white contour lines show the integrated intensity, starting at 0.25 Jy bm^-1 and increasing in steps of 0.5 Jy bm^-1. The colour scale shows the velocity centroid in units of km s^-1.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.15cm,clip]{5473f08.eps}\end{figure}$	Figure 8: The top left panel shows the false colour NICMOS image of L1489 IRS from Padgett et al. (1999). In the three remaining panels are shown synthetic three-colour composite images based on our model.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{5473f09.ps}\end{figure}$	Figure 9: An average of the observed ¹²CO P(6)-P(15) lines with a similarly averaged model result over plotted.
Open with DEXTER