All Figures

$\begin{figure} \par\includegraphics[width=17.1cm,clip]{4120_1.eps} \end{figure}$ Figure 1: a) and b) SCUBA maps of IRAS2 at 450 and 850 $\mu$ m, respectively, centered on IRAS2A. c) Observed SED (symbols) and model fit (solid curve). d) and e) Brightness profiles at 450 and 850 $\mu$ m (symbols) and the model fit (solid curve). The dashed curves show the beam profiles. f) Density (dashed line) and temperature (solid line) distributions of best-fit model. See Paper I for details.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{4120_2a.eps}\includegraphics{4120_2b.eps}} \end{figure}$ Figure 2: Maps of continuum emission at 86-89 GHz from OVRO a) and BIMA b). Offsets are with respect to the pointing center of $\alpha(2000)=03^{\rm h}28^{\rm m}56\hbox{$.\!\!^{\rm s}$ }29$ and $\delta(2000)=31^\circ14\hbox{$^\prime$ }33\hbox{$.\!\!^{\prime\prime}$ }93$ . Contours are shown at 3 $\sigma$ , 6 $\sigma$ , 12 $\sigma$ , 24 $\sigma$ and 48 $\sigma$ , where $\sigma$ is the rms noise level of Table 3. The filled ellipses in the lower left corner of the panels indicate the synthesized beam sizes; the large circles show the 50% sensitivity levels of the primary beams.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{4120_3a.eps}\vspace*{4mm} \includegraphics[width=8cm,clip]{4120_3b.eps} \end{figure}$ Figure 3: Visibility amplitudes of the observed continuum emission from the BIMA ( upper panel) and OVRO ( lower panel) observations as a function of projected baseline length in k $\lambda$ centered at the position of IRAS2A. The data are plotted as filled symbols with 1 $\sigma$ error bars, the continuous lines indicate the predictions from the continuum model of jorgensen02 with the same (u,v) sampling as the observations - respectively with (solid) and without (dashed) an unresolved compact source of 22 mJy added to the model. The dotted histogram indicates the zero-expectation level: the expected amplitude signal due to noise alone in the absence of source emission.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{4120_4a.eps}\hspace*{2mm} ... ...c.eps}\hspace*{2mm} \includegraphics[width=8.8cm,clip]{4120_4d.eps} \end{figure}$ Figure 4: Visibility amplitudes of the observed BIMA continuum emission as in Fig. 3 compared to various input models centered at the position of IRAS2A. Upper panels: a) models with changing steepness of the density profile; b) test of different values of the outer radius and inclusion of the interstellar radiation field. Models with an outer radius 3 times larger than the model from Paper I (i.e. 36 000 AU) are shown. Lower panels: c) fit to the inside-out collapse model of Shu (1977) with parameters constrained independently by molecular line observations and SCUBA continuum observations; d) models with changing size of the inner radius.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{4120_5.eps} \end{figure}$ Figure 5: Temperature profile in the outermost region of the envelope without (solid line) and with (dashed line) contributions from the interstellar radiation field. The dotted line indicates the temperature of 10 K corresponding to the envelope outer radius jorgensen02.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{4120_6.eps} \end{figure}$ Figure 6: Derived point source flux plotted against size of the inner envelope cavity.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{4120_7.eps} \end{figure}$ Figure 7: Changes of the emerging SED due to inclusion of a 200 AU outer, 0.3 $M_\odot$ disk: in the upper panel the SEDs from the star + envelope (solid line) and star + envelope + disk models (dashed line) are compared. In both models the central star is represented by a 5000 K blackbody. In the lower panel the ratio between the models are shown - the typical 20% error-level in the flux calibration is illustrated by the solid rectangle.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{4120_8.eps} \end{figure}$ Figure 8: Fits to the SCUBA observations with a inside-out collapse model with an isothermal sound speed, a, of 0.3 km s^-1 and an age of $1.7\times 10^4$ yrs.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{4120_9.eps} \end{figure}$ Figure 9: Constraints on the inside-out collapse model derived from the CS and C³⁴S line intensities, assuming CS and C³⁴S abundances of $1\times 10^{-9}$ and $1\times 10^{-10}$ respectively found in the single power-law density model. The inferred age and sound speed agree well with those derived from the continuum data.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{4120_10a.eps}\hspace*{2mm}... ....eps}\hspace*{2mm} \includegraphics[width=8.2cm,clip]{4120_10d.eps} \end{figure}$ Figure 10: Integrated line emission from the BIMA observations for a) HCN, b) HCO⁺, c) N₂H⁺ and d) C³⁴S plotted over the 3 mm continuum maps (grey-scale). The outflow axes have been marked with straight lines with the red part being solid and blue part being dashed. For HCN and HCO⁺ the emission has been integrated over the red and blue parts of the line (3 to 7 km s^-1 and 9 to 13 km s^-1) shown as the dashed and solid lines, respectively. For N₂H⁺ and C³⁴S the total integrated emission is presented, in the case of N₂H⁺ integrated over the main group of hyperfine lines. For C³⁴S the contours are presented in steps of 3 $\sigma$ , for HCN and HCO⁺ in steps of 5 $\sigma$ and for N₂H⁺ in steps of 7 $\sigma$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{4120_11a.eps}\includegraph... ...clip]{4120_11c.eps}\includegraphics[width=8.3cm,clip]{4120_11d.eps} \end{figure}$ Figure 11: Integrated line emission from the OVRO data, showing a) CS, b) H¹³CO⁺, c) SO and d) CH₃OH. CS is integrated over blue (5 to 9 km s^-1; dashed contours) and red (9 to 13 km s^-1; solid contours) parts of the line with contours in steps of 3 $\sigma$ . For the other molecules lines have been integrated from 7 to 11 km s^-1 and contours are given in steps of 2 $\sigma$ . The grey-scale indicate the 3 mm continuum maps.
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In the text

$\begin{figure} \par\includegraphics[width=5.9cm,clip]{4120_12a.eps}\hspace*{2mm}... ....eps}\hspace*{2mm} \includegraphics[width=5.9cm,clip]{4120_12c.eps} \end{figure}$ Figure 12: First order moment (velocity) maps of the a) HCN, b) HCO⁺(BIMA) and c) CS emission (OVRO). Each map has been overplotted with the total integrated emission in steps of 3 $\sigma$ (solid line contours). The outflow axes have been marked by lines and IRAS2A and IRAS2B continuum sources by stars.
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In the text

$\begin{figure} \par\includegraphics[width=7.1cm,clip]{4120_13.eps} \end{figure}$ Figure 13: The contrast between the N₂H⁺ and SCUBA emission: the N₂H⁺ emission divided by the 450 $\mu$ m continuum emission (normalized) along a straight line with a position angle of 45 $^\circ$ through IRAS2A (solid line) and the 450 $\mu$ m continuum emission in the same positions (dashed line).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{4120_14.eps} \end{figure}$ Figure 14: Comparison between the single-dish observations (dark) and corresponding spectra from the interferometer observations restored with the single-dish beam (red). The spectra from the interferometry observations have been scaled by the factors indicated in the upper right corner (factors 5-12) to include all spectra in the same plots.
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In the text

$\begin{figure} \par\resizebox{8.2cm}{!}{\rotatebox{90}{\includegraphics{4120_15a.eps}}}\par\resizebox{8.2cm}{!}{\includegraphics{4120_15b.eps}} \end{figure}$ Figure 15: Upper panel: comparison between the C³⁴S emission from the single-dish observations using the IRAM 30 m telescope with the BIMA interferometry observations (lower spectrum), offset along the $T_{\rm mb}$ axis by -0.8 K and restored with a 25 $^{\prime \prime }$ beam similar to the single-dish data. The prediction from the 1D static model of the emission brightness distribution from jorgensen02 with abundances derived from single-dish line observations given in Table 4 and sampled at the relevant (u,v)grid has been overplotted on the spectrum in red. Lower panel: visibility amplitude plotted as function of projected baseline length. The predictions from the envelope model with C³⁴S abundance constrained by the single-dish line observations have been overplotted as the solid line. The zero-expectation level is indicated as the dotted histogram.
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In the text

$\begin{figure} \par\resizebox{8.2cm}{!}{\rotatebox{90}{\includegraphics{4120_16a.eps}}}\par\resizebox{8.2cm}{!}{\includegraphics{4120_16b.eps}} \end{figure}$ Figure 16: As in Fig. 15, but for H¹³CO⁺ emission as traced by single-dish observations from the Onsala 20m telescope (44 $^{\prime \prime }$ beam) and interferometry with the OVRO millimeter array. The H¹³CO⁺ interferometer spectra have been scaled by a factor 3 in order to be able to visualize them together with the single-dish observations. The solid line in both panels indicate the model with H¹³CO⁺ abundance constrained by the high J line observations. The dashed line indicate the model constrained by the H¹³CO⁺ J=1-0line. In the lower panel models both with a turbulent broadening of 0.5 and 1.5 km s^-1 have been shown for the abundance constrained by the 1-0 line. The integrated intensities are the same, however.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{4120_17.eps} \end{figure}$ Figure 17: Comparison between interferometry observations and envelope model for CS.
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In the text

$\begin{figure} \par\includegraphics[width=16.7cm,clip]{4120_18.eps} \end{figure}$ Figure 18: Position-velocity diagrams for a) HCN, b) HCO⁺ and c) CS. The solid line indicates a linear gradient fitted to the centroids for the velocity channel. The hyperfine splitting of HCN is seen as the extension of emission along the velocity axis.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{4120_5.eps} \end{figure}$	Figure 5: Temperature profile in the outermost region of the envelope without (solid line) and with (dashed line) contributions from the interstellar radiation field. The dotted line indicates the temperature of 10 K corresponding to the envelope outer radius jorgensen02.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{4120_6.eps} \end{figure}$	Figure 6: Derived point source flux plotted against size of the inner envelope cavity.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{4120_8.eps} \end{figure}$	Figure 8: Fits to the SCUBA observations with a inside-out collapse model with an isothermal sound speed, a, of 0.3 km s^-1 and an age of $1.7\times 10^4$ yrs.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{4120_9.eps} \end{figure}$	Figure 9: Constraints on the inside-out collapse model derived from the CS and C³⁴S line intensities, assuming CS and C³⁴S abundances of $1\times 10^{-9}$ and $1\times 10^{-10}$ respectively found in the single power-law density model. The inferred age and sound speed agree well with those derived from the continuum data.
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$\begin{figure} \par\includegraphics[width=5.9cm,clip]{4120_12a.eps}\hspace{2mm}... ....eps}\hspace{2mm} \includegraphics[width=5.9cm,clip]{4120_12c.eps} \end{figure}$	Figure 12: First order moment (velocity) maps of the a) HCN, b) HCO⁺(BIMA) and c) CS emission (OVRO). Each map has been overplotted with the total integrated emission in steps of 3 $\sigma$ (solid line contours). The outflow axes have been marked by lines and IRAS2A and IRAS2B continuum sources by stars.
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$\begin{figure} \par\includegraphics[width=7.1cm,clip]{4120_13.eps} \end{figure}$	Figure 13: The contrast between the N₂H⁺ and SCUBA emission: the N₂H⁺ emission divided by the 450 $\mu$ m continuum emission (normalized) along a straight line with a position angle of 45 $^\circ$ through IRAS2A (solid line) and the 450 $\mu$ m continuum emission in the same positions (dashed line).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{4120_14.eps} \end{figure}$	Figure 14: Comparison between the single-dish observations (dark) and corresponding spectra from the interferometer observations restored with the single-dish beam (red). The spectra from the interferometry observations have been scaled by the factors indicated in the upper right corner (factors 5-12) to include all spectra in the same plots.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{4120_17.eps} \end{figure}$	Figure 17: Comparison between interferometry observations and envelope model for CS.
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$\begin{figure} \par\includegraphics[width=16.7cm,clip]{4120_18.eps} \end{figure}$	Figure 18: Position-velocity diagrams for a) HCN, b) HCO⁺ and c) CS. The solid line indicates a linear gradient fitted to the centroids for the velocity channel. The hyperfine splitting of HCN is seen as the extension of emission along the velocity axis.
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