All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{4099.f1.ps}\end{figure}$ Figure 1: C¹⁸O and C¹⁷O spectra towards the central position in the maps, which is the peak of the sub-mm emission (Molinari et al. 2000). The dashed line indicates the main component arising from the source. The dotted line with red-shifted velocity shows the second component. In the C¹⁷O (1-0), the vertical lines under the spectrum indicate the position of the hyperfine components.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{4099.f2.ps}\end{figure}$ Figure 2: From top to bottom: CH₃C₂H (6-5), (8-7) and (13-12) IRAM-30 m spectra towards the peak of the sub-mm emission (Molinari et al. 2000). The numbers under the spectra indicate the position of the different K components. The $V_{\rm LSR}$ is relative to the line with K=0.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{4099.f3.ps}\end{figure}$ Figure 3: Top panel: IRAM-30 m map of the main component of the C¹⁸O (1-0) line obtained integrating between -52.5 and -49.0 km s^-1. Contour levels go from $\sim$ 1.5 K km s^-1 (corresponding to $\sim$ $3\sigma$ ), to the maximum value of $\sim$ 4 K km s^-1 in steps of 0.5 K km s^-1 ( $\sim$ $1\sigma$ ). The thick, dashed contour indicates the half maximum power contour. Bottom panel: same as Top for the secondary component of the C¹⁸O (1-0) line, integrated between -49.0 and -45.0 km s^-1. Contour levels range from 1 K km s^-1 ( $\sim$ $3\sigma$ ) to 3.3 K km s^-1 in steps of 0.3 K km s^-1 ( $\sim$ $1\sigma$ ).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7cm,clip]{4099.f4.ps}\end{figure}$ Figure 4: Same as Fig. 3 for the main component of the C¹⁷O (2-1) line, integrated between -52.5 and -49.0 km s^-1. Contour levels go from $\sim$ 1K km s^-1 ( $\sim$ $3\sigma$ level), to 3.3 K km s^-1 in steps of $1\sigma$ .
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7cm,clip]{4099.f5.ps}\end{figure}$ Figure 5: SCUBA map of IRAS 23385+6053 at 850 $\mu$ m (grey scale). Levels range from 0.3 (3 $\sigma$ ) to 1.9 by 0.2 Jy beam^-1. The solid contours represent the C¹⁸O (1-0) map (main component) obtained with the IRAM-30 m telescope (Fig. 3), with the thick line corresponding to the contour at half maximum.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{4099.f6.ps}\end{figure}$ Figure 6: Maps obtained with the PdBI. a) C¹⁸O(1-0) map integrated over the velocity range (-49, -52) km s^-1. Contour levels range from 0.05 ( $\sim$ $3\sigma$ ) to 0.14 by 0.02 Jy beam^-1. The thick contour indicates the half maximum power contour. The spectral rms is $\sim$ 0.014 Jy beam^-1. The grey-scale image shows the 3 mm continuum emission, ranging from $\sim$ 1.9 ( $\sim$ $4 \sigma$ ) to 7.4 by 0.8 mJy beam^-1. The ellipse at the bottom right represents the synthesised beam. b) Same as a) for the C¹⁷O (2-1) line. The map has been integrated over (-47, -52) km s^-1. Contour levels range from 0.03 to 0.09 by 0.015 Jy beam^-1. The grey-scale image represents the 1.3 mm continuum emission, whose countour levels range from 6 to 24 by 2.5 mJy beam^-1. The spectral rms is $\sim$ 0.012 Jy beam^-1. c) Same as b) for the CH₃C₂H (13-12) line, integrated under the K=0and 1 lines. Contour levels range from 0.03 to 0.1 by 0.01 Jy beam^-1. The spectral rms is $\sim$ 0.013 Jy beam^-1
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{4099.f7.ps}\end{figure}$ Figure 7: Flux density comparison between IRAM single-dish (dashed line) spectra and Plateau-de-Bure interferometric spectra (solid line). The interferometric flux densities have been multiplied by a factor of 10 for the CO isotopomers, and by a factor of 3 for the CH₃C₂H lines. The velocity of the CH₃C₂H spectrum is computed with respect to the frequency of the line with K=0.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{4099.f8.ps}\end{figure}$ Figure 8: Top panel: map of the 3 mm continuum emission. The rms level is $\sim$ 0.6 mJy beam^-1 and the signal-to-noise ratio is $\sim$ 15. Contour levels range from 1.6 to 7.8 by 0.6 mJy beam^-1. The thick, dashed contour represents the half maximum power contour. Bottom panel: same as top for 1 mm continuum emission. The rms is $\sim$ 2 mJy beam^-1 at 1.3 mm and the signal-to-noise ratio is $\sim$ 14. Contour levels range from 6 to 24 by 2 mJy beam^-1. The ellipses in the bottom right are the synthesized beams.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=13cm,clip]{4099.f9.ps}\end{figure}$ Figure 9: Left panel: NH₃(1,1) integrated map over the velocity range (-48, -52) km s^-1. Contour levels range from 0.012 ( $\sim$ $3\sigma$ ) to 0.024 by 0.004 Jy beam^-1. The channel spacing of the integrated spectrum (shown over the map) is $\sim$ 1.13 km s^-1. The grey-scale represents the C¹⁸O (1-0) main line emission (Fig. 3). The cross indicates the core position detected with the PdBI. Right panel: same as Left for NH₃(2,2). Contour levels range from 0.012 to 0.025 by 0.004 Jy beam^-1. The channel spacing is $\sim$ 4.9 km s^-1. The ellipses in the bottom-right represent the VLA synthesised beam.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{4099.f10.ps}\end{figure}$ Figure 10: Flux density comparison between Effelsberg-100 m (dashed line) and VLA (solid line) spectra of the NH₃(1,1) and (2,2) lines. VLA fluxes have been multiplied by a factor of 2. The thick vertical lines under the NH₃(1,1) spectrum indicate the position of the two components. The Effelsberg spectra have been resampled to the channel spacing of the VLA spectra.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{4099.f11.ps}\end{figure}$ Figure 11: Image: IRAS 23385+6053 observed at 2 $\mu$ m with the IRCAM of the Palomar telescope in the Ks band (Molinari priv. comm.), which shows the cluster of stars around the core I23385 (indicated by the cross at map center). The dashed contours represent the emission of the two extended radio sources detected at 3.6 cm with the VLA: contour levels range between 0.3 and 3 by 0.3 mJy beam^-1 (Molinari et al. 2002).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{4099.f12.ps}\end{figure}$ Figure 12: Image of IRAS 23385+6053 at 15 $\mu$ m obtained with ISOCAM (Molinari et al. 1998b). The thick polygon represents the 3 $\sigma$ level of the HCO⁺ (1-0) line, and it identifies the core region. The dashed polygons indicate the two clusters of stars which lie around I23385, called "ring'' in the text.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{4099.f13.eps}\end{figure}$ Figure 13: Continuum SED of I23385. Open hexagons and stars indicate MSX and ISOCAM flux densities respectively measured integrating over the "ring'' region of Fig. 12. The filled triangle represents the SCUBA measurement. Filled squares, open squares, filled circles and open circles indicate respectively IRAS, JCMT, PdBI and OVRO data (see also Fig. 2 of Molinari et al. 1998b). The arrows on the bottom left and bottom right respectively indicate the ISOCAM and VLA upper limits ( $3\sigma$ level) of the core flux density. The solid line represents a grey-body fit, with dust temperature T=40 K and dust absorption coefficient $\beta \propto \nu ^{1.9}$ , while the dotted line is a grey-body fit with the same $\beta$ and T=15 K. The dashed line corresponds to a power-law extrapolation of the flux density arising from the "ring'' region.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{4099.f14.ps}\end{figure}$ Figure 14: Top panel: rotation diagram inferred from CH₃C₂H lines observed with the IRAM-30 m telescope. Filled circles, filled triangles and open circles indicate respectively the (6-5), (8-7) and (13-12) transitions. The straight line represents a least square fit to the data. Column densities are source-averaged values using a source diameter of 15 $^{\prime \prime }$ (see Sect. 4.2). Bottom panel: same as Top for CH₃C₂H (13-12) observed with PdBI. The assumed source size is 1.4 $^{\prime \prime }$ . The open circle represents the $3\sigma$ level of the spectrum, taken as an upper limit for the K=4 component.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{4099.f15.ps}\end{figure}$ Figure 15: Ratio between masses deduced from gas ( $M_{\rm line}$ ) or dust ( $M_{\rm cont}$ ) and the corresponding virial mass as a function of the angular diameter. All values have been taken from Tables 5 and 6. Filled circles assume masses of the region estimated from dust, while empty circles assume gas masses from the total column density of observed lines. The dotted line represents the ratio $M/M_{\rm VIR}$ , expected to be $\propto$ r^-0.3across the source. The estimated errors are of the order of $\sim$ $30\%$ .
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{4099.f16.ps}\end{figure}$ Figure 16: H₂ volume density against the linear diameter D for all the tracers observed. All values have been taken from Table 4. The straight line is a linear fit to the data, which gives $n_{\rm {H_{2}}\propto D^{-2.3}}$ .
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.6cm,clip]{4099.f17.ps}\end{figure}$ Figure 17: Brightness temperature of the C¹⁷O (1-0) line computed assuming a source as described in the text, and a C¹⁷O relative abundance of $1.4 \times 10^{-8}$ . R represents the radial distance from the source center.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.5cm,clip]{4099.f18.ps}\end{figure}$ Figure 18: Brightness temperature of Fig. 17 convolved with the IRAM-30 m telescope beam (22 $^{\prime \prime }$ ).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=14cm,clip]{4099.f19.ps}\end{figure}$ Figure 19: Left panel: map of the C¹⁷O (1-0) line in the peak channel (at -50.5 km s^-1). The solid contour represents the observed 2 $\sigma$ level ( $\sim$ 0.024 Jy beam^-1), while the dashed contours indicate the emission of a "core-halo'' source model, as described in Fig. 17. Levels range from 0.024 to 0.14 by 0.024 Jy beam^-1. Right panel: same as left for a source model without the central core. Both contours represent the $2\sigma$ observed level.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{4099.f20.ps}\end{figure}$ Figure 20: Kinetic temperature measured at the surface of molecular cores plotted against the distance-independent ratio $L^{1/2}/\theta$ , where $\theta$ is the angular diameter of the core, and L the luminosity of the embedded (proto)star. Open circles indicate HCs (Kurtz et al. 2000) while the filled circle corresponds to I23385. The straight line represents the steepest power law for spherical cores, $T\propto (L^{1/2}/\theta d)^{0.5}$ , expected for a dusty core heated by an embedded star (Doty & Leung 1994).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{4099.f1.ps}\end{figure}$	Figure 1: C¹⁸O and C¹⁷O spectra towards the central position in the maps, which is the peak of the sub-mm emission (Molinari et al. 2000). The dashed line indicates the main component arising from the source. The dotted line with red-shifted velocity shows the second component. In the C¹⁷O (1-0), the vertical lines under the spectrum indicate the position of the hyperfine components.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{4099.f2.ps}\end{figure}$	Figure 2: From top to bottom: CH₃C₂H (6-5), (8-7) and (13-12) IRAM-30 m spectra towards the peak of the sub-mm emission (Molinari et al. 2000). The numbers under the spectra indicate the position of the different K components. The $V_{\rm LSR}$ is relative to the line with K=0.
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$\begin{figure} \par\includegraphics[angle=-90,width=7cm,clip]{4099.f4.ps}\end{figure}$	Figure 4: Same as Fig. 3 for the main component of the C¹⁷O (2-1) line, integrated between -52.5 and -49.0 km s^-1. Contour levels go from $\sim$ 1K km s^-1 ( $\sim$ $3\sigma$ level), to 3.3 K km s^-1 in steps of $1\sigma$ .
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$\begin{figure} \par\includegraphics[angle=-90,width=7cm,clip]{4099.f5.ps}\end{figure}$	Figure 5: SCUBA map of IRAS 23385+6053 at 850 $\mu$ m (grey scale). Levels range from 0.3 (3 $\sigma$ ) to 1.9 by 0.2 Jy beam^-1. The solid contours represent the C¹⁸O (1-0) map (main component) obtained with the IRAM-30 m telescope (Fig. 3), with the thick line corresponding to the contour at half maximum.
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$\begin{figure} \par\includegraphics[width=6cm,clip]{4099.f7.ps}\end{figure}$	Figure 7: Flux density comparison between IRAM single-dish (dashed line) spectra and Plateau-de-Bure interferometric spectra (solid line). The interferometric flux densities have been multiplied by a factor of 10 for the CO isotopomers, and by a factor of 3 for the CH₃C₂H lines. The velocity of the CH₃C₂H spectrum is computed with respect to the frequency of the line with K=0.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{4099.f10.ps}\end{figure}$	Figure 10: Flux density comparison between Effelsberg-100 m (dashed line) and VLA (solid line) spectra of the NH₃(1,1) and (2,2) lines. VLA fluxes have been multiplied by a factor of 2. The thick vertical lines under the NH₃(1,1) spectrum indicate the position of the two components. The Effelsberg spectra have been resampled to the channel spacing of the VLA spectra.
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$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{4099.f12.ps}\end{figure}$	Figure 12: Image of IRAS 23385+6053 at 15 $\mu$ m obtained with ISOCAM (Molinari et al. 1998b). The thick polygon represents the 3 $\sigma$ level of the HCO⁺ (1-0) line, and it identifies the core region. The dashed polygons indicate the two clusters of stars which lie around I23385, called "ring'' in the text.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{4099.f16.ps}\end{figure}$	Figure 16: H₂ volume density against the linear diameter D for all the tracers observed. All values have been taken from Table 4. The straight line is a linear fit to the data, which gives $n_{\rm {H_{2}}\propto D^{-2.3}}$ .
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$\begin{figure} \par\includegraphics[angle=-90,width=7.6cm,clip]{4099.f17.ps}\end{figure}$	Figure 17: Brightness temperature of the C¹⁷O (1-0) line computed assuming a source as described in the text, and a C¹⁷O relative abundance of $1.4 \times 10^{-8}$ . R represents the radial distance from the source center.
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$\begin{figure} \par\includegraphics[angle=-90,width=7.5cm,clip]{4099.f18.ps}\end{figure}$	Figure 18: Brightness temperature of Fig. 17 convolved with the IRAM-30 m telescope beam (22 $^{\prime \prime }$ ).
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