All Figures

$\begin{figure} \par\includegraphics[width=16.25cm,clip]{6255fig1.eps}\end{figure}$ Figure 1: ATCA images of the $\lambda = 3.3$ -mm continuum emission (contours), overplotted on 2MASS K-band (2.1 $\mu$ m) images (grayscales). Contour levels are drawn at 2, 4, 6, 10, 15, and 20 times the noise level; negative contours are dashed. The positional offsets are with respect to the fitted coordinates (see Table 3).
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In the text

$\begin{figure} \par\hbox{\hspace{-0.5cm}\psfig{figure=6255fig2.eps,width=7.5cm} ... ...5fi11.eps,width=7.5cm} \put(-75,130){{\bf HK Lup}} \hspace{5.6cm}} \end{figure}$ Figure 2: Amplitude vs. (u, v) distance for sources observed with the ATCA. The data points give the vector-averaged amplitude per bin, where the data are binned in annuli according to (u, v) distance. The error bars show the statistical $1\sigma$ errors, and the dotted lines give the expected amplitude for zero signal.
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In the text

$\begin{figure} \par\hspace{0cm} \hbox{\hspace{-0.6cm}\psfig{figure=6255fi12.eps,... ...255fi16.eps,width=7.5cm}\put(-75,130){{\bf HK Lup}} \hspace{5.6cm}} \end{figure}$ Figure 3: Same as Fig. 2 for sources observed with the SMA.
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{6255fi17.eps}\end{figure}$ Figure 4: $F_\nu$ vs. $\nu$ for RU Lup. Filled symbols show fluxes from single-dish observations (JCMT and SEST, Nürnberger et al. 1997; Weintraub et al. 1989), open symbols show the values for the interferometric observations from this work. All points fall on a line with $\alpha = 2.5$ $\pm$ 0.1, where $F_\nu \propto \nu ^\alpha$ . This suggests that there is no extended emission over the size scale of the primary beams of the different telescopes, as may be the result of, e.g., a remnant envelope or ambient cloud material. Hence, no extended emission is filtered out in the interferometric observations.
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{6255fi18.eps}\end{figure}$ Figure 5: Cumulative number of sources with an opacity index less than a given value of $\beta$ for the sources in our sample (solid line), those studied by Rodmann et al. (2006) (dashed line), and those studied by Natta et al. (2004) (dotted line).
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In the text

$\begin{figure} \par\includegraphics[width=7.15cm,clip]{6255fi19.eps}\end{figure}$ Figure 6: Spectrum of HCO⁺ J = 1-0 line emission observed from IM Lup, at the position of the peak continuum emission, binned to 0.44 km s^-1 velocity resolution, in the $2\hbox{$.\!\!^{\prime\prime}$ }3$ $\times$ $1\hbox{$.\!\!^{\prime\prime}$ }7$ synthesized beam.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{6255fi20.eps}\end{figure}$ Figure 7: Slope in the millimetre regime vs. the peak 10- $\mu$ m flux ( upper panel) and the ratio of the 11.3 to 9.8 $\mu$ m flux ( lower panel) of the 10- $\mu$ m silicate feature, for those sources in our sample for which data are available. 1 = HT Lup, 2 = GW Lup, 3 = IM Lup, 4 = RU Lup, 5 = CR Cha, 6 = WW Cha, 7 = Glass I. The source T Cha is depicted with a diamond.
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In the text

$\begin{figure} \par\includegraphics[width=16.25cm,clip]{6255fig1.eps}\end{figure}$	Figure 1: ATCA images of the $\lambda = 3.3$ -mm continuum emission (contours), overplotted on 2MASS K-band (2.1 $\mu$ m) images (grayscales). Contour levels are drawn at 2, 4, 6, 10, 15, and 20 times the noise level; negative contours are dashed. The positional offsets are with respect to the fitted coordinates (see Table 3).
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$\begin{figure} \par\hbox{\hspace{-0.5cm}\psfig{figure=6255fig2.eps,width=7.5cm} ... ...5fi11.eps,width=7.5cm} \put(-75,130){{\bf HK Lup}} \hspace{5.6cm}} \end{figure}$	Figure 2: Amplitude vs. (u, v) distance for sources observed with the ATCA. The data points give the vector-averaged amplitude per bin, where the data are binned in annuli according to (u, v) distance. The error bars show the statistical $1\sigma$ errors, and the dotted lines give the expected amplitude for zero signal.
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$\begin{figure} \par\hspace{0cm} \hbox{\hspace{-0.6cm}\psfig{figure=6255fi12.eps,... ...255fi16.eps,width=7.5cm}\put(-75,130){{\bf HK Lup}} \hspace{5.6cm}} \end{figure}$	Figure 3: Same as Fig. 2 for sources observed with the SMA.
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$\begin{figure} \par\includegraphics[width=7.3cm,clip]{6255fi18.eps}\end{figure}$	Figure 5: Cumulative number of sources with an opacity index less than a given value of $\beta$ for the sources in our sample (solid line), those studied by Rodmann et al. (2006) (dashed line), and those studied by Natta et al. (2004) (dotted line).
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$\begin{figure} \par\includegraphics[width=7.15cm,clip]{6255fi19.eps}\end{figure}$	Figure 6: Spectrum of HCO⁺ J = 1-0 line emission observed from IM Lup, at the position of the peak continuum emission, binned to 0.44 km s^-1 velocity resolution, in the $2\hbox{$.\!\!^{\prime\prime}$ }3$ $\times$ $1\hbox{$.\!\!^{\prime\prime}$ }7$ synthesized beam.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{6255fi20.eps}\end{figure}$	Figure 7: Slope in the millimetre regime vs. the peak 10- $\mu$ m flux ( upper panel) and the ratio of the 11.3 to 9.8 $\mu$ m flux ( lower panel) of the 10- $\mu$ m silicate feature, for those sources in our sample for which data are available. 1 = HT Lup, 2 = GW Lup, 3 = IM Lup, 4 = RU Lup, 5 = CR Cha, 6 = WW Cha, 7 = Glass I. The source T Cha is depicted with a diamond.
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