All Figures

$\begin{figure} \par\includegraphics[width=11cm,clip]{0755fig1.ps}\vspace*{4mm} \includegraphics[width=11cm,clip]{0755fig2.ps} % \end{figure}$ Figure 1: Galactic distribution of the sources in the survey. Top: longitude-latitude coverage. Bottom: longitude-velocity distribution.
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In the text

$\begin{figure} \par\includegraphics[width=2.5in,height=2.5in,clip]{0755fig3.eps}... ...4mm} \includegraphics[width=2.55in,height=2.55in,clip]{0755fig4.eps}\end{figure}$ Figure 2: SED of typical 1.2-mm/IRAS sources. Top: IRAS 15439-5449. Bottom: IRAS 17143-3700. The subscripts C and H refers to cold and hot components, respectively.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=2.5in,height=2.5in,clip]{0755fig... ...\includegraphics[width=2.5in,height=2.5in,clip]{0755f010.eps} } \par\end{figure}$ Figure 3: Distribution of parameters of 1.2-mm cores associated with high-mass star forming regions. Upper left: size distribution. The averageradius is $0.4 \pm 0.2$ pc. Upper right: temperature distribution. The average temperature is $32 \pm 5$ K. Middle left: mass distribution. Theaverage mass is $5.0 \times 10^{3}~M_{\odot}$ . Middle right: luminosity distribution.The average luminosity is $2.3 \times 10^5~L_\odot$ . Lower left: density distribution. The average density is $2.1 \times 10^{5}$ cm^-3. Lower right: distance distribution. The average distance is 4.4 kpc.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=2.5in,height=2.5in,clip]{0755f01... ...cm} \includegraphics[width=2.5in,height=2.5in,clip]{0755f012.eps} } \end{figure}$ Figure 4: Left: histogram of the distribution of the L/M ratio for the whole sample of cores. Right: luminosity-to-mass ratio of two subsamples. Dotted line: cores without radio detections; continuous line: cores associated with radio emission. The tail of low L/M in sources with no radio continuum detections is produced by contamination of low-mass cores with non-ionizing sources.
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In the text

$\begin{figure} \par\includegraphics[width=2.5in,height=2.5in,clip]{0755f013.eps}\end{figure}$ Figure 5: Histogram of the distribution of the number of sources per map.
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In the text

$\begin{figure} \par\includegraphics[width=2.5in,height=2.5in,clip]{0755f014.eps} \end{figure}$ Figure 6: Luminosity-to-mass ratio of the cores versus the luminosity of the most luminous star within the core. The equation of the straight line, fitted using a robust estimator, is $L_{\rm c}/M_{\rm c} = 0.75~(L_{\max})^{0.46}$ . The mean absolute deviation is 0.2.
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In the text

$\begin{figure} \par\mbox{\hspace{2.4cm} \tiny {08076-3556} \hspace{4.5cm} \tiny ... ...psfig{figure=0755f023.ps,height=1.5in,angle=-90} } \normalsize { } \end{figure}$ Figure 7: Maps of the 1.2 mm emission IRAS name is given on top of each figure. Contour levels are $-3\sigma$ , $3\sigma$ , $6\sigma$ , $12\sigma$ , $24\sigma$ , $48\sigma$ ... Unless stated otherwise, $\sigma = 40$ mJy for all sources.
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In the text

$\begin{figure} \par\mbox{\hspace{2cm} \tiny {11332-6258} \hspace{4.6cm} \tiny {1... ...ght=2.3in}\psfig{figure=0755f032.ps,height=2.3in} } \normalsize { } \end{figure}$ Figure 8: Same as fig. 6. IRAS 12326-6245: $\sigma = 200$ mJy, IRAS 12572-6316: $\sigma = 50$ mJy and IRAS 13079-6218: $\sigma = 60$ mJy.
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In the text

$\begin{figure} \par\mbox{\hspace{2.7cm} \tiny {13134-6242} \hspace{4.5cm} \tiny ... ...\psfig{figure=0755f041.ps,height=2.3in,angle=-90} } \normalsize { } \end{figure}$ Figure 9: Same as Fig. 6. IRAS 13295-6152: $\sigma = 60$ mJy.
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In the text

$\begin{figure} \par\mbox{\hspace{2.4cm} \tiny {14164-6028} \hspace{4.2cm} \tiny ... ...e=-90}\psfig{figure=0755f050.ps,height=2.1in} } \par\normalsize { } \end{figure}$ Figure 10: Same as Fig. 6.
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In the text

$\begin{figure} \par\mbox{\hspace{2.4cm} \tiny {15384-5348} \hspace{4.5cm} \tiny ... ...ght=2.7in}\psfig{figure=0755f059.ps,height=2.7in} } \normalsize { } \end{figure}$ Figure 11: Same as Fig. 6. IRAS 15384-5348: $\sigma = 90$ mJy, IRAS 15437-5343: $\sigma = 130$ mJy.
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In the text

$\begin{figure} \par\mbox{\hspace{2.4cm} \tiny {15557-5215} \hspace{4.5cm} \tiny ... ...angle=-90}\psfig{figure=0755f068.ps,height=2.5in} } \normalsize { } \end{figure}$ Figure 12: Same as Fig. 6. IRAS 16060-5146 and 16065-5158: $\sigma = 70$ mJy.
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In the text

$\begin{figure} \par\mbox{\hspace{2.2cm} \tiny {16071-5142} \hspace{4.0cm} \tiny ... ...angle=-90}\psfig{figure=0755f077.ps,height=2.3in} } \normalsize { } \end{figure}$ Figure 13: Same as Fig. 6. IRAS 16071-5142: $\sigma = 140$ mJy.
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In the text

$\begin{figure} \par\mbox{\hspace{2.2cm} \tiny {16297-4757} \hspace{4.0cm} \tiny ... ...ngle=-90}\psfig{figure=0755f086.ps,height=2.5in} } \normalsize { } \end{figure}$ Figure 14: Same as Fig. 6. IRAS 16304-4710: $\sigma = 60$ mJy, IRAS 16313-4729 and 16348-4654: $\sigma = 90$ mJy, IRAS 16330-4725: $\sigma = 170$ mJy, IRAS 16344-4658: $\sigma = 110$ mJy and IRAS 16362-4639: $\sigma = 70$ mJy.
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In the text

$\begin{figure} \par\mbox{\hspace{2.4cm} \tiny {16372-4545} \hspace{4.5cm} \tiny ... ...psfig{figure=0755f095.ps,height=2.5in,angle=-90} } \normalsize { } \end{figure}$ Figure 15: Same as Fig. 6. IRAS 16372-4545: $\sigma = 60$ mJy and IRAS 16484-4603: $\sigma = 120$ mJy.
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In the text

$\begin{figure} \par\mbox{\hspace{2.2cm} \tiny {16524-4300} \hspace{4.0cm} \tiny ... ...ht=2.5in}\psfig{figure=0755f104.ps,height=2.5in} } \normalsize { } \end{figure}$ Figure 16: Same than Fig. 6. IRAS 16562-3959 has $\sigma = 60$ mJy, IRAS 17008-4040 has $\sigma = 110$ mJy and IRAS 17016-4124 has $\sigma = 80$ mJy.
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In the text

$\begin{figure} \par\mbox{\hspace{2.4cm} \tiny {17158-3901} \hspace{5.5cm} \tiny ... ...angle=-90}\psfig{figure=0755f113.ps,height=2.3in} } \normalsize { } \end{figure}$ Figure 17: Same as Fig. 6 IRAS 17175-3544, 17220-3609 and 17258-3637: $\sigma = 90$ mJy.
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In the text

$\begin{figure} \par\mbox{\hspace{2.4cm} \tiny {17271-3439} \hspace{4.5cm} \tiny ... ...ght=2.3in}\psfig{figure=0755f122.ps,height=2.3in} } \normalsize { } \end{figure}$ Figure 18: Same as Fig. 6. IRAS 17439-2845, 17455-2800 and 17545-2357: $\sigma = 90$ mJy. IRAS 17441-2822: $\sigma = 300$ mJy.
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In the text

$\begin{figure} \par\mbox{\hspace{3.4cm} \tiny {18056-1952} \hspace{5.0cm} \tiny ... ...ght=2.5in}\psfig{figure=0755f131.ps,height=2.5in} } \normalsize { } \end{figure}$ Figure 19: Same as Fig. 6. IRAS 18075-2040: $\sigma = 25$ mJy.
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In the text

$\begin{figure} \par\mbox{\hspace{2.6cm} \tiny {18159-1648} \hspace{4.8cm} \tiny ... ...ig{figure=0755f140.ps,height=1.9in,angle=-90} } \par\normalsize { } \end{figure}$ Figure 20: Same as Fig. 6. IRAS 18290-0924: $\sigma = 20$ mJy and IRAS 18308-0503: $\sigma = 25$ mJy.
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In the text

$\begin{figure} \par\mbox{\hspace{2.7cm} \tiny {18314-0720} \hspace{5.0cm} \tiny ... ...psfig{figure=0755f149.ps,height=1.7in,angle=-90} } \normalsize { } \end{figure}$ Figure 21: Same as Fig. 6.
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In the text

$\begin{figure} \mbox{\hspace{2.6cm} \tiny {18461-0113} \hspace{5.5cm} \tiny {184... ...\psfig{figure=0755f158.ps,height=1.8in,angle=-90} } \normalsize { } \end{figure}$ Figure 22: Same as Fig. 6. IRAS 19078+0901: $\sigma = 70$ mJy.
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In the text

$\begin{figure} \mbox{\hspace{4.0cm} \tiny {19095+0930} \hspace{8.0cm} \tiny {190... ...ace{2cm} \psfig{figure=0755f160.ps,height=2.5in} } \normalsize { } \end{figure}$ Figure 23: Same as Fig. 6.
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In the text

$\begin{figure} \par\includegraphics[width=11cm,clip]{0755fig1.ps}\vspace*{4mm} \includegraphics[width=11cm,clip]{0755fig2.ps} % \end{figure}$	Figure 1: Galactic distribution of the sources in the survey. Top: longitude-latitude coverage. Bottom: longitude-velocity distribution.
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$\begin{figure} \par\includegraphics[width=2.5in,height=2.5in,clip]{0755fig3.eps}... ...4mm} \includegraphics[width=2.55in,height=2.55in,clip]{0755fig4.eps}\end{figure}$	Figure 2: SED of typical 1.2-mm/IRAS sources. Top: IRAS 15439-5449. Bottom: IRAS 17143-3700. The subscripts C and H refers to cold and hot components, respectively.
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$\begin{figure} \par\mbox{\includegraphics[width=2.5in,height=2.5in,clip]{0755f01... ...cm} \includegraphics[width=2.5in,height=2.5in,clip]{0755f012.eps} } \end{figure}$	Figure 4: Left: histogram of the distribution of the L/M ratio for the whole sample of cores. Right: luminosity-to-mass ratio of two subsamples. Dotted line: cores without radio detections; continuous line: cores associated with radio emission. The tail of low L/M in sources with no radio continuum detections is produced by contamination of low-mass cores with non-ionizing sources.
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$\begin{figure} \par\includegraphics[width=2.5in,height=2.5in,clip]{0755f013.eps}\end{figure}$	Figure 5: Histogram of the distribution of the number of sources per map.
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$\begin{figure} \par\includegraphics[width=2.5in,height=2.5in,clip]{0755f014.eps} \end{figure}$	Figure 6: Luminosity-to-mass ratio of the cores versus the luminosity of the most luminous star within the core. The equation of the straight line, fitted using a robust estimator, is $L_{\rm c}/M_{\rm c} = 0.75~(L_{\max})^{0.46}$ . The mean absolute deviation is 0.2.
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$\begin{figure} \par\mbox{\hspace{2.4cm} \tiny {08076-3556} \hspace{4.5cm} \tiny ... ...psfig{figure=0755f023.ps,height=1.5in,angle=-90} } \normalsize { } \end{figure}$	Figure 7: Maps of the 1.2 mm emission IRAS name is given on top of each figure. Contour levels are $-3\sigma$ , $3\sigma$ , $6\sigma$ , $12\sigma$ , $24\sigma$ , $48\sigma$ ... Unless stated otherwise, $\sigma = 40$ mJy for all sources.
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$\begin{figure} \par\mbox{\hspace{2cm} \tiny {11332-6258} \hspace{4.6cm} \tiny {1... ...ght=2.3in}\psfig{figure=0755f032.ps,height=2.3in} } \normalsize { } \end{figure}$	Figure 8: Same as fig. 6. IRAS 12326-6245: $\sigma = 200$ mJy, IRAS 12572-6316: $\sigma = 50$ mJy and IRAS 13079-6218: $\sigma = 60$ mJy.
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$\begin{figure} \par\mbox{\hspace{2.7cm} \tiny {13134-6242} \hspace{4.5cm} \tiny ... ...\psfig{figure=0755f041.ps,height=2.3in,angle=-90} } \normalsize { } \end{figure}$	Figure 9: Same as Fig. 6. IRAS 13295-6152: $\sigma = 60$ mJy.
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$\begin{figure} \par\mbox{\hspace{2.4cm} \tiny {14164-6028} \hspace{4.2cm} \tiny ... ...e=-90}\psfig{figure=0755f050.ps,height=2.1in} } \par\normalsize { } \end{figure}$	Figure 10: Same as Fig. 6.
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$\begin{figure} \par\mbox{\hspace{2.4cm} \tiny {15384-5348} \hspace{4.5cm} \tiny ... ...ght=2.7in}\psfig{figure=0755f059.ps,height=2.7in} } \normalsize { } \end{figure}$	Figure 11: Same as Fig. 6. IRAS 15384-5348: $\sigma = 90$ mJy, IRAS 15437-5343: $\sigma = 130$ mJy.
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$\begin{figure} \par\mbox{\hspace{2.4cm} \tiny {15557-5215} \hspace{4.5cm} \tiny ... ...angle=-90}\psfig{figure=0755f068.ps,height=2.5in} } \normalsize { } \end{figure}$	Figure 12: Same as Fig. 6. IRAS 16060-5146 and 16065-5158: $\sigma = 70$ mJy.
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$\begin{figure} \par\mbox{\hspace{2.2cm} \tiny {16071-5142} \hspace{4.0cm} \tiny ... ...angle=-90}\psfig{figure=0755f077.ps,height=2.3in} } \normalsize { } \end{figure}$	Figure 13: Same as Fig. 6. IRAS 16071-5142: $\sigma = 140$ mJy.
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$\begin{figure} \par\mbox{\hspace{2.2cm} \tiny {16297-4757} \hspace{4.0cm} \tiny ... ...ngle=-90}\psfig{figure=0755f086.ps,height=2.5in} } \normalsize { } \end{figure}$	Figure 14: Same as Fig. 6. IRAS 16304-4710: $\sigma = 60$ mJy, IRAS 16313-4729 and 16348-4654: $\sigma = 90$ mJy, IRAS 16330-4725: $\sigma = 170$ mJy, IRAS 16344-4658: $\sigma = 110$ mJy and IRAS 16362-4639: $\sigma = 70$ mJy.
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$\begin{figure} \par\mbox{\hspace{2.4cm} \tiny {16372-4545} \hspace{4.5cm} \tiny ... ...psfig{figure=0755f095.ps,height=2.5in,angle=-90} } \normalsize { } \end{figure}$	Figure 15: Same as Fig. 6. IRAS 16372-4545: $\sigma = 60$ mJy and IRAS 16484-4603: $\sigma = 120$ mJy.
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$\begin{figure} \par\mbox{\hspace{2.2cm} \tiny {16524-4300} \hspace{4.0cm} \tiny ... ...ht=2.5in}\psfig{figure=0755f104.ps,height=2.5in} } \normalsize { } \end{figure}$	Figure 16: Same than Fig. 6. IRAS 16562-3959 has $\sigma = 60$ mJy, IRAS 17008-4040 has $\sigma = 110$ mJy and IRAS 17016-4124 has $\sigma = 80$ mJy.
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$\begin{figure} \par\mbox{\hspace{2.4cm} \tiny {17158-3901} \hspace{5.5cm} \tiny ... ...angle=-90}\psfig{figure=0755f113.ps,height=2.3in} } \normalsize { } \end{figure}$	Figure 17: Same as Fig. 6 IRAS 17175-3544, 17220-3609 and 17258-3637: $\sigma = 90$ mJy.
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$\begin{figure} \par\mbox{\hspace{2.4cm} \tiny {17271-3439} \hspace{4.5cm} \tiny ... ...ght=2.3in}\psfig{figure=0755f122.ps,height=2.3in} } \normalsize { } \end{figure}$	Figure 18: Same as Fig. 6. IRAS 17439-2845, 17455-2800 and 17545-2357: $\sigma = 90$ mJy. IRAS 17441-2822: $\sigma = 300$ mJy.
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$\begin{figure} \par\mbox{\hspace{3.4cm} \tiny {18056-1952} \hspace{5.0cm} \tiny ... ...ght=2.5in}\psfig{figure=0755f131.ps,height=2.5in} } \normalsize { } \end{figure}$	Figure 19: Same as Fig. 6. IRAS 18075-2040: $\sigma = 25$ mJy.
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$\begin{figure} \par\mbox{\hspace{2.6cm} \tiny {18159-1648} \hspace{4.8cm} \tiny ... ...ig{figure=0755f140.ps,height=1.9in,angle=-90} } \par\normalsize { } \end{figure}$	Figure 20: Same as Fig. 6. IRAS 18290-0924: $\sigma = 20$ mJy and IRAS 18308-0503: $\sigma = 25$ mJy.
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$\begin{figure} \par\mbox{\hspace{2.7cm} \tiny {18314-0720} \hspace{5.0cm} \tiny ... ...psfig{figure=0755f149.ps,height=1.7in,angle=-90} } \normalsize { } \end{figure}$	Figure 21: Same as Fig. 6.
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$\begin{figure} \mbox{\hspace{2.6cm} \tiny {18461-0113} \hspace{5.5cm} \tiny {184... ...\psfig{figure=0755f158.ps,height=1.8in,angle=-90} } \normalsize { } \end{figure}$	Figure 22: Same as Fig. 6. IRAS 19078+0901: $\sigma = 70$ mJy.
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$\begin{figure} \mbox{\hspace{4.0cm} \tiny {19095+0930} \hspace{8.0cm} \tiny {190... ...ace{2cm} \psfig{figure=0755f160.ps,height=2.5in} } \normalsize { } \end{figure}$	Figure 23: Same as Fig. 6.
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