Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=8.8cm]{9949fg1a.ps} \includegraphics... ...th=8.8cm]{9949fg1b.ps} \includegraphics[width=8.8cm]{9949fg1c.ps} \end{figure}$ Figure 1: Distribution of IR sources with uncertainty ${\rm rms} < 0.1~$ mag towards the R Cr A cloud. The 1.2 mm contours from the SIMBA map are superimposed. The fields are labelled (NW, A, A3, B, D, C). R Cr A in the overlap of fields A and A3 is marked with a diamond.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{9949fg2.ps} \end{figure}$ Figure 2: Surface density of sources with ${\rm rms} < 0.2~$ mag as a function of wavelength and the SIMBA 1.2 mm emission towards these sources. For J and H, only five fields are considered, while $K_{\rm s}$ refers to all six fields including field A.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{9949fg3.ps} \end{figure}$ Figure 3: 1.2 mm surface brightness versus $H-K_{\rm s}$ . Sources above the solid line S_1.2 = 25 MJy/sr are considered to be probable members, and sources above the long-dashed line S_1.2 = 8 MJy/sr are called possible members. The thick solid line indicates A_V adopting standard dust properties; it is not a fit to the median data points (red squares).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{9949fg4.ps} \end{figure}$ Figure 4: Sky position of the probable members and the possible NW cloud members. All probable members are located towards the Coronet around R CrA (filled diamond). Some sources lie near saturated areas or spikes in our $K_{\rm s}$ -image, and their photometry was taken from Wilking et al. (1997). The possible members are located towards the core of the NW dust ridge, north and west of S CrA (filled diamond). The subdivision of stars into group-1/-2 has been derived from the colour-magnitude diagram (Fig. 7). The dotted triangle encircles the stars in the NW off-core region used for comparisons.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{9949fg5.ps} \end{figure}$ Figure 5: Colour-magnitude diagram of the probable members, i.e. projected mm-excess sources with S_1.2 > 25 MJy/sr.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{9949fg6.ps} \end{figure}$ Figure 6: $K_{\rm s}$ brightness versus S_1.2: plotted are sources of field A having only $K_{\rm s}$ photometry. They are compared with sources detected in both H and $K_{\rm s}$ in any of our fields, which are located towards S_1.2> 25 MJy/sr or have red $H-K_{\rm s} > 1.5$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{9949fg7.ps} \end{figure}$ Figure 7: Colour-magnitude diagram of the NW-core and NW-off-core. Group-1/-2 sources are defined to lie above/below the $A_{\rm V}$ line. The main sequence shifted to the distance of R CrA is plotted only for illustrative purposes.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{9949fg8.ps} \end{figure}$ Figure 8: Sky position of the possible members towards MMS 25 in field C. The dotted triangle encircles the stars in the C off-core region used for comparions. The off-field contains 12 group-1 and 55 group-2 stars.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{9949fg9a.ps} \includegraphics[width=8.8cm]{9949fg9b.ps} \end{figure}$ Figure 9: Colour-colour and colour-magnitude diagrams showing the K-band excess candidates. The statistical significance for a K-band excess is low because of the large 1 $\sigma$ error bars in the colour-colour diagram. In the colour-magnitude diagram the K-band excess candidates lie at the faint end of our sources.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{9949f10a.ps} \includegraphics[width=8.8cm]{9949f10b.ps} \end{figure}$ Figure 10: $K_{\rm s}$ -band image and SED of the X-shaped Isabelle Nebula. The lines and symbols in the SED plot mean: filled circles connected by the solid line mark our NIR data together with Spitzer and ISOCAM MIR data; the filled diamonds connected with a long-dashed line mark IRAS data; SCUBA 450 + 850 $\mu$ m and SIMBA 1.2 mm photometry is plotted with filled diamonds; the dotted line represents a modified blackbody with emissivity index $\beta = 1$ and temperature T = 30 K.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{9949fg11.ps} \end{figure}$ Figure 11: Sky positions of the resolved nebulae.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{9949fg12.ps} \end{figure}$ Figure 12: $K_{\rm s}$ -band image of HH 99 with its bow-shock arrow cap. The black and white lines point to its driving star candidates R CrA and IRS 9 (marked with a ``+'' sign, right of R CrA), respectively. Because the bright stars are saturated in our frames, the position of the sources has been taken from Wilking et al. (1997) and Taylor & Storey (1984). The positional uncertainty is about the size of the ``+'' sign.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{9949fg1a.ps} \includegraphics... ...th=8.8cm]{9949fg1b.ps} \includegraphics[width=8.8cm]{9949fg1c.ps} \end{figure}$	Figure 1: Distribution of IR sources with uncertainty ${\rm rms} < 0.1~$ mag towards the R Cr A cloud. The 1.2 mm contours from the SIMBA map are superimposed. The fields are labelled (NW, A, A3, B, D, C). R Cr A in the overlap of fields A and A3 is marked with a diamond.
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$\begin{figure} \par\includegraphics[width=8.8cm]{9949fg2.ps} \end{figure}$	Figure 2: Surface density of sources with ${\rm rms} < 0.2~$ mag as a function of wavelength and the SIMBA 1.2 mm emission towards these sources. For J and H, only five fields are considered, while $K_{\rm s}$ refers to all six fields including field A.
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$\begin{figure} \par\includegraphics[width=8.8cm]{9949fg3.ps} \end{figure}$	Figure 3: 1.2 mm surface brightness versus $H-K_{\rm s}$ . Sources above the solid line S_1.2 = 25 MJy/sr are considered to be probable members, and sources above the long-dashed line S_1.2 = 8 MJy/sr are called possible members. The thick solid line indicates A_V adopting standard dust properties; it is not a fit to the median data points (red squares).
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$\begin{figure} \par\includegraphics[width=8.8cm]{9949fg5.ps} \end{figure}$	Figure 5: Colour-magnitude diagram of the probable members, i.e. projected mm-excess sources with S_1.2 > 25 MJy/sr.
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$\begin{figure} \par\includegraphics[width=8.8cm]{9949fg6.ps} \end{figure}$	Figure 6: $K_{\rm s}$ brightness versus S_1.2: plotted are sources of field A having only $K_{\rm s}$ photometry. They are compared with sources detected in both H and $K_{\rm s}$ in any of our fields, which are located towards S_1.2> 25 MJy/sr or have red $H-K_{\rm s} > 1.5$ .
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$\begin{figure} \par\includegraphics[width=8.8cm]{9949fg7.ps} \end{figure}$	Figure 7: Colour-magnitude diagram of the NW-core and NW-off-core. Group-1/-2 sources are defined to lie above/below the $A_{\rm V}$ line. The main sequence shifted to the distance of R CrA is plotted only for illustrative purposes.
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$\begin{figure} \par\includegraphics[width=8.8cm]{9949fg8.ps} \end{figure}$	Figure 8: Sky position of the possible members towards MMS 25 in field C. The dotted triangle encircles the stars in the C off-core region used for comparions. The off-field contains 12 group-1 and 55 group-2 stars.
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$\begin{figure} \par\includegraphics[width=8.8cm]{9949fg9a.ps} \includegraphics[width=8.8cm]{9949fg9b.ps} \end{figure}$	Figure 9: Colour-colour and colour-magnitude diagrams showing the K-band excess candidates. The statistical significance for a K-band excess is low because of the large 1 $\sigma$ error bars in the colour-colour diagram. In the colour-magnitude diagram the K-band excess candidates lie at the faint end of our sources.
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$\begin{figure} \par\includegraphics[width=8.8cm]{9949fg11.ps} \end{figure}$	Figure 11: Sky positions of the resolved nebulae.
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