All Figures

$\begin{figure} \includegraphics[width=12cm]{6158f01.eps} \end{figure}$ Figure 1: Plot of the Coronet region covered in this multi-wavelength dataset. The background image shows the combined X-ray data, the big circle indicates the half-power beam width of the VLA primary beam. The outer two boxes mark the coverage of the SMARTS- UBVRI and SIRIUS- $JHK_{\rm S}$ data (thick line). The two small boxes show the fields of view of the SofI observations. The central Coronet cluster is shown in detail in Fig. 3. Three 2MASS sources discussed in the text are marked as small circles: a) 2MASS J19014041-3651422 b) 2MASS J19013385-3657448 c) 2MASS J19012872-3659317
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{6158f02.eps}\end{figure}$ Figure 2: Graphical depiction of the observing times at the different observatories indicated on the lefthand side.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.4cm,clip]{6158f03.eps}\end{figure}$ Figure 3: Combined Chandra data (Obs ID 5402-5406, smoothed). The circle denotes the approximate VLA half-power primary beam.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{6158f04.eps} \end{figure}$ Figure 4: Exemplary VLA radio flux density curves for the three class I protostars IRS 1, 2, and 5, as well as for R CrA. Flux densities were derived by fitting Gaussians with the AIPS task SAD. The error bars mainly take into account actual noise (1 $\sigma$ ) rather than the quality of the fit.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.4cm,clip]{6158f05.eps}\end{figure}$ Figure 5: The double source IRS 5 (marginally resolved here) and its neighbouring source IRS 5N seen in $K_{\rm S}$ (SofI/NTT) on August 9, 2005.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{6158f06.eps}\end{figure}$ Figure 6: Top panel: Chandra X-ray light curves of IRS 5 for the five observations S1-S5, bin size is 1 ks. Center and bottom panel: $K_{\rm S}$ -band differential photometry of IRS 5 taken with SIRIUS and SofI, respectively. If anything, the $K_{\rm S}$ -band flux appears to slightly decrease around the enhanced X-ray activity of IRS 5. Error bars are $1\sigma$ .
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In the text

$\begin{figure} \mbox{\hspace*{5cm}a) IRS~1\hspace*{5.5cm}} \includegraphics*[wi... ...4cm}} \includegraphics*[width=12cm,bb=20 480 540 700]{6158f07d.eps}\end{figure}$ Figure 7: Chandra X-ray light curves for YSOs with near-simultaneous IRSF J-band data in the respective lower panels (with 1 $\sigma$ error bars).
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In the text

$\begin{figure*} \mbox{\hspace*{5cm}a) R CrA\hspace*{5.4cm}} \includegraphics*[w... ...cm}} \includegraphics*[width=12cm,bb=20 470 540 700]{6158f08d.eps}\end{figure*}$ Figure 8: Chandra X-ray light curves for YSOs with simultaneous CTIO I-band data in the respective lower panels (with 1 $\sigma$ error bars). The I-band light curve for S CrA results from a special analysis involving Gaussian fitting to its two components NW and SE (see Fig. 9 and text). Figure continues on next page.
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In the text

$\begin{figure} \mbox{\hspace*{3.9cm}e) 2MASS~J19012872-3659317\hspace*{4.2cm}} \includegraphics*[width=12cm,bb=20 470 540 700]{6158f08e.eps} \end{figure}$ Figure 8: continued.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{6158f09.eps}\end{figure}$ Figure 9: Upper panel: the total I-band magnitude of S CrA, determined as described in the text. The dashed horizontal line is the historical mean in the Van Vleck Observatory data base, used as the zero point here. Lower panel: the magnitude difference between the two components of S CrA. The dashed horizontal line is the median difference.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{6158f10.eps}\end{figure}$ Figure 10: Detail of the X-ray and I-band light curves shown in Fig. 8. The optical flare seen in the NW component does not appear to directly correspond to the maximum in the X-ray light curve.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{6158f11.eps}\end{figure}$ Figure 11: CTIO-I light curves for T CrA ( upper panel) and HBC 680 ( lower panel). While the former source is barely detected in X-rays, the latter remains undetected. Error bars are $1\sigma$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{6158f02.eps}\end{figure}$	Figure 2: Graphical depiction of the observing times at the different observatories indicated on the lefthand side.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.4cm,clip]{6158f03.eps}\end{figure}$	Figure 3: Combined Chandra data (Obs ID 5402-5406, smoothed). The circle denotes the approximate VLA half-power primary beam.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{6158f04.eps} \end{figure}$	Figure 4: Exemplary VLA radio flux density curves for the three class I protostars IRS 1, 2, and 5, as well as for R CrA. Flux densities were derived by fitting Gaussians with the AIPS task SAD. The error bars mainly take into account actual noise (1 $\sigma$ ) rather than the quality of the fit.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.4cm,clip]{6158f05.eps}\end{figure}$	Figure 5: The double source IRS 5 (marginally resolved here) and its neighbouring source IRS 5N seen in $K_{\rm S}$ (SofI/NTT) on August 9, 2005.
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$\begin{figure} \par\includegraphics[width=12cm,clip]{6158f06.eps}\end{figure}$	Figure 6: Top panel: Chandra X-ray light curves of IRS 5 for the five observations S1-S5, bin size is 1 ks. Center and bottom panel: $K_{\rm S}$ -band differential photometry of IRS 5 taken with SIRIUS and SofI, respectively. If anything, the $K_{\rm S}$ -band flux appears to slightly decrease around the enhanced X-ray activity of IRS 5. Error bars are $1\sigma$ .
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$\begin{figure} \mbox{\hspace{5cm}a) IRS~1\hspace{5.5cm}} \includegraphics[wi... ...4cm}} \includegraphics[width=12cm,bb=20 480 540 700]{6158f07d.eps}\end{figure}$	Figure 7: Chandra X-ray light curves for YSOs with near-simultaneous IRSF J-band data in the respective lower panels (with 1 $\sigma$ error bars).
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$\begin{figure} \mbox{\hspace{5cm}a) R CrA\hspace{5.4cm}} \includegraphics[w... ...cm}} \includegraphics[width=12cm,bb=20 470 540 700]{6158f08d.eps}\end{figure}$	Figure 8: Chandra X-ray light curves for YSOs with simultaneous CTIO I-band data in the respective lower panels (with 1 $\sigma$ error bars). The I-band light curve for S CrA results from a special analysis involving Gaussian fitting to its two components NW and SE (see Fig. 9 and text). Figure continues on next page.
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$\begin{figure} \mbox{\hspace{3.9cm}e) 2MASS~J19012872-3659317\hspace{4.2cm}} \includegraphics*[width=12cm,bb=20 470 540 700]{6158f08e.eps} \end{figure}$	Figure 8: continued.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{6158f09.eps}\end{figure}$	Figure 9: Upper panel: the total I-band magnitude of S CrA, determined as described in the text. The dashed horizontal line is the historical mean in the Van Vleck Observatory data base, used as the zero point here. Lower panel: the magnitude difference between the two components of S CrA. The dashed horizontal line is the median difference.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{6158f10.eps}\end{figure}$	Figure 10: Detail of the X-ray and I-band light curves shown in Fig. 8. The optical flare seen in the NW component does not appear to directly correspond to the maximum in the X-ray light curve.
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$\begin{figure} \par\includegraphics[width=12cm,clip]{6158f11.eps}\end{figure}$	Figure 11: CTIO-I light curves for T CrA ( upper panel) and HBC 680 ( lower panel). While the former source is barely detected in X-rays, the latter remains undetected. Error bars are $1\sigma$ .
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