All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=18cm,clip]{2871f01.eps} \end{figure}$ Figure 1: Optical (DSS2-Red, left) and near-infrared (K', right) views of the Coronet cluster. T CrA, seen at left, is not covered by the radio data presented here. It is marginally detected in X-rays (Skinner et al. 2004). The K' image is from Hodapp (1994), coordinates are J2000.
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In the text

$\begin{figure} \par\includegraphics[width=12cm]{2871f02.eps} \end{figure}$ Figure 2: Upper panel: image made from the combined uv data of all five VLA observation epochs. Contours shown are 5, 10 and 100 $\sigma$ in the main plot and -3 (dashed), 3, 5, 50 and 100 $\sigma$ in the inset showing IRS 7. Coordinates are J2000.0. Lower panel: the same view, showing the merged Chandra ACIS-I data. The inset shows approximately the same view in the merged XMM- Newton data (MOS+EPN, X1-X3).
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{2871f03a.eps}\hspace*{3mm} \includegraphics[width=7.6cm,clip]{2871f03b.eps} \par\end{figure}$ Figure 3: Radio flux curves of sources identified in the 1998 VLA data. Error bars indicate the uncertainty estimates given by the AIPS task "sad'', they are based on actual noise ( $1\sigma$ ) rather than the quality of the fit. Filled triangles denote upper limits. Also shown is Stokes-V for IRS 5.
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In the text

$\begin{figure} \par\includegraphics*[width=7.5cm,clip]{2871f04.eps} \end{figure}$ Figure 4: IRS 5 epoch-averaged polarization degrees in percent. Errors are propagated from those shown in Fig. 3.
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In the text

$\begin{figure} \includegraphics[width=17cm]{2871f5.eps} \end{figure}$ Figure 5: X-ray spectra of IRS 2, 5 and 1 derived from the five X-ray datasets. The line shows the result of fitting an absorbed APEC model.
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In the text

$\begin{figure} \includegraphics[width=18cm]{2871f6.eps} \end{figure}$ Figure 6: Results of fitting XSWABS $\times$ XSAPEC, fit parameters $N_{\rm H}$ and kT. Abundances set to values determined from best spectra. Errorbars are 3 $\sigma$ . The X-ray datasets are numbered according to Table 2. The NIR-determined $N_{\rm H}$ column densities from Nisini et al. (2005) are $6 \times 10^{22}$ cm^-2 (IRS 1), $4 \times 10^{22}$ cm^-2 (IRS 2) and $9 \times 10^{22}$ cm^-2 (IRS 5).
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In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{2871f07.eps} \end{figure}$ Figure 7: Kilosecond-binned, background-subtracted X-ray luminosity curves in temporal order for the three class I protostars IRS 2,5, and 1. In the X2 and X3 observations, around 20% of the flux from IRS 1 is lost due to a chip gap in the source region.
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In the text

$\begin{figure} \par\includegraphics*[width=7.8cm,clip]{2871f08.eps} \end{figure}$ Figure 8: X-ray vs. radio luminosity of identified young stellar objects for which X-ray luminosities can be derived from spectra. The errorbars correspond to the standard deviation within the 1998 VLA and archival X-ray data, except for IRS 7E/W, where the X-ray luminosities are from Hamaguchi et al. (2005). For IRS 7E, the X-ray errorbars reflect the flare seen in X2/X3 while for IRS 7W, only a single luminosity was determined from the X2 data. The line shows the empirical relationship for active late-type stars from Benz & Guedel (1994).
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In the text

$\begin{figure} \par\includegraphics*[width=8cm,clip]{2871f09.eps} \par\end{figure}$ Figure 9: IRS 7E X-ray luminosity. Countrates for the five X-ray datasets were converted into luminosities without background subtraction, assuming a single-temperature spectrum of kT=3 keV and $N_{\rm H}=2.8 \times 10^{23}$ cm^-2 (Hamaguchi et al. 2005). The errorbars denote errors of 30%. Note that the source is only marginally detected in C1 and C2.
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In the text

$\begin{figure} \includegraphics[width=12cm]{2871f10.eps} \end{figure}$ Figure 10: R CrA spectra, taken from an ellipse region avoiding the neighbouring source IRS 9. The results of fitting an absorbed APEC model are shown. In the X3 fit, the column density was frozen to the values from X1 and X2.
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In the text

$\begin{figure} \par\includegraphics[width=15.7cm,clip]{2871f11.eps} \end{figure}$ Figure 11: R CrA X-ray luminosity curves from the same elliptical region also used for the spectra. Luminosity calculated assuming spectral properties of the best spectrum (X2). Data is kilosecond-binned and background-subtracted, datasets are in temporal order as labeled.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=18cm,clip]{2871f01.eps} \end{figure}$	Figure 1: Optical (DSS2-Red, left) and near-infrared (K', right) views of the Coronet cluster. T CrA, seen at left, is not covered by the radio data presented here. It is marginally detected in X-rays (Skinner et al. 2004). The K' image is from Hodapp (1994), coordinates are J2000.
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$\begin{figure} \par\includegraphics[width=7.4cm,clip]{2871f03a.eps}\hspace*{3mm} \includegraphics[width=7.6cm,clip]{2871f03b.eps} \par\end{figure}$	Figure 3: Radio flux curves of sources identified in the 1998 VLA data. Error bars indicate the uncertainty estimates given by the AIPS task "sad'', they are based on actual noise ( $1\sigma$ ) rather than the quality of the fit. Filled triangles denote upper limits. Also shown is Stokes-V for IRS 5.
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$\begin{figure} \par\includegraphics*[width=7.5cm,clip]{2871f04.eps} \end{figure}$	Figure 4: IRS 5 epoch-averaged polarization degrees in percent. Errors are propagated from those shown in Fig. 3.
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$\begin{figure} \includegraphics[width=17cm]{2871f5.eps} \end{figure}$	Figure 5: X-ray spectra of IRS 2, 5 and 1 derived from the five X-ray datasets. The line shows the result of fitting an absorbed APEC model.
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$\begin{figure} \par\includegraphics[width=16cm,clip]{2871f07.eps} \end{figure}$	Figure 7: Kilosecond-binned, background-subtracted X-ray luminosity curves in temporal order for the three class I protostars IRS 2,5, and 1. In the X2 and X3 observations, around 20% of the flux from IRS 1 is lost due to a chip gap in the source region.
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$\begin{figure} \par\includegraphics*[width=8cm,clip]{2871f09.eps} \par\end{figure}$	Figure 9: IRS 7E X-ray luminosity. Countrates for the five X-ray datasets were converted into luminosities without background subtraction, assuming a single-temperature spectrum of kT=3 keV and $N_{\rm H}=2.8 \times 10^{23}$ cm^-2 (Hamaguchi et al. 2005). The errorbars denote errors of 30%. Note that the source is only marginally detected in C1 and C2.
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$\begin{figure} \includegraphics[width=12cm]{2871f10.eps} \end{figure}$	Figure 10: R CrA spectra, taken from an ellipse region avoiding the neighbouring source IRS 9. The results of fitting an absorbed APEC model are shown. In the X3 fit, the column density was frozen to the values from X1 and X2.
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$\begin{figure} \par\includegraphics[width=15.7cm,clip]{2871f11.eps} \end{figure}$	Figure 11: R CrA X-ray luminosity curves from the same elliptical region also used for the spectra. Luminosity calculated assuming spectral properties of the best spectrum (X2). Data is kilosecond-binned and background-subtracted, datasets are in temporal order as labeled.
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