All Figures

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{6320fig1.eps}\end{figure}$ Figure 1: Example of an OM image. This rich field (XEST-11, toward FS Tau) shows artefacts, such as the "ring'' of emission at the center (due to the reflection of diffuse sky light from outside the FOV), fixed pattern noise around the bright source XEST-11-OM-133 (HD 283579, which is not classified as a TMC member), and a ghost ring below source XEST-11-OM-147 which is also caused by XEST-11-OM-133. Other artefacts can be seen (trail along the bright source, defects on the detector).
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{6320fig2.eps}\end{figure}$ Figure 2: X-ray luminosity ( $L_{\rm X}$ ) in 10³⁰ erg s^-1 as a function of the observed OM magnitude. Various types of stars are identified (see text). Ultraviolet magnitudes are identified with filled symbols.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{6320fig3.eps}\end{figure}$ Figure 3: Cumulative distributions of X-ray count rates of type 2 and 3 stars.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{6320fig4.eps}\end{figure}$ Figure 4: Histogram of OM U magnitudes for type 2 and 3 stars.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{6320fig5.eps}\end{figure}$ Figure 5: Cumulative distributions of stellar luminosity of type 2 and 3 objects detected in the U filter.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{6320fig6.eps}\end{figure}$ Figure 6: Cumulative distributions of U-band OM magnitudes after correction for extinction. Type 2 stars have brighter OM magnitudes than type 3 stars. Stars with known $T_{\rm eff}$ and A_J are shown.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{6320fig7a.eps}\includegraphics[width=8cm,clip]{6320fig7b.eps}\end{figure}$ Figure 7: Normalized distributions of U-band excesses for type 2 and 3 stars. Excesses determined when A_J was used to calculate A_U are shown in the left figure, whereas excesses determined with A_V used are shown in the right figure.
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In the text

$\begin{figure} \par\includegraphics[width=16.5cm,clip]{6320fig8.eps}\end{figure}$ Figure 8: The TMC sample of stars with OM FAST mode data. The upper curve in each panel is the OM light curve ( right y-axis), whereas the lower curve is the X-ray light curve ( left y-axis). The OM light curves were rebinned to bin sizes of 200 s, except for CIDA 7, which required a bin size of 400 s. The type of the source is given together with the source name. The OM FAST data of IT Tau and UZ Tau EW are not shown since the sources were not properly placed on the small OM FAST window, and thus the light curves were unreliable. In addition, the T Tau OM FAST light curve is the subject of a separate paper and will be presented elsewhere (Güdel et al. 2007c). Note that small manual corrections were necessary for DN Tau, DI Tau AB, and BP Tau (see footnote 5).
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{6320fig9.eps}\end{figure}$ Figure 9: Details of the GK Tau OM and X-ray light curves. The OM light curve (top curve) was rebinned to a bin size of 200 s, while the X-ray light curve (bottom histogram) used a 400 s bin size. The thick dashed line corresponds to the OM light curve convolved through a kernel $K(t,t^\prime )$ (see text) but it was shifted down for clarity. The GK Tau A event shows evidence of a Neupert-like effect.
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In the text

$\begin{figure}\par\resizebox{.88\textwidth}{!}{\includegraphics{6320apBf1.eps}}\par\resizebox{.88\textwidth}{!}{\includegraphics{6320apBf2.eps}}\end{figure}$ Figure B.1: Light curves.

In the text

$\begin{figure}\par\resizebox{.9\textwidth}{!}{\includegraphics{6320apBf3.eps}}\par\resizebox{.9\textwidth}{!}{\includegraphics{6320apBf4.eps}} \end{figure}$ Figure B.1: continued.

In the text

$\begin{figure}\par\resizebox{.9\textwidth}{!}{\includegraphics{6320apBf5.eps}}\par\resizebox{.9\textwidth}{!}{\includegraphics{6320apBf6.eps}} \end{figure}$ Figure B.1: continued.

In the text

$\begin{figure}\par\resizebox{.9\textwidth}{!}{\includegraphics{6320apBf7.eps}}\par\resizebox{.9\textwidth}{!}{\includegraphics{6320apBf8.eps}} \end{figure}$ Figure B.1: continued.

In the text

$\begin{figure}\par\resizebox{.9\textwidth}{!}{\includegraphics{6320apBf9.eps}}\par\resizebox{.9\textwidth}{!}{\includegraphics{6320apBf10.eps}} \end{figure}$ Figure B.1: continued.

In the text

$\begin{figure}\par\resizebox{.9\textwidth}{!}{\includegraphics{6320apBf11.eps}}\par\resizebox{.9\textwidth}{!}{\includegraphics{6320apBf12.eps}} \end{figure}$ Figure B.1: continued.

In the text

$\begin{figure}\par\resizebox{.9\textwidth}{!}{\includegraphics{6320apBf13.eps}}\par\resizebox{.9\textwidth}{!}{\includegraphics{6320apBf14.eps}} \end{figure}$ Figure B.1: continued.

In the text

$\begin{figure}\par\resizebox{.9\textwidth}{!}{\includegraphics{6320apBf15.eps}}\par\resizebox{.9\textwidth}{!}{\includegraphics{6320apBf16.eps}} \end{figure}$ Figure B.1: continued.

In the text

$\begin{figure}\par\resizebox{.9\textwidth}{!}{\includegraphics{6320apBf17.eps}}\par\resizebox{.9\textwidth}{!}{\includegraphics{6320apBf18.eps}} \end{figure}$ Figure B.1: continued.

In the text

$\begin{figure}\par\resizebox{.9\textwidth}{!}{\includegraphics{6320apBf19.eps}}\par\resizebox{.9\textwidth}{!}{\includegraphics{6320apBf20.eps}} \end{figure}$ Figure B.1: continued.

In the text

$\begin{figure}\par\resizebox{.9\textwidth}{!}{\includegraphics{6320apBf21.eps}}\par\resizebox{.9\textwidth}{!}{\includegraphics{6320apBf22.eps}} \end{figure}$ Figure B.1: continued.

In the text

$\begin{figure}\par\resizebox{.9\textwidth}{!}{\includegraphics{6320apBf23.eps}}\par\resizebox{.9\textwidth}{!}{\includegraphics{6320apBf24.eps}} \end{figure}$ Figure B.1: continued.

In the text

$\begin{figure}\par\resizebox{.9\textwidth}{!}{\includegraphics{6320apBf25.eps}}\par\resizebox{.9\textwidth}{!}{\includegraphics{6320apBf26.eps}} \end{figure}$ Figure B.1: continued.

In the text

$\begin{figure}\par\resizebox{.9\textwidth}{!}{\includegraphics{6320apBf27.eps}}\par\resizebox{.9\textwidth}{!}{\includegraphics{6320apBf28.eps}} \end{figure}$ Figure B.1: continued.

In the text

$\begin{figure}\par\resizebox{.9\textwidth}{!}{\includegraphics{6320apBf29.eps}}\par\resizebox{.9\textwidth}{!}{\includegraphics{6320apBf30.eps}} \end{figure}$ Figure B.1: continued.

In the text

$\begin{figure}\par\resizebox{.9\textwidth}{!}{\includegraphics{6320apBf31.eps}}\par\resizebox{.9\textwidth}{!}{\includegraphics{6320apBf32.eps}} \end{figure}$ Figure B.1: continued.

In the text

$\begin{figure}\par\resizebox{.9\textwidth}{!}{\includegraphics{6320apBf33.eps}}\par\resizebox{.9\textwidth}{!}{\includegraphics{6320apBf34.eps}} \end{figure}$ Figure B.1: continued.

In the text

$\begin{figure}\par\resizebox{.9\textwidth}{!}{\includegraphics{6320apBf35.eps}}\par\resizebox{.9\textwidth}{!}{\includegraphics{6320apBf36.eps}} \end{figure}$ Figure B.1: continued.

In the text

$\begin{figure}\par\resizebox{.9\textwidth}{!}{\includegraphics{6320apBf37.eps}}\par\resizebox{.9\textwidth}{!}{\includegraphics{6320apBf38.eps}} \end{figure}$ Figure B.1: continued.

In the text

$\begin{figure}\par\resizebox{.9\textwidth}{!}{\includegraphics{6320apBf39.eps}}\par\resizebox{.9\textwidth}{!}{\includegraphics{6320apBf40.eps}} \end{figure}$ Figure B.1: continued.

In the text

$\begin{figure}\par\resizebox{.9\textwidth}{!}{\includegraphics{6320apBf41.eps}}\par\resizebox{.9\textwidth}{!}{\includegraphics{6320apBf42.eps}} \end{figure}$ Figure B.1: continued.

In the text

$\begin{figure}\par\resizebox{.9\textwidth}{!}{\includegraphics{6320apBf43.eps}}\par\resizebox{.9\textwidth}{!}{\includegraphics{6320apBf44.eps}} \end{figure}$ Figure B.1: continued.

In the text

$\begin{figure}\par\resizebox{.9\textwidth}{!}{\includegraphics{6320apBf45.eps}}\par\resizebox{.9\textwidth}{!}{\includegraphics{6320apBf46.eps}} \end{figure}$ Figure B.1: continued.

In the text

$\begin{figure}\par\resizebox{.9\textwidth}{!}{\includegraphics{6320apBf47.eps}}\par\resizebox{.9\textwidth}{!}{\includegraphics{6320apBf48.eps}} \end{figure}$ Figure B.1: continued.

In the text

$\begin{figure}\par\resizebox{.9\textwidth}{!}{\includegraphics{6320apBf49.eps}} \end{figure}$ Figure B.1: continued.

In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{6320fig2.eps}\end{figure}$	Figure 2: X-ray luminosity ( $L_{\rm X}$ ) in 10³⁰ erg s^-1 as a function of the observed OM magnitude. Various types of stars are identified (see text). Ultraviolet magnitudes are identified with filled symbols.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{6320fig3.eps}\end{figure}$	Figure 3: Cumulative distributions of X-ray count rates of type 2 and 3 stars.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{6320fig4.eps}\end{figure}$	Figure 4: Histogram of OM U magnitudes for type 2 and 3 stars.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{6320fig5.eps}\end{figure}$	Figure 5: Cumulative distributions of stellar luminosity of type 2 and 3 objects detected in the U filter.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{6320fig6.eps}\end{figure}$	Figure 6: Cumulative distributions of U-band OM magnitudes after correction for extinction. Type 2 stars have brighter OM magnitudes than type 3 stars. Stars with known $T_{\rm eff}$ and A_J are shown.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{6320fig7a.eps}\includegraphics[width=8cm,clip]{6320fig7b.eps}\end{figure}$	Figure 7: Normalized distributions of U-band excesses for type 2 and 3 stars. Excesses determined when A_J was used to calculate A_U are shown in the left figure, whereas excesses determined with A_V used are shown in the right figure.
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