Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=5.8cm,clip]{5736fig1a.ps}\in... ...6fig1b.ps}\includegraphics[angle=-90,width=5.8cm,clip]{5736fig1c.ps}\end{figure}$ Figure 1: Average spectra of DG Tau A ( left), GV Tau ( middle), and DP Tau ( right). Also shown are the fits to the spectra (black histograms) and separately the soft (red) and the hard (blue) spectral components.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{5736fig2a.ps}\vspace*{1mm} ... ...g2b.ps}\vspace*{1mm} \includegraphics[width=7cm,clip]{5736fig2c.ps}\end{figure}$ Figure 2: Background-subtracted light curves of DG Tau A ( top), GV Tau ( middle), and DP Tau ( bottom), binned to 500 s, 500 s, and 1000 s, respectively. Each figure contains three panels, showing, from top to bottom: Soft photons (0.4-1.0 keV for DG Tau A and GV Tau, and 0.35-1 keV for DP Tau); hard photons (1.6-7.3 keV for DG Tau A, 1.7-7.3 keV for GV Tau, 1.8-10 keV for DP Tau); full band (0.4-7.3 keV for DG Tau A and GV Tau, and 0.35-10 keV for DP Tau). For DG Tau A and GV Tau, intervals separately studied are marked by red vertical lines. Only the time intervals observed jointly by all three EPIC cameras are shown.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=5.95cm]{5736fig3a.ps}\includ... ...{5736fig3e.ps}\includegraphics[angle=-90,width=5.95cm]{5736fig3f.ps}\end{figure}$ Figure 3: Upper panel: spectra and fits of DG Tau A during low-level episodes ( left), during the rise to the large flare ( middle) and during the decay phase ( right). Lower panel: spectra and fits of GV Tau during low-level episodes ( left), during the first flare episode ( middle) and during the second flare episode ( right).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=6.5cm,clip]{5736fig4a.ps}\vspace{5mm} \includegraphics[angle=-90,width=6.5cm,clip]{5736fig4b.ps}\end{figure}$ Figure 4: Chandra spectrum of DG Tau A (from ACIS-S) and GV Tau (from ACIS-I). The histogram corresponds to the soft component modeled from XMM-Newton data but folded through the appropriate ACIS responses.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{5736fig5a.ps}\vspace*{.5mm} ... ...g5c.ps}\vspace*{.5mm} \includegraphics[width=7cm,clip]{5736fig5d.ps}\end{figure}$ Figure 5: Chandra ACIS-S images of jet-driving sources. Pixel size is $0.49\hbox {$^{\prime \prime }$ }$ ; all images were exposed for $\approx$ 30 ks and show counts in the 0.5-7 keV range except for HH 111, where only counts in the 3-7 keV range are shown to minimize background. From top to bottom: DG Tau A and B (separation $\approx$ $50^{\prime \prime }$ ); FS Tau A and B (separation $\approx$ $20^{\prime \prime }$ ); HH34 IRS; HH111 IRS (tentative detection).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=6cm,clip]{5736fig6a.ps}\hspa... ...space*{1mm} \includegraphics[angle=-90,width=6cm,clip]{5736fig6c.ps}\end{figure}$ Figure 6: Binned ACIS-S CCD spectra (red/gray, with error bars) of ( from left to right) DG Tau B, FS Tau B, and HH34 IRS, compared with the modeled, response-folded intrinsic spectra if the photoelectric absorption is removed (black solid histograms).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{5736fig7a.ps}\par\includegraphics[width=8cm,clip]{5736fig7b.ps}\end{figure}$ Figure 7: Correlation between X-ray emission and U band emission. The U band data are shown by the large crosses above the X-ray light curves and refer to the y axis labels on the right side. Top: DG Tau A; bottom: GV Tau.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.6cm]{5736fig8.ps}\end{figure}$ Figure 8: Comparison of the three Chandra spectra from DG Tau A (black, with soft component), FS Tau A (blue, thick), and FS Tau B (red).
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In the text

$\begin{figure} \hbox{\includegraphics[angle=-0,width=5.7cm]{5736fig9a.ps} \inclu... ...736fig9b.ps} \includegraphics[angle=-0,width=5.7cm]{5736fig9c.ps} } \end{figure}$ Figure 9: Chandra images of GV Tau. Left: counts in the range 0.5-5 keV. The lower cross marks the 2MASS position of GV Tau A, the upper cross the GV Tau B protostar, applying the same offset to GV Tau A as measured in radio data (Reipurth et al. 2004). Middle: similar, for the 0.5-1 keV range. Right: similar, for the 2.2-7 keV range. Pixel size is $0\hbox{$.\!\!^{\prime\prime}$ }492$ .
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=5.8cm,clip]{5736fig1a.ps}\in... ...6fig1b.ps}\includegraphics[angle=-90,width=5.8cm,clip]{5736fig1c.ps}\end{figure}$	Figure 1: Average spectra of DG Tau A ( left), GV Tau ( middle), and DP Tau ( right). Also shown are the fits to the spectra (black histograms) and separately the soft (red) and the hard (blue) spectral components.
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$\begin{figure} \par\includegraphics[angle=-90,width=5.95cm]{5736fig3a.ps}\includ... ...{5736fig3e.ps}\includegraphics[angle=-90,width=5.95cm]{5736fig3f.ps}\end{figure}$	Figure 3: Upper panel: spectra and fits of DG Tau A during low-level episodes ( left), during the rise to the large flare ( middle) and during the decay phase ( right). Lower panel: spectra and fits of GV Tau during low-level episodes ( left), during the first flare episode ( middle) and during the second flare episode ( right).
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$\begin{figure} \par\includegraphics[angle=-90,width=6.5cm,clip]{5736fig4a.ps}\vspace{5mm} \includegraphics[angle=-90,width=6.5cm,clip]{5736fig4b.ps}\end{figure}$	Figure 4: Chandra spectrum of DG Tau A (from ACIS-S) and GV Tau (from ACIS-I). The histogram corresponds to the soft component modeled from XMM-Newton data but folded through the appropriate ACIS responses.
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$\begin{figure} \par\includegraphics[angle=-90,width=6cm,clip]{5736fig6a.ps}\hspa... ...space*{1mm} \includegraphics[angle=-90,width=6cm,clip]{5736fig6c.ps}\end{figure}$	Figure 6: Binned ACIS-S CCD spectra (red/gray, with error bars) of ( from left to right) DG Tau B, FS Tau B, and HH34 IRS, compared with the modeled, response-folded intrinsic spectra if the photoelectric absorption is removed (black solid histograms).
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$\begin{figure} \par\includegraphics[width=8cm,clip]{5736fig7a.ps}\par\includegraphics[width=8cm,clip]{5736fig7b.ps}\end{figure}$	Figure 7: Correlation between X-ray emission and U band emission. The U band data are shown by the large crosses above the X-ray light curves and refer to the y axis labels on the right side. Top: DG Tau A; bottom: GV Tau.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.6cm]{5736fig8.ps}\end{figure}$	Figure 8: Comparison of the three Chandra spectra from DG Tau A (black, with soft component), FS Tau A (blue, thick), and FS Tau B (red).
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