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Figure 1: The field centered on the system V892 Tau and V892 Tau NE in the EPIC-pn camera before the flare (top left) and during the flare (top right), in the ACIS camera (bottom left) and in the Digital Sky Survey (bottom right). The images are on the same coordinate scale. The system is resolved in the Chandra data. The source at the south-east of the V892 Tau system is [BH98] MHO 11, a T Tauri star, the source at North-East is Hubble 4, also a T Tauri.

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In the text

	Figure 2: Background-corrected light curves of V892 Tau (top) and V892 Tau NE (bottom) from the Chandra data, where the two stars are well resolved. Note the different vertical scale.
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In the text

	Figure 3: Background-corrected spectra of V892 Tau (top) and V892 Tau NE (bottom), from the Chandra data. The best-fit absorbed 1-T models are also shown.
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In the text

	Figure 4: Background-subtracted light curve of the system V892 Tau, from the two consecutive XMM-Newton observations. With XMM-Newton the Herbig Ae star V892 Tau is unresolved from the companion V892 Tau NE, nevertheless our data indicate that this light curve is completely dominated by the activity of V892 Tau (see discussion).
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In the text

	Figure 5: Background corrected spectrum of the V892 Tau system during the first XMM-Newton observation (before the flare).
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In the text

	Figure 6: Background-corrected spectra of the V892 Tau system during the tree different phases of the second XMM-Newton observation. From top to bottom: 14 ks integration time before the flare, 8 ks during the rising phase of the flare, 10 ks during the flare maximum.
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In the text