All Tables

• Table 1: Positions for the two components of the V892 Tau system from radio (VLA) observations (Skinner et al. 1993) and as derived here from XMM-Newton and Chandra images.
• Table 2: The first four lines of the table report the best-fit spectral parameters for the V892 Tau system during the first XMM-Newton observation (before the flare). The parameters are derived assuming a two-temperature optically thin plasma model. Fits with a single temperature absorbed plasma model are unacceptable in this case. The last line reports the result of a spectral fit to the Chandra data on V892 Tau with a two-temperature plasma model with the two plasma temperatures and the metal abundance frozen at the values derived from this XMM-Newton exposure (first line). See text.
• Table 3: Best-fit spectral parameters for V892 Tau and V892 Tau NE during the Chandra observation and the second XMM-Newton exposure. The spectral parameters are derived assuming a single-temperature optically thin plasma model.