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A magnetic white dwarf in a detached eclipsing binary

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Figure

Table 1. Journal of observations. Exposure times for X-shooter observations are for UVB arm, VIS arm and NIR arm, respectively
Figure 1. Phase-folded ULTRACAM and HAWK-I light curves. The light curves have been normalized to the regions immediately before and after theprimary eclipse and offset from each other vertically by 1
Figure 3. HAWK-I KS-band light curve around the time of the WD eclipse. Overplotted is a model (grey line) of the WD eclipse from fitting the g′-band lightcurve (i.e
Figure 6. Trailed spectrum of the Htracted. Two emission components are visible, the strongest, high-amplitudecomponent originates from the M dwarf and becomes stronger around phase0.5
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