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Fig. 1


Fundamental properties of the DA stars observed in this HST/COS far-ultraviolet spectroscopic survey. From top left to bottom right: effective temperature and surface gravity (Sect. 3), V-band magnitude, white dwarf mass and cooling age computed from Teff and log  g using the cooling models of Fontaine et al. (2001), and the main-sequence progenitor mass computed from Mwd and the initial-to-final mass relation of Kalirai et al. (2008). The full sample is indicated by the outlined histogram. 48 white dwarfs where at least photospheric Si has been detected are shown with the filled histograms, of which 23 must be currently accreting (black). The remaining 25 (grey) have Si abundances consistent with support from radiative levitation alone, and have very likely accreted in the recent past (Sect. 9.1).

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