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The white dwarf binary pathways survey – I a sample of FGK stars with white dwarf companions

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Figure

Figure 1. Distribution of the 23 484 RAVE dwarf stars (log g > 3.5) withboth a GALEX FUV and NUV detection
Figure 3. The distribution of temperatures of the UV-excess stars in ourcombined RAVE+LAMOST sample
Figure 6. Simulated distribution of white dwarf and main-sequence startemperatures. Our sample of UV-excess objects does not cover systemscontaining cool (Teff < 20 000 K) white dwarfs and hot (F-type, Teff >=6500 K) main-sequence stars
Figure 8. Same as Fig. 5 but with a log g = 3.5 metal-poor (log Z = −3.0)main-sequence star.
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