Fig. 3
Observed Balmer and He II lines of the white dwarf in EGB 6 (red: SDSS spectrum, gray: SPY spectrum; two lowest lines: HST spectrum) compared to a model spectrum (blue graph; Teff = 105 000 K, log g = 7.4) withthe adopted parameters (see Table 1). Nebular emission lines in the photospheric Balmer line cores are truncated for clarity.
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