Pulsating hydrogen-deficient white dwarfs and pre-white dwarfs observed with TESS - V. Discovery of two new DBV pulsators, WDJ152738.4−450207.4 and WD 1708−871, and asteroseismology of the already known DBV stars PG 1351+489, EC 20058−5234, and EC 04207−4748

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Fig. 27.

Inverse of the quality function of the period fit in terms of the effective temperature, shown with different colors for the different stellar masses, corresponding to three of the five periods of L 7−44 in Table 8. The vertical black dashed line corresponds to the spectroscopic T_eff of L 7−44 and the vertical dotted lines its uncertainties (T_eff = 23 980 ± 1686 K; Rolland et al. 2018).

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