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. 24.

Inverse of the quality function of the period fit with ℓ = 2 in terms of the effective temperature, shown with different colors for the different stellar masses, corresponding to the four periods of EC 04207 in Table 15. The vertical black dashed line corresponds to the spectroscopic T_eff of EC 04207 and the vertical dotted lines its uncertainties (T_eff = 27 288 ± 545 K; Voss et al. 2007). A prominent maxima corresponds to the best-fit model selected for EC 04207, with M_⋆ = 0.542 M_⊙ and T_eff = 27 614 K.

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