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. 21.

Schematic distribution of the pulsation periods of EC 04207 according to TESS (3 periods, black lines, upper panel), and according to Chote et al. (2013; 4 periods, blue lines, lower panel). Actually, the period of ∼423 s from TESS is a couple of very similar periods, of 423.882 s and 423.427 s. The amplitudes have been arbitrarily set to one for clarity.

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