An analysis of spectroscopic, seismological, astrometric, and photometric masses of pulsating white dwarf stars

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Volume 691 (November 2024)

A&A, 691 (2024) A194

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Table B.2.

Stellar masses of the DBV star sample.

Star	M_Spec	M_Seis	M_Seis(ps)	N_Π	M_Astr	M_Phot
	[M_⊙]	[M_⊙]	[M_⊙]		[M_⊙]	[M_⊙]
KIC 8626021	0.553 ± 0.037	0.664 ± 0.077⁽¹⁾	0.696 ± 0.031⁽¹⁾	5	$0 . 747_{- 0.057}^{+ 0.059}$ $0.747^{+0.059}_{-0.057}$	$0 . 680_{- 0.039}^{+ 0.049}$ $0.680^{+0.049}_{-0.039}$
KUV 05134+2605	0.726 ± 0.039	0.840 ± 0.010⁽²⁾	0.850 ± 0.050⁽²⁾	16	$0 . 798_{- 0.034}^{+ 0.033}$ $0.798^{+0.033}_{-0.034}$	$0 . 731_{- 0.033}^{+ 0.035}$ $0.731^{+0.035}_{-0.033}$
TIC 257459955	0.542 ± 0.019	0.609 ± 0.055⁽³⁾	0.621 ± 0.057⁽³⁾	10	$0 . 651_{- 0.027}^{+ 0.024}$ $0.651^{+0.024}_{-0.027}$	$0 . 596_{- 0.020}^{+ 0.022}$ $0.596^{+0.022}_{-0.020}$
GD 358	0.561 ± 0.028	0.584 ± 0.025⁽⁴⁾	0.588 ± 0.024⁽⁴⁾	19	$0 . 616_{- 0.026}^{+ 0.025}$ $0.616^{+0.025}_{-0.026}$	$0 . 579_{- 0.031}^{+ 0.034}$ $0.579^{+0.034}_{-0.031}$
PG 1351+489	0.559 ± 0.040	0.664 ± 0.013⁽⁵⁾	0.740 to 0.870⁽⁵⁾	4	$0 . 648_{- 0.047}^{+ 0.047}$ $0.648^{+0.047}_{-0.047}$	$0 . 598_{- 0.035}^{+ 0.038}$ $0.598^{+0.038}_{-0.035}$
EC 20058−5234	0.611 ± 0.029	0.664 ± 0.013⁽⁵⁾	0.530 to 0.550⁽⁵⁾	11	$0 . 618_{- 0.020}^{+ 0.020}$ $0.618^{+0.020}_{-0.020}$	$0 . 556_{- 0.018}^{+ 0.021}$ $0.556^{+0.021}_{-0.018}$
EC 04207−4748	0.516 ± 0.026	0.542 ± 0.017⁽⁵⁾	0.565 ± 0.020⁽⁵⁾	4	$0 . 660_{- 0.019}^{+ 0.020}$ $0.660^{+0.020}_{-0.019}$	$0 . 580_{- 0.018}^{+ 0.020}$ $0.580^{+0.020}_{-0.018}$
WD J1527−4502	0.673 ± 0.007	0.542 ± 0.023⁽⁵⁾	⋯	4	$0 . 694_{- 0.021}^{+ 0.018}$ $0.694^{+0.018}_{-0.021}$	$0 . 574_{- 0.026}^{+ 0.028}$ $0.574^{+0.028}_{-0.026}$
L 7−44	0.631 ± 0.020	0.565 ± 0.023⁽⁵⁾	⋯	6	$0 . 651_{- 0.030}^{+ 0.031}$ $0.651^{+0.031}_{-0.030}$	$0 . 594_{- 0.024}^{+ 0.026}$ $0.594^{+0.026}_{-0.024}$

Notes. The first column displays the star names, the second column corresponds to the spectroscopic stellar mass (M_Spec), the third column shows the seismological mass (M_Seis), the fourth column corresponds to the seismological mass inferred from the measured period spacing (M_Seis(ps)), the fifth column corresponds to the number of g-mode periods employed to derive the seismological model and the period spacing (N_Π), and the sixth and seventh columns are the astrometric (M_Astr) and photometric (M_Phot) masses, respectively.

References. (1) Córsico et al. (2012); (2) Bognár et al. (2014); (3) Bell et al. (2019); (4) Córsico et al. (2022b); (5) Córsico et al. (2022a).

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