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.1.

Stellar masses of the DAV star sample.

Star	M_Spec	M_Seis	N_Π	M_Astr	M_Phot
	[M_⊙]	[M_⊙]		[M_⊙]	[M_⊙]
GD 244	0.656 ± 0.030	0.593 ± 0.012⁽¹⁾	5	$0 . 651_{- 0.026}^{+ 0.025}$ $0.651^{+0.025}_{-0.026}$	$0 . 614_{- 0.025}^{+ 0.027}$ $0.614^{+0.027}_{-0.025}$
G 226−29	0.815 ± 0.032	0.770 ± 0.034⁽¹⁾	1	$0 . 815_{- 0.012}^{+ 0.015}$ $0.815^{+0.015}_{-0.012}$	$0 . 770_{- 0.014}^{+ 0.015}$ $0.770^{+0.015}_{-0.014}$
HS 0507+0434B	0.715 ± 0.031	0.660 ± 0.023⁽¹⁾	4	$0 . 715_{- 0.027}^{+ 0.021}$ $0.715^{+0.021}_{-0.027}$	$0 . 675_{- 0.033}^{+ 0.028}$ $0.675^{+0.028}_{-0.033}$
EC 11507−1519	0.722 ± 0.031	0.705 ± 0.033⁽¹⁾	2	$0 . 691_{- 0.020}^{+ 0.018}$ $0.691^{+0.018}_{-0.020}$	$0 . 620_{- 0.024}^{+ 0.025}$ $0.620^{+0.025}_{-0.024}$
L 19−2	0.680 ± 0.030	0.705 ± 0.033⁽¹⁾	5	$0 . 691_{- 0.017}^{+ 0.013}$ $0.691^{+0.013}_{-0.017}$	$0 . 668_{- 0.015}^{+ 0.015}$ $0.668^{+0.015}_{-0.015}$
MCT 2148−2911	0.591 ± 0.005	0.632 ± 0.014⁽¹⁾	1	$0 . 650_{- 0.021}^{+ 0.023}$ $0.650^{+0.023}_{-0.021}$	$0 . 589_{- 0.025}^{+ 0.027}$ $0.589^{+0.027}_{-0.025}$
EC 14012−1446	0.709 ± 0.031	0.632 ± 0.014⁽¹⁾	9	$0 . 697_{- 0.039}^{+ 0.036}$ $0.697^{+0.036}_{-0.039}$	$0 . 632_{- 0.048}^{+ 0.054}$ $0.632^{+0.054}_{-0.048}$
EC 23487−2424	0.655 ± 0.030	0.770 ± 0.034⁽¹⁾	3	$0 . 667_{- 0.033}^{+ 0.031}$ $0.667^{+0.031}_{-0.033}$	$0 . 620_{- 0.031}^{+ 0.034}$ $0.620^{+0.034}_{-0.031}$
GD 165	0.668 ± 0.030	0.632 ± 0.014⁽¹⁾	4	$0 . 660_{- 0.016}^{+ 0.018}$ $0.660^{+0.018}_{-0.016}$	$0 . 639_{- 0.017}^{+ 0.018}$ $0.639^{+0.018}_{-0.017}$
Ross 808	0.593 ± 0.028	0.705 ± 0.033⁽¹⁾	17	$0 . 615_{- 0.025}^{+ 0.024}$ $0.615^{+0.024}_{-0.025}$	$0 . 591_{- 0.019}^{+ 0.020}$ $0.591^{+0.020}_{-0.019}$
HL Tau−76	0.563 ± 0.026	0.548 ± 0.012⁽¹⁾	12	$0 . 571_{- 0.026}^{+ 0.025}$ $0.571^{+0.025}_{-0.026}$	$0 . 532_{- 0.029}^{+ 0.027}$ $0.532^{+0.027}_{-0.029}$
GALEX J0048+1521	0.702 ± 0.043	0.949 ± 0.014⁽²⁾	6	$0 . 821_{- 0.081}^{+ 0.067}$ $0.821^{+0.067}_{-0.081}$	$0 . 852_{- 0.060}^{+ 0.066}$ $0.852^{+0.066}_{-0.060}$
SDSS J0843+0431	0.655 ± 0.024	0.837 ± 0.021⁽²⁾	6	$0 . 662_{- 0.028}^{+ 0.028}$ $0.662^{+0.028}_{-0.028}$	$0 . 594_{- 0.025}^{+ 0.026}$ $0.594^{+0.026}_{-0.025}$
GALEX J1257+0124	0.782 ± 0.051	0.705 ± 0.023⁽²⁾	8	$0 . 668_{- 0.064}^{+ 0.059}$ $0.668^{+0.059}_{-0.064}$	$0 . 744_{- 0.044}^{+ 0.053}$ $0.744^{+0.053}_{-0.044}$
2QZ J1323+0103	0.876 ± 0.038	0.917 ± 0.020⁽²⁾	15	$1 . 049_{- 0.033}^{+ 0.037}$ $1.049^{+0.037}_{-0.033}$	$0 . 820_{- 0.036}^{+ 0.040}$ $0.820^{+0.040}_{-0.036}$
GALEX J1612+0830	0.776 ± 0.025	0.705 ± 0.023⁽²⁾	1	$0 . 874_{- 0.037}^{+ 0.023}$ $0.874^{+0.023}_{-0.037}$	$0 . 830_{- 0.023}^{+ 0.024}$ $0.830^{+0.024}_{-0.023}$
SDSS J1641+3521	0.808 ± 0.069	0.721 ± 0.025⁽²⁾	2	$0 . 721_{- 0.059}^{+ 0.046}$ $0.721^{+0.046}_{-0.059}$	$0 . 596_{- 0.035}^{+ 0.049}$ $0.596^{+0.049}_{-0.035}$
GALEX J1650+3010	0.863 ± 0.032	1.024 ± 0.013⁽²⁾	3	$0 . 877_{- 0.028}^{+ 0.028}$ $0.877^{+0.028}_{-0.028}$	$0 . 824_{- 0.026}^{+ 0.027}$ $0.824^{+0.027}_{-0.026}$
GALEX J2208+0654	0.750 ± 0.025	0.949 ± 0.014⁽²⁾	2	$0 . 832_{- 0.037}^{+ 0.028}$ $0.832^{+0.028}_{-0.037}$	$0 . 825_{- 0.031}^{+ 0.033}$ $0.825^{+0.033}_{-0.031}$
KIC 11911480	0.575 ± 0.021	0.548 ± 0.010⁽³⁾	5	$0 . 692_{- 0.026}^{+ 0.025}$ $0.692^{+0.025}_{-0.026}$	$0 . 597_{- 0.023}^{+ 0.029}$ $0.597^{+0.029}_{-0.023}$
GD 1212	0.620 ± 0.029	0.632 ± 0.014⁽³⁾	7	$0 . 641_{- 0.018}^{+ 0.018}$ $0.641^{+0.018}_{-0.018}$	$0 . 609_{- 0.016}^{+ 0.017}$ $0.609^{+0.017}_{-0.016}$
GALEX J1345−0055	0.662 ± 0.012	0.686 ± 0.011⁽⁴⁾	2	$0 . 636_{- 0.015}^{+ 0.017}$ $0.636^{+0.017}_{-0.015}$	$0 . 611_{- 0.015}^{+ 0.016}$ $0.611^{+0.016}_{-0.015}$
SDSS J2159+1322	1.012 ± 0.034	0.917 ± 0.040⁽⁴⁾	3	$0 . 881_{- 0.070}^{+ 0.069}$ $0.881^{+0.069}_{-0.070}$	$0 . 928_{- 0.059}^{+ 0.060}$ $0.928^{+0.060}_{-0.059}$
BPM 37093	1.012 ± 0.029	1.160 ± 0.014⁽⁵⁾	8	$1 . 045_{- 0.038}^{+ 0.029}$ $1.045^{+0.029}_{-0.038}$	$1 . 010_{- 0.010}^{+ 0.010}$ $1.010^{+0.010}_{-0.010}$
GD 518	1.158 ± 0.028	1.220 ± 0.030⁽⁵⁾	3	$1 . 117_{- 0.013}^{+ 0.017}$ $1.117^{+0.017}_{-0.013}$	$1 . 106_{- 0.020}^{+ 0.020}$ $1.106^{+0.020}_{-0.020}$
TIC 8445665	0.578 ± 0.021	0.675⁽⁶⁾	5	$0 . 614_{- 0.034}^{+ 0.035}$ $0.614^{+0.035}_{-0.034}$	$0 . 580_{- 0.034}^{+ 0.038}$ $0.580^{+0.038}_{-0.034}$
TIC 46847635	0.595 ± 0.028	0.686⁽⁶⁾	1	$0 . 628_{- 0.032}^{+ 0.032}$ $0.628^{+0.032}_{-0.032}$	$0 . 597_{- 0.041}^{+ 0.047}$ $0.597^{+0.047}_{-0.041}$
TIC 167486543	0.934 ± 0.017	0.820⁽⁶⁾	2	$0 . 959_{- 0.025}^{+ 0.026}$ $0.959^{+0.026}_{-0.025}$	$0 . 930_{- 0.023}^{+ 0.023}$ $0.930^{+0.023}_{-0.023}$
TIC 441500792	0.632 ± 0.029	0.705⁽⁶⁾	3	$0 . 660_{- 0.046}^{+ 0.044}$ $0.660^{+0.044}_{-0.046}$	$0 . 630_{- 0.042}^{+ 0.048}$ $0.630^{+0.048}_{-0.042}$
TIC 442962289	0.858 ± 0.019	0.837⁽⁶⁾	3	$0 . 884_{- 0.036}^{+ 0.028}$ $0.884^{+0.028}_{-0.036}$	$0 . 851_{- 0.030}^{+ 0.030}$ $0.851^{+0.030}_{-0.030}$
TIC 686044219	0.616 ± 0.035	0.639⁽⁶⁾	3	$0 . 649_{- 0.052}^{+ 0.047}$ $0.649^{+0.047}_{-0.052}$	$0 . 616_{- 0.050}^{+ 0.059}$ $0.616^{+0.059}_{-0.050}$
TIC 712406809	0.556 ± 0.037	0.646⁽⁶⁾	5	$0 . 589_{- 0.048}^{+ 0.049}$ $0.589^{+0.049}_{-0.048}$	$0 . 563_{- 0.062}^{+ 0.066}$ $0.563^{+0.066}_{-0.062}$
TIC 20979953	0.590 ± 0.022	0.593⁽⁶⁾	3	$0 . 631_{- 0.029}^{+ 0.031}$ $0.631^{+0.031}_{-0.029}$	$0 . 591_{- 0.034}^{+ 0.038}$ $0.591^{+0.038}_{-0.034}$
TIC 55650407	0.580 ± 0.011	0.570⁽⁶⁾	4	$0 . 610_{- 0.018}^{+ 0.015}$ $0.610^{+0.015}_{-0.018}$	$0 . 580_{- 0.016}^{+ 0.017}$ $0.580^{+0.017}_{-0.016}$
TIC 282783760	0.623 ± 0.017	0.593⁽⁶⁾	3	$0 . 662_{- 0.030}^{+ 0.028}$ $0.662^{+0.028}_{-0.030}$	$0 . 621_{- 0.029}^{+ 0.031}$ $0.621^{+0.031}_{-0.029}$
BPM 31594	0.632 ± 0.006	0.632⁽⁷⁾	6	$0 . 643_{- 0.016}^{+ 0.015}$ $0.643^{+0.015}_{-0.016}$	$0 . 622_{- 0.029}^{+ 0.032}$ $0.622^{+0.032}_{-0.029}$
G 29−38	0.703 ± 0.025	0.632 ± 0.030⁽⁸⁾	38	$0 . 684_{- 0.022}^{+ 0.026}$ $0.684^{+0.026}_{-0.022}$	$0 . 629_{- 0.025}^{+ 0.027}$ $0.629^{+0.027}_{-0.025}$

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 shows the number of g-mode periods employed to derive the seismological mode (N_Π), the fifth column corresponds to the astrometric mass (M_Astr), and the sixth column corresponds to the photometric mass (M_Phot). It is important to note that the sample is comprised solely of DAV stars with asteroseismological models characterised by a canonical H-envelope thickness. In the case of the stars analysed by Romero et al. (2022) and Romero et al. (2023), the uncertainties in the seismological masses are not available, as they have not been explicitly provided by the authors.

References. (1) Romero et al. (2012); (2) Romero et al. (2013); (3) Romero et al. (2017); (4) Romero et al. (2019a); (5) Córsico et al. (2019b); (6) Romero et al. (2022); (7) Romero et al. (2023); (8) Uzundag et al. (2023).

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