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Table 2

Atmospheric parameters Teff , log g , and C and Si abundances.

Object Teff[K] log g [C/He] [Si/He] log N(HI) [cm-2] Distance [pc]

WD J1929+4447 30 000 (1000) 7.89 (0.15) < −6.2 < −7.5 20.4 (0.1) 395
WD 1654+160 29 410 (500) 7.97 (0.08) < −6.4 < −7.0 20.4 (0.1) 170
EC 04207-4748 25 970 (500) 7.79 (0.08) −5.6 (0.2) < −8.4 18.9 (0.1) 108
EC 20058-5234 25 500 (500) 8.01 (0.05) −5.3 (0.2) < −8.7 19.1 (0.1) 104
PG 1115+158 25 000 (500) 7.91 (0.07) −5.6 (0.2) −6.3 (0.2) 19.8 (0.1) 192

WD 0100-068 19 800 8.07 −7.3 −7.5
WD 0435+410 16 810 8.19 < −9.0 −7.2
WD 0840+262 17 770 8.30 < −8.3 < −9.0
WD 1557+192 19 570 8.15 < −7.8 < −8.1
WD 1822+410 16 230 8.01 −7.2 −7.4
WD 1940+374 16 630 8.07 < −8.5 < −9.0
WD 2144-079 16 340 8.18 < −8.5 −7.8

Notes. PG 1115+158 has additional photospheric S (−6.7 ± 0.3) and Al (−7.0 ± 0.3). All hot objects show interstellar lines from H, C, N, Si, S; some also O and/or Al. For the hot variables we also give the interstellar hydrogen column density from Lα, which was used in deriving our parameters. Numbers in brackets are estimated errors. The distance is determined from the spectroscopic radius and the solid angle. The parameters for the cool objects are from Bergeron et al. (2011), where the errors and more details can be found.

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