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Table 2

Atmospheric properties and derived stellar parameters of the analyzed stars.

Parameter Gaia DR3 52 GSC 08265 UCAC4 108 Sun
spectral type O(He) PG1159 CO-sdO
Teff (K) 90 000 ± 5000 72 000 ± 3000 50 000 ± 3000
log (g/cm s−2) 5.5 ± 0.2 4.8 ± 0.2 5.3 ± 0.2
H <0.001 <0.001 <0.001 0.74
He 0.99 0.62−0.10+0.10$\[0.62_{-0.10}^{+0.10}\]$ 0.85 ± 0.05 0.25
C <3.0 × 10−5 0.15 ± 0.05 0.11 ± 0.03 2.4 × 10−3
N 0.003 ± 0.002 0.003−0.002+0.007$\[0.003_{-0.002}^{+0.007}\]$ 0.005 ± 0.003 6.9 × 10−4
O <5.0 × 10−4 0.23 ± 0.05 0.03 ± 0.02 5.7 × 10−3
Si 2 ± 1 × 10−4 <0.001 (3−1+3)×10−4$\[\left(3_{-1}^{+3}\right) \times 10^{-4}\]$ 6.6 × 10−4
vrad (km s−1) 0 ± 5 −10 ± 5 −15 ± 5
log (L/L⊙) 3.48−0.29+0.37$\[3.48_{-0.29}^{+0.37}\]$ 3.75−0.29+0.37$\[3.75_{-0.29}^{+0.37}\]$ ≈2.79
log (LSED/L⊙) 3.42−0.25+0.55$\[3.42_{-0.25}^{+0.55}\]$ 3.54−0.17+0.18$\[3.54_{-0.17}^{+0.18}\]$ 2.71−0.17+0.18$\[2.71_{-0.17}^{+0.18}\]$
R/R⊙ 0.23−0.05+0.08$\[0.23_{-0.05}^{+0.08}\]$ 0.48−0.10+0.19$\[0.48_{-0.10}^{+0.19}\]$ ≈0.33
RSED (R⊙) 0.21−0.02+0.03$\[0.21_{-0.02}^{+0.03}\]$ 0.38−0.04+0.05$\[0.38_{-0.04}^{+0.05}\]$ 0.30−0.02+0.03$\[0.30_{-0.02}^{+0.03}\]$
Mg (M⊙) 0.51−0.25+0.55$\[0.51_{-0.25}^{+0.55}\]$ 0.33−0.16+0.34$\[0.33_{-0.16}^{+0.34}\]$ 0.66−0.30+0.60$\[0.66_{-0.30}^{+0.60}\]$
M/M⊙ (VLTP) 0.52−0.02+0.02$\[0.52_{-0.02}^{+0.02}\]$ 0.53−0.02+0.13$\[0.53_{-0.02}^{+0.13}\]$ −
M/M⊙ (merger) 0.65−0.05+0.06$\[0.65_{-0.05}^{+0.06}\]$ 0.76−0.08+0.09$\[0.76_{-0.08}^{+0.09}\]$ ≈0.80
EB–V (mag) 0.08 ± 0.1 0.08 ± 0.1 0.13 ± 0.1
d (pc) (Gaia parallax) 2283−163+205$\[2283_{-163}^{+205}\]$ 1529−111+115$\[1529_{-111}^{+115}\]$ 1765−72+91$\[1765_{-72}^{+91}\]$

Notes. Element abundances given in mass fractions. Solar abundances from Asplund et al. (2009). Masses (M), luminosities (L), and radii (R) derived from evolutionary tracks (VLTP or merger tracks) using Teff and log g from spectroscopy (see the main text). Alternatively, these quantities (designated as Mg, LSED, and RSED) were derived from SED fits along with reddening EB–V, using Gaia parallax distances (d) from Bailer-Jones et al. (2021).

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