Table 4
Atmospheric properties and derived stellar parameters of the analysed stars.
| RL 104 | JL 9 | J1418 | Gaia DR2 53 | Gaia DR2 67 | Sun | |
|---|---|---|---|---|---|---|
| Spectral type | PG1159 | O(He) | He-sdO | He-sdO | He-sdO | |
| Teff/K | 80 000 ± 5000 | 80 000 ± 5000 | 70 000 ± 5000 | 75 000 ± 5000 | 75 000 ± 5000 | |
| log(g/cm s−2) | 6.0 ± 0.5 | 5.2 ± 0.3 | 6.0 ± 0.3 | 6.0 ± 0.3 | 6.3 ± 0.3 | |
| H | < 3.0 × 10−3 |  |
0.10 ± 0.04 | 0.10 ± 0.04 | 0.10 ± 0.04 | 0.74 |
| He | 0.43 |  |
0.90 ± 0.04 | 0.90 ± 0.04 | 0.90 ± 0.04 | 0.25 |
| C | 0.38 | 7.0 × 10−5 | 5.7 × 10−3 | 5.7 × 10−3 | < 1.0 × 10−3 | 2.4 × 10−3 |
| N | 0.02 | 6.9 × 10−3 | 5.8 × 10−4 | 5.8 × 10−4 | 3.5 × 10−3 | 6.9 × 10−4 |
| O | 0.17 | 7.9 × 10−5 | 6.6 × 10−4 | 6.6 × 10−4 | < 2.0 × 10−3 | 5.7 × 10−3 |
| Si | 7.9 × 10−4 | 6.6 × 10−4 | ||||
| P | 2.3 × 10−6 | 5.8 × 10−6 | ||||
| S | 1.9 × 10−4 | 3.1 × 10−4 | ||||
| Ar | 7.3 × 10−5 | 8.2 × 10−5 | ||||
| Fe | 4.5 × 10−3 | 1.3 × 10−3 | ||||
| Ni | 2.6 × 10−4 | 7.1 × 10−5 | ||||
| vrad / km s−1 | + 23 ± 10 | + 76.4 ± 1.0 | − 55 ± 3 | + 143 ± 3 | − 71 ± 6 | |
| log(L / L⊙) |  |
 |
 |
 |
 |
|
| R / R⊙ |  |
 |
 |
 |
 |
|
| M / M⊙ (VLTP) |  |
 |
||||
| M / M⊙ (merger) |  |
 |
 |
 |
||
| EB-V / mag | 0.274 | 0.019 | 0.052 | 0.029 | 0.027 | |
| Hν / erg cm−2s−1Hz−1 | 1.307 × 10−3 | 1.221 × 10−3 | 1.002 × 10−3 | 1.073 × 10−3 | 1.059 × 10−3 | |
| d / pc (spectroscopic) |  |
 |
 |
 |
 |
|
| d / pc (Gaia parallax) |  |
 |
 |
 |
 |
|
Notes. Element abundances given in mass fractions. The error limits for the abundances in RL 104 are ± 0.3 dex. For the metal abundances in the other objects, see main text. Solar abundances from Asplund et al. (2009). Luminosities, radii, and reddening derived from SED fitting using Gaia parallax distances from Bailer-Jones et al. (2021). Masses derived from VLTP tracks (Fig. 11) or merger tracks (Fig. 12). Hν is the Eddington flux of the best-fit atmosphere model used for the spectroscopic distance estimate.
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