Table 9.
SB1 solutions with f(ℳ) > 3 ℳ⊙.
| Gaia DR3 | f(ℳ) | Period | a1 sin i | R | MG | GBP − GRP | |
|---|---|---|---|---|---|---|---|
| (ℳ⊙) | (days) | (R⊙) | (R⊙) | ||||
| 4661290764764683776 (a) | 13.67 | 204.930 ± 0.862 | 349.49 | 60.52 | −6.707 | 0.474 | |
| 5863544023161862144 (b) | 7.80 | 10.605 ± 0.001 | 40.25 | −1.531 | 1.783 | ||
| 442992311418593664 (c) | 4.77 | 216.531 ± 1.463 | 255.33 | 20.16 | −1.592 | 0.862 | |
| 206292746724589824 (d) | 4.53 | 347.002 ± 0.364 | 343.50 | 42.25 | −2.741 | 2.067 | |
| 5857059996952633984 (e) | 4.25 | 155.085 ± 0.228 | 196.63 | 7.42 (h) | −0.893 | 0.684 | |
| 2174777963318889344 | 3.83 | 82.723 ± 0.158 | 124.88 | 34.82 | −1.970 | 2.021 | |
| 2031113506311851904 (f) | 3.78 | 35.908 ± 0.030 | 71.29 | −0.145 | 1.736 | ||
| 1996704839648530816 | 3.75 | 7.54574 ± 0.00077 | 25.13 | 7.29 | −1.414 | 0.520 | |
| 251157906379754496 | 3.62 | 296.676 ± 2.176 | 287.10 | −0.928 | 1.714 | ||
| 3331748140308820352 | 3.56 | 225.268 ± 1.189 | 237.61 | 0.485 | 1.836 | ||
| 1828150428697001472 | 3.54 | 333.688 ± 0.205 | 308.23 | −3.716 | 1.583 | ||
| 3112097229257687680 (g) | 3.33 | 260.978 ± 0.608 | 256.40 | 23.98 (h) | −1.711 | 1.422 | |
| 5963629779180627968 | 3.19 | 11.369 ± 0.002 | 31.30 | 11.86 (h) | 0.922 | 2.078 | |
| 512307478642441984 (f) | 3.14 | 145.578 ± 0.074 | 170.44 | −1.885 | 1.886 | ||
| 527155253604491392 | 3.13 | 149.155 ± 0.318 | 173.06 | 12.15 (h) | 0.371 | 1.856 | |
| 5869320651099982464 (f) | 3.09 | 63.924 ± 0.011 | 97.95 | −1.615 | 1.214 | ||
| 2929565719083290240 | 3.09 | 32.473 ± 0.014 | 62.31 | 7.84 (h) | 0.484 | 1.237 |
Notes. The radii R are from GSP-Phot or FLAME when available.
LHA 120-S 80: B8Ie (Rousseau et al. 1978) star in the LMC with emission lines. A distance of 49.59 kpc from Pietrzyński et al. (2019) was used to compute absolute magnitude MG.
V878 Cen: eclipsing binary star classified as a hot semi-detached system (Avvakumova et al. 2013) with the same period, confirmed by Gaia photometry.
HIP 15429: B5Ib star (Navarro et al. 2012); belongs to PMa sample of Kervella et al. (2022).
EM* GGA 311: Emission-line star (González & González 1956).
EM* RJHA 92: Emission-line Star (Robertson & Jordan 1989).
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