Table 3.
Some information of interest for the nine ‘bona fide’ SB1 systems found among the fast-rotating sample, ordered by increasing v sin i estimates.
| Target | HD 163892 | HD 308813 | HD 37737 | HD 152200 | HD 165246 | HD 15137 | HD 165174 | HD 52533 | HD 46485 |
|---|---|---|---|---|---|---|---|---|---|
| SpC | O9.5 IV(n) | O9.7 IV(n) | O9.5 II-III(n) | O9.7 IV(n) | O8 V(n) | O9.5 II-IIIn | O9.7 IIn | O8.5 IVn | O7 V((f))nvar? |
| v sin i [km s−1] | 201 | 205 | 209 | 210 | 254 | 283 | 299 | 312 | 334 |
| RVPP [km s−1] | 83.5 | 41.5 | 156.5 | 32.0 | 126.0 | 44.0 | 59.5 | 166.0 | 29.5 |
| Teff [kK] | 32.8 | 31.8 | 30.0 | 30.4 | 35.9 | 30.3 | 30.2 | 35.2 | 36.1 |
| log(ℒ/ℒ⊙) | 3.68 | 3.52 | 3.8 | 3.63 | 3.62 | 3.84 | 3.86 | 3.6 | 3.74 |
| R [R⊙] | 9.3 | 6.9 | 10.3 | 6.8 | 7.8 | 10.7 | 10.7 | 7.9 | 7.5–11 |
| log(L/L⊙) | 4.95 | 4.65 | 4.88 | 4.54 | 4.96 | 4.94 | 4.93 | 4.92 | 4.93 |
| Msp [M⊙] | 19 | 12.3 | 12.4 | < 8 | 22 | 13 | < 15 | 22 | 17 |
| v sin i/vcrit | 0.3 | 0.3 | 0.4 | 0.4 | 0.4 | 0.5 | 0.6 | 0.4 | 0.5 |
| Runaway tag | n | n | n | n | n | y | n | n | n |
| EB tag | – | ? | EB | RM | EB | n | – | EB | EB+RM |
| P [d] | 7.8 | 6.3 | 7.8 | 4.5 (c) | 4.6 (b) | 55.3 | 23.9 | 22.0 | 6.9 (c) |
| K1 [km s−1] | 41 | 32 | 70 | 23 (c) | 53 (b) | 16 | 30 (a) | 88 | 15 (c) |
| e | 0.04 | 0.38 | 0.38 | 0.17 (c) | 0.03 (b) | 0.66 | 0.16 | 0.27 | 0.01 (c) |
| f(m) [M⊙] | 0.0708 (e) | 0.0198 | 0.2224 | 0.004c | 0.071 (b) | 0.0092 | 0.0313 | 1.02 (d) | 0.002–0.00091 (c) |
| i [°] | 70 | 25 | 75 | (45) (c) | 84 (b) | 45 | (45) | 90 | 80–75 (c) |
| vsync [km s−1] | 60 | 55 | 67 | 76 | 86 | 10 | 23 | 18 | 55 |
| veq [km s−1] | 215 | 485 | 215 | 295 | 255 | 400 | 420 | 310 | 340 |
| Rough mass estimation of the hidden secondary companion (M2 [M⊙]) | |||||||||
| From Msp, f(m), i | 3.5 | 4.1 | 4.1 | < 1.0 | 3.6 | 1.8 | < 3.1 | 10.0 | 0.9 |
| From Mev, f(m), i | 3.4 – 4.2 | 5.8 – 7.5 | 5.6 – 7.2 | < 1.7 – 2.3 | 3.4 – 4.5 | 2.6 – 3.3 | < 4.8 – 6.2 | 11.2 – 14.1 | 1.0 – 1.3 |
Notes. The table includes two newly detected SB1 systems (HD 152200 and HD 46485), as well as two other ones for which Mahy et al. (2022) could detect the weak lines of a fainter secondary companion (HD 163892 and HD52533). Uncertainties on the stellar parameters can be found in Table C.2, except for the case of the spectroscopic mass (Msp), which is on the order of 15–20%. Uncertainties on the orbital parameters can be found in the quoted references. Information presented in the top half of the table has been extracted from Tables 1 and C.2 in this paper. The orbital parameters presented in the second half of the table have been mainly compiled from Mahy et al. (2022) except from those quantities conveniently specified, extracted from: (a)This work; (b)Johnston et al. (2021); (c)Simón-Díaz et al. (in prep.) and Nazé et al. (2023); (d)Trigueros Páez et al. (2021); (e)Cazorla et al. (2017b). Values of v sin i/vcrit, P, K1, e, vsync, and veq have been rounded to 0.1, 0.1 d, 1 km s−1, 0.01, 1 km s−1, and 5 km s−1, respectively.
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