Table B.14
The 54 companion masses measured in this paper, with re-evaluation thanks to HIPPARCOS and Gaia astrometry.
| Radial velocities | HIPPARCOS + | Gaia + | HIPPARCOS+Gaia | ||
|---|---|---|---|---|---|
| Name | Period | M2 sin i | M2 (1σ) | M2 (1σ) | ΔQ > 100? |
| (days) | (MJ) | (MJ) | (MJ) | ||
| 20 MJ < Msin i < 90 MJ | |||||
| Brown dwarfs | |||||
| BD+291539 b | 175.87 | 59.7 | <500 | <70 | |
| HD 23965 b | 3975 | 40 | (47, 68) | ||
| HD 48679 b | 1111.61 | 36 | <320 | (41, 55) | |
| HD 82460 b | 590.9 | 73.2 | <270 | (78, 81) | |
| Possible BDs | |||||
| HD 211681 b | 7612 | 77.8 | <100 | ||
| HD 28635 b | 2636.8 | 77.1 | (83, 94) | ||
| HD 71827 b | 15.05 | 26.3 | <1070 | <640 (b) | |
| M-dwarfs | |||||
| BD+210055 b | 1322.63 | 85.3 | (190, 230) | (96, 110) | |
| HD 130396 b | 2060.6 | 50.9 | (88, 130) | ||
| HD 210631 b | 4030 | 83.4 | (330, 730) | ||
| HD 217850 b | 3508.2 | 22.3 | (100, 140) | ||
| HD 77712 b (c) | 1311.7 | 42.1 | <180 | (150, 210) | |
| 90 MJ < Msin i < 0.52 M⊙ | |||||
| BD+132550 b | 2537 | 463 | <680 | ||
| BD+192536 b | 178.54 | 108.5 | <460 | (120, 130) | |
| BD+212816 b | 788.91 | 120.4 | (140, 180) | (170, 190) | |
| BD+281779 b | 46.32 | 90.8 | <830 | <130 | |
| BD+362641 b | 17.31 | 251 | <5670 | (350, 450) | |
| BD+680971 b | 1134.14 | 276 | (300, 460) | (350, 410) | |
| HD 101305 b | 1677.4 | 106.1 | (230, 310) | (220, 270) | |
| HD 103913 b | 2322 | 98.1 | (120, 150) | ||
| HD 104289 b | 2389 | 125.8 | (120, 210) | (140, 160) | |
| HD 106888 b | 365.61 | 108.3 | <300 | (130, 160) | |
| HD 108436 b | 2720 | 305 | (385, 395) | Yes | |
| HD 109157 b | 300.21 | 153.1 | <320 | (175, 190) | |
| HD 110376 b | 1282.2 | 177.7 | (200, 240) | (210, 220) | |
| HD 13014 b | 3450 ± 390 | 370 ± 50 | Yes | ||
| HD 133621 b | 448.6 | 101.8 | (120, 140) | (110, 120) | |
| HD 144286 b | 316.77 | 117.6 | <570 | (140, 160) | |
| HD 146735 b | 13 932 ± 3864 | 244 | |||
| HD 147487 b | 533.23 | 279.7 | (320, 360) | <380 | |
| HD 15292 b | 2087 | 176.5 | (200, 220) | ||
| HD 153376 b | 4878 | 236.8 | (385, 540) | Yes | |
| HD 155228 b | 432.98 | 268.9 | (290, 310) | (340, 430) | |
| HD 156111 b | 39.44 | 92 | <790 | (220, 280) | |
| HD 156728 b | 4097 | 126.5 | <170 | Yes | |
| HD 161479 b | 10.24 | 268.7 | <2490 | <395 | |
| HD 167215 b | 3460.1 | 167.4 | (190, 215) | ||
| HD 18450 b | 25.04 | 114.6 | <600 | ||
| HD 193554 b | 798.6 | 173.6 | (227, 391) | (200, 210) | |
| HD 204613 b | 876.84 | 151.7 | (470, 550) | (265, 305) | |
| HD 207992 b | 2090 | 206.8 | (330, 410) | (265, 390) | |
| HD 212029 b | 771.02 | 122.1 | (180, 240) | (195, 225) | |
| HD 212733 b | 89.86 | 112.1 | <310 | (125, 130) | |
| HD 212735 b | 37.94 | 92.5 | <960 | <140 | |
| HD 225239 b | 701.49 | 100.5 | (1050, 1210) (a) | (480, 575) | |
| HD 24505 b | 11 268 | 238.2 | (274, 276) | ||
| HD 40647 b | 8080 ± 870 | 172 ± 11 | |||
| HD 5470 b | 7788 | 208.5 | |||
| HD 60846 b | 6030 ± 890 | 450 ± 100 | Yes | ||
| HD 62923 b | 175.22 | 91.8 | (630, 710) (a) | (595, 700) | |
| HD 73636 b | 155.29 | 102.7 | <280 | (130, 180) | |
| HD 78536 b | 11.35 | 213.7 | <2910 | (265, 390) | |
| HD 85533 b | 31 214 ± 30144 | 450 ± 100 | Yes | ||
| HD 87899 b | 1527 | 195.3 | (270, 430) | (230, 250) | |
Notes. The relative errors on the period and the M sin i are lower than 8% except for 6 companions for which it is larger than 10%. In these cases, the error bars are given for the M sin i as well as for the period. The last column indicates with a “yes” the systems for which a significant binary motion is detected with ΔQ > 100 (see Sect. 6.2). (a)Most likely overestimated, since it was assumed that the secondary is dark. (b) Assuming that only the inner companion of the triple system HD 71827 is responsible for the astrometric motion of the primary star observed with Gaia is most likely incorrect, as explained in Sect. 6.1. The astrometric noise is more likely to be explained by the outer companion. Therefore, the mass of HD 71827-b is not constrained. (c) The orbital parameters of the primary star, except the period, are certainly wrong, due to pollution by a secondary component in the CCF of the SOPHIE spectra obtained for this target. The mass is therefore most likely underestimated here.
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