Table 4
Inferred companion presence and mass from the Gaia EDR3 proper motion analysis for the ATOMIUM sample (Kervella et al. 2022).
| Star | Parallax | RUWE(a) | S/N Prop. Mot. anomaly Hip2 - Gaia EDR3 | R1(b) (R⊙) | M1 (c) (M⊙) | M2 at 5 au(d) (M⊙) | |
|---|---|---|---|---|---|---|---|
| HIPPARCOS 2 (mas) | Gaia EDR3 (mas) | ||||||
| S Pav | 5.44 ± 1.27 | 5.758 ± 0.704 | 4.191 | 1.86 | 710 ± 36 | 1.93 ± 0.39 |  |
| T Mic | 4.75 ± 1.01 | 5.435 ± 0.283 | 2.059 | 0.90 | 722 ± 37 | 2.19 ± 0.44 |  |
| U Del | 2.08 ± 0.72 | 3.031 ± 0.115 | 1.060 | 2.23 | 449 ± 23 | 1.46 ± 0.07 |  |
| V PsA | – | – | – | – | – | – | – |
| SV Aqr | – | – | – | – | – | – | – |
| R Hya | 8.05 ± 0.69 | 6.761 ± 0.532 | 2.913 | 4.60 | 845 ± 43 | 0.73 ± 0.04 |  |
| U Her | 4.26 ± 0.85 | 2.402 ± 0.088 | 1.320 | 2.12 | 1111 ± 59 | 2.37 ± 0.47 |  |
| pi1 Gru | 6.13 ± 0.76 | 6.202 ± 0.512 | 2.908 | 18.44 | 737 ± 37 | 0.64 ± 0.03 |  |
| R Aql | 2.37 ± 0.87 | 4.323 ± 0.183 | 1.439 | 4.16 | 551 ± 29 | 0.65 ± 0.03 |  |
| W Aql | – | – | – | – | – | – | – |
| GY Aql | 4.48 ± 4.02 | 1.528 ± 0.190 | 1.479 | 4.45 | 1836 ± 102 | 2.07 ± 0.41 |  |
| AH Sco | −0.09 ± 0.57 | 0.608 ± 0.091 | 0.961 | 4.08 | 1427 ± 168 | 11.29 ± 2.26 |  |
| KW Sgr | −2.43 ± 0.94 | 0.485 ± 0.083 | 1.094 | 0.30 | 1166 ± 158 | 12.07 ± 2.41 |  |
| VX Sgr | 3.82 ± 2.73 | 0.080 ± 0.214 | 2.451 | 6.58 | 20772 ± 2136 | 23.79 ± 4.76 |  |
Notes. Note that for VX Sgr the values are meaningless due to the much-biased value of the Gaia EDR3 parallax. We also saw in Sect. 2 that the Gaia measurements for U Her and GY Aql were not reliable. (a)The RUWE is the Gaia EDR3 renormalized unit weight error. (b)R1 refer to the radius of the primary star. (c)M1 refer to the mass of the primary star. (d)M2 refer to the mass of a companion with semimajor axis of the orbit of 5 au.
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