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This article has an erratum: [https://doi.org/10.1051/0004-6361/202450066e]


Table A.5.

Properties and observed tangential velocity anomaly ΔvT, G3 for the 17 white dwarfs of our sample.

Name HIP m1 ΔG2 ΔvT, G3 ΔG3 Δ
(M) (m s−1) (MJ at 5 au)
Wolf 28 3829 0.680.02 2.1 9.44.6 2.1 °
GD 279 8709 0.640.03 2.7 12.29.2 1.3
Feige 22 11650 0.590.02 1.0 16.127.1 0.6
CPD-69 177 14754 0.680.02 0.7 5.24.6 1.1
LAWD 23 32560 0.690.03 0.8 6.811.4 0.6
GD 140 56662 0.970.03 3.4 35.510.0 3.5
LAWD 37 57367 0.610.01 5.1 8.72.1 4.1
BD-07 3632 65877 0.530.08 1.7 18.313.2 1.4
LAWD 52 66578 0.580.01 1.3 19.915.9 1.2
CD-38 10980 80300 0.680.02 1.1 7.87.6 1.0
DN Dra 82257 0.750.03 1.3 7.17.1 1.0
LAWD 74 95071 0.620.02 0.6 8.87.9 1.1
CD-30 17706 99438 0.610.02 0.4 5.813.8 0.4
HD 340611 101516 0.640.03 2.2 10.17.2 1.4
EGGR 141 102207 0.620.02 1.0 2.014.1 0.1
EGGR 150 107968 0.630.02 1.0 8.117.9 0.5
LAWD 93 117059 0.560.05 0.4 36.466.5 0.6

Notes. The estimated mass of the WD is listed in the m1 column, ΔG2 is the signal-to-noise ratio of the Hip-DR2 PMa, ΔG3 is the signal-to-noise ratio of the Hip-EDR3 PMa and is the normalized mass of the companion at an orbital radius of 5 au (or an upper limit). The column Δ is set to • for 3< ΔG3< 5 and ° for 2< ΔG3< 3.

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