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Table 6

Our measurements of candidate companions to HAT, HATS, and WASP planet host stars.

Target MJD N obs Separation (′′) Pos. angle (°) Δr TCI Δv TCI Bound? References

HAT-P-30 56 770 1 3.856 ± 0.016 3.9 ± 0.2 4.333 ± 0.017 Yes (M) 4 9 10 12
HAT-P-35 56 769 1 1.016 ± 0.011 149.4 ± 0.2 3.81 ± 0.13 14
HAT-P-41 (1) 56 768 1 3.599 ± 0.016 183.7 ± 0.2 3.425 ± 0.004 6 13 14
HAT-P-41 (2) 56 768 1 0.987 ± 0.011 189.8 ± 0.2 4.42 ± 0.09
HATS-2 56 779 4 1.022 ± 0.005 42.76 ± 0.09 3.93 ± 0.03
HATS-3 56 768 1 3.671 ± 0.016 108.7 ± 0.21 7.59 ± 0.15
WASP-2 56 772 1 0.709 ± 0.010 103.4 ± 0.2 4.95 ± 0.15 Yes (M) 1 2 8 9 12 13
WASP-7 56 779 3 4.414 ± 0.011 228.73 ± 0.12 9.38 ± 0.02
WASP-8 56 883 7 4.495 ± 0.007 170.93 ± 0.08 3.534 ± 0.002 4.486 ± 0.006 Yes (M) 3 12
WASP-36 56 770 1 4.872 ± 0.019 66.5 ± 0.2 4.579 ± 0.018 5, 14
WASP-45 56 847 1 4.364 ± 0.018 317.7 ± 0.2 6.381 ± 0.011
WASP-49 56 769 1 2.239 ± 0.013 178.2 ± 0.2 4.979 ± 0.018
WASP-55 56 783 3 4.345 ± 0.010 163.62 ± 0.12 5.210 ± 0.018
WASP-64 56 769 2 4.55 ± 0.02 324.1 ± 0.2 8.3 ± 0.4
WASP-67 56 768 1 4.422 ± 0.018 51.6 ± 0.2 7.23 ± 0.10
WASP-70 56 768 1 3.140 ± 0.015 167.0 ± 0.2 2.1507 ± 0.0009 Yes (M) 11 14
WASP-77 56 883 9 3.274 ± 0.005 153.68 ± 0.07 1.512 ± 0.002 1.698 ± 0.004 Yes (MC) 7 14
WASP-90 56 786 1 0.992 ± 0.011 184.9 ± 0.2 3.22 ± 0.09
WASP-100 56 921 2 3.982 ± 0.012 186.30 ± 0.15 6.152 ± 0.008 6.18 ± 0.05 No (C)

Notes. “N” indicates the number of observations used for each star. Where more than one observation was used, the MJD quoted is in the middle of the range of observing dates. The ‘Bound?’ column indicates cases where our analyses determined that the companion is bound or unbound, and the method with which this was confirmed (Proper Motion M, Relative Brightness B, or Stellar Colours C) – no entry is given if our analyses were inconclusive. The references column lists previous analyses (if any) of the candidates.

Reference. (1) Collier Cameron et al. (2007); (2) Daemgen et al. (2009); (3) Queloz et al. (2010); (4) Enoch et al. (2011); (5) Smith et al. (2012); (6) Hartman et al. (2012); (7) Maxted et al. (2013); (8) Bergfors et al. (2013); (9) Adams et al. (2013); (10) Ginski et al. (2013); (11) Anderson et al. (2014); (12) Ngo et al. (2015); (13) Wöllert et al. (2015); (14) Wöllert & Brandner (2015).

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