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Table 3

Radial velocities derived from the WHT/ISIS and VLT/FLAMES spectra.

HJD Orbital S/N Primary Secondary
phase (/pixel) C W (km s-1) RV (km s-1) C W (km s-1) RV (km s-1)
2 455 899.51482 0.716 ~ 14 0.36 33.3 ± 1.8 + 73.6 ± 1.9 0.28 35.4 ± 2.5 −68.7 ± 2.7
2 455 899.73483 0.773 ~ 13 0.25 (+ 83.4 ± 3.9) 0.08
2 455 900.55487* 0.985 ~ 19 0.69 30.9 ± 1.0 (+16.5 ± 1.0)
2 455 901.50491 0.230 ~ 18 0.37 32.7 ± 1.2 (− 40.6 ± 1.4) 0.28 31.2 ± 1.6 (+96.2 ± 1.8)
2 455 901.57491 0.248 ~ 25 0.60 32.7 ± 1.1 −50.0 ± 1.1 0.42 35.0 ± 2.0 +95.0 ± 1.8
2 455 901.69492 0.279 ~ 24 0.56 32.8 ± 1.3 −49.2 ± 1.2 0.42 33.3 ± 1.7 +93.2 ± 1.6
2 455 901.77492 0.300 ~ 21 0.51 34.8 ± 1.3 −49.0 ± 1.2 0.43 34.8 ± 1.6 +88.7 ± 1.4
2 455 915.65584 0.882 ~ 26 0.36 20.8 ± 1.8 + 60.5 ± 1.6 0.21 16.1 ± 1.7 −38.1 ± 1.7
2 455 917.70423 0.411 ~ 22 0.37 19.9 ± 1.3 −13.2 ± 1.3 0.17 + 66.5 ± 5.3
2 455 918.68222 0.663 ~ 22 0.38 17.6 ± 1.1 + 74.9 ± 1.2 0.15 −46.4 ± 2.7
2 455 922.69870 0.700 ~ 22 0.40 18.2 ± 1.1 + 75.3 ± 1.2 0.20 −53.1 ± 2.4
2 455 939.65778 0.077 ~ 22 0.37 19.0 ± 1.6 −8.1 ± 1.2 0.18 16.7 ± 1.6 (+52.6 ± 2.2)
2 455 940.64342 0.331 ~ 34 0.38 17.6 ± 1.1 −33.2 ± 1.1 0.24 16.1 ± 1.4 +89.9 ± 1.5
2 455 940.67976 0.341 ~ 34 0.41 18.4 ± 1.1 −31.1 ± 1.1 0.27 16.2 ± 1.2 +88.2 ± 1.4
2 455 941.66163 0.594 ~ 35 0.38 18.4 ± 1.2 + 50.9 ± 1.0 0.22 24.2 ± 3.0 (−19.4 ± 2.6)
2 455 943.68750 0.117 ~ 23 0.38 18.5 ± 1.3 −21.6 ± 1.2 0.19 21.4 ± 4.0 +76.3 ± 3.0
2 455 944.63515 0.362 ~ 32 0.36 19.4 ± 1.8 −24.9 ± 1.5 0.22 17.1 ± 1.9 +84.4 ± 2.1
2 455 945.66720 0.628 ~ 36 0.34 16.7 ± 1.2 + 62.0 ± 1.2 0.18 16.8 ± 1.9 −39.8 ± 2.2
2 455 946.68154 0.890 ~ 22 0.36 20.7 ± 1.6 + 56.9 ± 1.4 0.23 19.3 ± 2.3 −29.1 ± 1.9
2 455 977.63971 0.880 ~ 30 0.33 19.4 ± 1.8 + 62.1 ± 1.4 0.19
2 455 979.57946 0.380 ~ 31 0.40 18.7 ± 1.0 −21.9 ± 1.0 0.17 (+81.4 ± 4.8)
2 455 981.61509 0.906 ~ 28 0.40 18.1 ± 1.0 + 50.5 ± 1.0 0.24 24.2 ± 2.6 −21.1 ± 2.5

Notes. RV values in brackets were not used in deriving the orbital solution, for reasons detailed in the text. C and W are the height and standard deviation of each peak, respectively.

(*)

Only one stellar peak was resolved in the CCF because the spectra was taken close to primary eclipse.

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