Table A.1
Radial velocities at times out of transit for MASCARA-3 using the SONG telescope.
Time (BJD) | RV + 6 000 (m s−1) |
---|---|
2 458 223.357685 | 613.1 |
2 458 224.382018 | 183.3 |
2 458 225.434460 | 67.3 |
2 458 233.607846 | 704.9 |
2 458 234.418452 | 770.2 |
2 458 235.720058 | 234.6 |
2 458 236.641036 | 32.2 |
2 458 237.678446 | 153.1 |
2 458 238.692052 | 603.9 |
2 458 241.674223 | −70.7 |
2 458 243.368995 | 265.3 |
2 458 245.410918 | 805.6 |
2 458 246.571993 | 240.1 |
2 458 247.398019 | −31.2 |
2 458 248.368253 | 82.6 |
2 458 249.365280 | 470.8 |
2 458 250.368275 | 844.0 |
2 458 250.681785 | 837.2 |
2 458 251.366037 | 687.0 |
2 458 251.666389 | 485.7 |
2 458 252.366480 | 192.9 |
2 458 253.365122 | 120.4 |
2 458 254.365100 | 237.8 |
2 458 255.374490 | 605.4 |
2 458 256.384282 | 796.1 |
2 458 257.382395 | 330.0 |
2 458 259.383303 | 18.0 |
2 458 263.567251 | 154.9 |
2 458 265.589542 | 291.4 |
2 458 267.372280 | 829.5 |
2 458 268.609046 | 306.4 |
2 458 270.572919 | 5.0 |
2 458 274.379165 | 192.8 |
2 458 280.423224 | 17.1 |
2 458 283.600292 | 812.6 |
2 458 418.763646 | 161.4 |
2 458 426.556824 | 222.3 |
2 458 434.627715 | 639.1 |
2 458 439.611331 | 713.9 |
2 458 448.692687 | 285.5 |
2 458 449.708606 | 658.2 |
2 458 450.690659 | 709.9 |
2 458 453.742034 | 106.8 |
2 458 454.745732 | 493.1 |
2 458 586.621310 | 20.0 |
2 458 594.703421 | 710.9 |
2 458 598.446201 | 150.2 |
2 458 600.395783 | 819.7 |
2 458 602.394577 | 19.7 |
2 458 604.398027 | 462.9 |
2 458 606.403578 | 680.6 |
2 458 608.402462 | − 36.2 |
2 458 610.402961 | 656.7 |
2 458 612.656473 | 323.0 |
2 458 614.640588 | 99.4 |
2 458 616.679269 | 892.4 |
2 458 621.434468 | 611.2 |
2 458 623.623973 | 586.7 |
2 458 625.668018 | 199.2 |
2 458 627.634024 | 974.2 |
2 458 629.638527 | 312.8 |
2 458 631.621685 | 345.4 |
2 458 633.654485 | 949.8 |
2 458 638.605001 | 913.8 |
2 458 643.571329 | 579.7 |
Notes. We list the barycentric time of mid-exposure and the RVs corrected for barycentric motion. All spectra were taken with the iodine cell as reference. Although the individual uncertainties have some dependence on the flux level (which is near 30 m sec−1 at the highest and 60 m sec−1 at the lowest flux level), the overall instrumental uncertainty (σRV) is estimated to be ~ 40 m sec−1. To account for the possibility of underestimating this error, we introduced an additional jitter term during the fitting procedure (see Table 4).
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