Table 5
Parameters from the best-fitting models of the RM effect for the five planetary systems.
| Object | λ (degree) | v sin i* (km s−1) | γ (km s−1) | CBV (km s−1) |
|---|---|---|---|---|
| HAT-P-15 | 25 ± 23 | 1.58 ± 0.29 | 31.7627 ± 0.0014 | −1.40 ± 0.85 |
| 13 ± 6 | 1.53 ± 0.25 | 31.7622 ± 0.0009 | – | |
| HAT-P-17 | −27.5 ± 6.7 | 0.84 ± 0.07 | 20.3141 ± 0.0021 | −0.46 ± 0.11 |
| −41.1 ± 3.6 | 1.00 ± 0.09 | 20.3125 ± 0.0021 | – | |
| HAT-P-21 | −0.5 ± 12.4 | 3.9 ± 0.9 | –53.018 ± 0.005 | undetected |
| −0.7 ± 12.5 | 3.9 ± 0.9 | −53.018 ± 0.005 | – | |
| HAT-P-26 | 18 ± 49 | – | – | – |
| HAT-P-29 | −21 ± 28 | 5.1 ± 0.9 | −21.6511 ± 0.0020 | > −0.58 |
| −26 ± 16 | 5.2 ± 0.7 | −21.6513 ± 0.0019 | – |
Notes. Except for the first, the columns contain two values. Those on the top are from the fit in which we considered the stellar convective blueshift (CB), whereas those on the bottom did not. The preferred values are given in bold font for each target; see the text for details. Due to the low quality of the HAT-P-26 data, we were not able to well constrain λ for this system, which was merely estimated by fixing the value of v sin i*.
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