Table 1.
CaRM parameters.
| Parameter | Physical meaning |
|---|---|
| Vsys [km s−1] | Systematic velocity of the system |
| Rp/R* | Radius ratio between planet and host star |
| K [km s−1] | Keplerian semi-amplitude |
| a/R⋆ | Semi-major axis in units of stellar radius |
| ip [°] | Orbital inclination |
| λ [°] | Spin-orbit angle |
| σ0 [km s−1] ( * ) | Width of the best Gaussian fit to the CCFs |
| log(σW) | Jitter logarithm amplitude |
| ξ [km] | Linear slope |
| log(a) ( * *) | Log-amplitude of the GP kernel |
| log(τ) ( * *) | Log-timescale of the GP kernel |
| Δϕ0 | Shift in phase about the mid-transit |
| Stellar properties | |
| v sin i⋆ [km s−1] ( * ) | Projected stellar rotation velocity |
| ui | Limb-darkening coefficients |
| β0 [km s−1] ( * ) | Width of the nonrotating star |
| ζt [km s−1] ( * ) | Macro-turbulence amplitude |
| (Teff, σTeff) [K] | Effective temperature and uncertainty |
| (log(g), σlog(g)) | Surface gravity and uncertainty |
| ([Fe/H], σ[Fe/H]) [dex] | Metallicity and uncertainty |
Notes. The first set corresponds to the orbital properties combined with the parameters that may help to model activity signals. The second constitutes the set of stellar properties, from which ui, v sin i⋆, β0, and ζt are also employed for the RM modeling. ( * )These parameters are replaced in the PyAstronomy RM model by the stellar angular velocity Ω. Additionally it is necessary to provide the inclination of the stellar rotation axis i⋆. This model does not incorporate the macro-turbulence effect on the RM anomaly. ( * *)Used for GPs.
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