Spectroscopic measurements, MCMC parameters, and derived parameters for five host and companion stars.
|Spectroscopic measurements of primary star|
|log g1 (dex)|
|v sin i1 (km s−1)||<5|
|Parameters from bagemass iteration|
|System age (Gyr])|
|Free parameters in MCMC sampling|
|K (km s−1)|
|fs||0 (fixed)||0 (fixed)||0 (fixed)|
|fc||0 (fixed)||0 (fixed)||0 (fixed)|
|log g2 (cgs)|
|e||0 (fixed)||0 (fixed)||0 (fixed)|
|ω (deg)||180 (fixed)||180 (fixed)||180 (fixed)|
|Prot, primary (d)(**)||–|
|Instruments and fit properties|
|Instruments||TR, Eu, COR||TR, COR||TR, COR||TR, W, COR||TR, HARPS, COR|
|Radial velocity baseline||–||–||–||–||quadratic time|
Notes. Uncertainties correspond to the 68% confidence level, where these are provided in brackets, they refer to the last significant figures. The instruments used for the observations are indicated by TR – TRAPPIST, Eu – Euler, SP – SPECULOOS, W – WASP, COR – CORALIE spectrograph, HARPS – HARPS spectrograph. Dates refer to BJDUTC − 2 450 000. The detection of the sky-projected rotation velocity is reliable for v sin i1 > 5 km s−1. (*)D denotes the observed eclipse depth of EBLM J0555-57A. A blend of the eclipse by a third component is accounted for in the derivation of the stellar radii, described in von Boetticher et al. (2017). (**) ssuming a negligible inclination of the primary star spin axis. (†)Subtraction of the background flux.
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