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Table 1.

Best-fitted solution for the planetary system orbiting HD 10180, using either the RVs derived from our new RV extraction procedure (top) or the ones derived by the HARPS DRS (bottom).

Param. Units HD 10180b HD 10180c HD 10180d HD 10180e HD 10180f HD 10180g
NEW REDUCTION

P (d)
K (m s−1)
e
ω (deg)
TP (d)
Ar (AU)
M.sini (MEarth)

σ(O–C) (m s−1) 1.60
log(Post)

HARPS DRS

P (d)
K (m s−1)
e
ω (deg)
TP (d)

Ar (AU)
M.sini (MEarth)

σ(O–C) (m s−1) 1.58
log(Post)

Notes. For each parameter, the median of the posterior is considered, with error bars computed from the MCMC chains using a 68.3% confidence interval. σ(O–C) corresponds to the weighted standard deviation of the RV residuals around this best solutions. The orbital parameters derived using our new RV extraction procedure are all compatible within 1-σ with the parameters derived using the HARPS DRS RVs.

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