A quarter century of spectroscopic monitoring of the nearby M dwarf Gl 514 - A super-Earth on an eccentric orbit moving in and out of the habitable zone

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Table C.2

Best-fit parameters obtained for the model with a rotational (dSHO) kernel applied to HARPS_TERRA and CARMENES-VIS RVs.

Fitted parameter	Best-fit value^a

	e_b = 0	e_b ≠ 0
log A_harps	0.9 ± 0.1	0.9 ± 0.1
log A_CARMENES	0.6 ± 0.1	0.6 ± 0.1
θ [d]	31.0 ± 0.5
log Q₀
log ∆Q
f
γ_{HARPS pre-2015} [m s⁻¹]	−0.2 ± 0.2	−0 1 ± 0 2
γ_{HARPS post-2015} [m s⁻¹]	−0.2 ± 0.6	−0 3 ± 0 6
γ_CARMENES [m s⁻¹]	0.2 ± 0.2	0.2 ± 0.2
σ_{jit, HARPS pre-2015} [m s⁻¹]	0.8 ± 0.1	0.8 ± 0.1
σ_{jit, HARPS post-2015} [m s⁻¹]
σ_jit,CARMENES [m s⁻¹]	0.6 ± 0.3
K_b [m s⁻¹]	0.88 ± 0.16
P_b [d]
T_conj,b [BJD-2450000]
	-
	-
K_{365–d,CARMENES} [m s⁻¹]	1.2 ± 0.2	1 2 ± 2
P_{365–d, CARMENES} [d]
T_{0,365–d CARMENES} [BJD-2450000]

Derived parameter

eccentricity, e_b	-
arg. of periapsis, ω_*, b	-

ln Z	−958.2	−956.7
ln Z_1p-ln Z_0p	+11.9	+13.4

Notes. ^(a) The uncertainties of the parameters are calculated as the 16^th and 84^th percentiles of their posterior distributions.

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