Confirmation of the hot super-Neptune TOI-672 b with NIRPS and HARPS - Insights into the Neptunian desert around M dwarfs

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Table C.2

Stellar elemental abundances of TOI-672.

X	N	[X/H]	σ_rand	σT_eff	σ_[M/H]	σ_{log g}	σ_mac	σ_mic	σ_total
O	33	−0.282	0.002	0.005	0.063	0.004	0.008	0.005	0.064
Na	5	0.166	0.024	0.015	0.018	0.008	0.006	0.001	0.035
Mg	7	−0.204	0.072	0.087	0.029	0.011	0.001	0.005	0.117
Al	8	−0.151	0.043	0.040	0.009	0.017	0.001	0.006	0.062
Si	15	−0.152	0.034	0.055	0.060	0.021	0.022	0.027	0.097
K	6	0.156	0.061	0.018	0.030	0.027	0.036	0.033	0.090
Ca	19	0.074	0.019	0.009	0.021	0.010	0.016	0.006	0.036
Ti	54	−0.096	0.015	0.087	0.036	0.009	0.012	0.017	0.098
Cr	24	−0.072	0.021	0.016	0.022	0.010	0.012	0.007	0.038
Mn	8	0.151	0.040	0.032	0.040	0.016	0.001	0.016	0.069
Fe	63	−0.138	0.022	0.039	0.008	0.017	0.041	0.019	0.066
Ni	3	−0.006	0.032	0.060	0.035	0.019	0.003	0.001	0.082

Stellar elemental abundances [X/H] are calculated as described in Section 3.2. This table reports the number of lines N used for each element’s abundance calculation and the systematic uncertainties from random errors across multiple lines of the same element (i.e. σ_[X/H]/√N) and from variations in [X/H] with the following stellar parameters: effective temperature T_eff, overall metallicity [M/H], surface gravity logg, macro- and micro-turbulence velocities. The total uncertainty σ_total on each [X/H] value is computed from the quadrature sum of the individual error terms.

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