Table 2
Best-fit parameters obtained by fitting the Doppler-shifted emission trace of each of the detected species according to Eq. (4).
| Element | A | C | γ | σw | θ | υorb | υsys |
|---|---|---|---|---|---|---|---|
| Ca I | 149 ± 40 | −0.53 ± 0.68 | 3.1 ± 1.5 | 6.36 ± 0.96 | 4±12 | 220.2 ± 1.7 | 37.8 ± 1.1 |
| Ti I | −19 ± 19 | 0.05 ± 0.41 | 3.7 ± 1.6 | 4.8 ± 2.1 | 17 ± 46 | 221.5 ± 7.0 | 35.3 ± 3.0 |
| V I | 92 ± 17 | −0.33 ± 0.54 | 0.68 ± 0.64 | 3.98 ± 0.74 | 23 ± 23 | 216.8 ± 1.1 | 39.09 ± 0.78 |
| Cr I | 81 ± 18 | −0.37 ± 0.53 | 1.15 ± 0.84 | 5.12 ± 0.89 | 11 ± 21 | 214.9 ± 1.3 | 39.8 ± 1.0 |
| Mn I | 137 ± 39 | −0.7 ± 1.3 | 1.3 ± 1.2 | 5.7 ± 1.5 | −7 ± 27 | 216.9 ± 2.5 | 39.2 ± 2.1 |
| Fe I | 130±15 | −0.47 ± 0.35 | 1.37 ± 0.45 | 4.21 ± 0.36 | −1.5 ± 7.6 | 216.24 ± 0.51 | 38.72 ± 0.37 |
| Ni I | 177 ± 39 | −0.6 ± 1.1 | 0.42 ± 0.62 | 3.12 ± 0.71 | 3 ± 31 | 214.89 ± 0.83 | 38.33 ± 0.71 |
| Co I | 194 ± 55 | −0.49 ± 0.94 | 4.5 ± 1.1 | 5.3 ± 1.4 | 3.1 ± 7.0 | 217.8 ± 2.2 | 39.5 ± 1 .3 |
Notes. These values reflect the median and standard deviations of the marginalized posterior distributions for purposes of clarity. In reality, some posteriors are asymmetric. Refer to Fig. A.4 for the uncertainty intervals in the positive and negative direction separately.
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