Table 4
Gaussian fits to the detected species shown in Fig. 8.
| Species | A(× 10−3) | v0 (km s−1) | FWHM (km s−1) | Model (#2) discrepancy |
|---|---|---|---|---|
| Mg I | 1.23 ± 0.15 | 36.36 ± 0.75 | 12.4 ± 1.8 | 6.97 ± 0.87 |
| Ca I | 0.37 ± 0.056 | 37.6 ± 1.1 | 14.8. ± 2.6 | 2.17 ± 0.33 |
| V I | 0.247 ± 0.049 | 35.7 ± 1.1 | 11.0 ± 2.5 | 1.58 ± 0.32 |
| Cr I | 0.224 ± 0.029 | 36.40 ± 0.88 | 14.0 ± 2.1 | 3.23 ± 0.42 |
| Fe I | 0.393 ± 0.024 | 34.37 ± 0.48 | 15.9 ± 1.1 | 4.70 ± 0.29 |
| Ni I | 0.313 ± 0.067 | 37.21 ± 0.92 | 8.7 ± 2.2 | 8.2 ± 1.8 |
Notes. The line amplitude (A) is equivalentto the fractional area of the star that is obscured. In the last column, the line amplitude is compared to the amplitude obtained after injection of a model spectrum containing opacity of all species minus TiO, with a temperature of 2000 K (model #2 in Fig. 3 and Table 2). Note that the line-amplitude of Mg I is significantly greater than that of the other species, due to the fact that the cross-correlation is dominated by the line triplet near 517 nm.
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