Table 11
Qualitative assessment of the stellar spectral feature deviations from the solar spectrum, expressed as measured in the ratio spectra between the stars and Ganymede.
| HD | CN | CH | H & K | |
|
|
||||
| 4308 | much weaker | solar | weaker | |
| 6512 | stronger | weaker | solar | |
| 8291 | weaker | weaker | stronger | |
| 9562 | much weaker | much weaker | much weaker | |
| 12264 | weaker | weaker | much stronger | |
| 13724 | stronger | solar | much stronger | |
| 16141 | solar | solar | weaker | |
| 19467 | much weaker | solar | much weaker | |
| 19518 | much weaker | weaker | solar | |
| 24293 | solar | weaker | solar | |
| 26767 | much weaker | much weaker | much stronger | |
| 28068 | much weaker | much weaker | much stronger | |
| 28255 | much weaker | weaker | solar | |
| 28821 | much weaker | solar | solar | |
| 32963 | solar | weaker | solar | |
| 35041 | much weaker | much weaker | much stronger | |
| 37773 | much stronger | weaker | solar | |
| 43180 | much weaker | much weaker | stronger | |
| 66653 | solar | solar | solar | |
| 68618 | solar | solar | much weaker | |
| 71334 | much weaker | solar | weaker | |
| 140690 | solar | solar | solar | |
| 143337 | much weaker | solar | solar | |
| 146233 | weaker | solar | weaker | |
| 155114 | much weaker | much weaker | much stronger | |
| 157750 | solar | weaker | much stronger | |
| 159222 | much weaker | solar | stronger | |
| 159656 | solar | solar | much stronger | |
| 189625 | solar | stronger | weaker | |
| 190771 | much weaker | weaker | much stronger | |
| 191487 | much weaker | much weaker | much stronger | |
| 202072 | much weaker | solar | solar | |
| 211786 | much weaker | weaker | solar | |
| 214385 | much weaker | weaker | weaker | |
| 216436 | weaker | solar | weaker | |
| 221343 | solar | solar | much stronger | |
| 221627 | much weaker | weaker | much weaker | |
Notes. In the second and third columns we classify the strength of ratio features around the λ3870 CN bandheads and the λ4310 CH bandhead, respectively. In the fourth column, the chromospheric filling in the Ca ii H and K lines is given.
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