Table A.1
Distribution of stars with IRAC magnitudes
| Count | Percentage | σ % | |
|---|---|---|---|
| Base population AGB stars | 539 | 12.3% | |
| Base population non-AGB stars | 3,828 | 87.7% | |
| High [C/Fe] stars in AGB region | 4 | 17.4% | 7.9% |
| High [C/Fe] stars in non-AGB region | 19 | 82.6% | |
| High [C/O] stars in AGB region | 4 | 17.4% | 7.9% |
| High [C/O] stars in non-AGB region | 19 | 82.6% | |
| Binary stars in AGB region | 84 | 13.8% | 1.4% |
| Binary stars in non-AGB region | 523 | 86.2% |
Notes. Base population consists of stars in initial sample that all have IRAC magnitudes and are divided into AGB and non-AGB based on IR excess. Only about 8% of stars in the parent DR17 catalogue have IRAC magnitudes. Preliminary filtering on log g, Teff and other criteria as explained reduce this percentage to 4,367 stars or 7.4% in this initial sample. The last column gives the standard deviation based on an assumed uniform binomial distribution and expressed as a percentage of the total count. The number of high [C/Fe], high [C/O] and binaries, split between AGB and non-AGB follows the distribution of the base population to within 1.1σ. This demonstrates that no significant bias is being introduced by ignoring the Mid IR excess method.
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