Table A.1
Sample of early massive AGBs: spectroscopic Teff and derived Li, Rb, and Zr abundancesa.
| Star | Gal. Coor. | T eff | log ε(Li) | log ε(Rb) | log ε(Zr) | Tc | Periodb | Masers | |
| (l, b) | K | log N(Li) + 12 | log N(Rb) + 12 | log N(Zr) + 12 | (days) | SiO/H2O/OH | Ref.c | ||
|
|
|||||||||
| RU Cyg | (97.37,+1.20) | 3000 | 2.0 ± 0.5 | <2.6 ± 0.3 | 2.6 ± 0.2 | No | 442 | No/No/No | 1/1/1 |
| SV Cas | (111.83, −9.04) | 3000 | 3.5 ± 0.5 | 2.6 ± 0.3 | 2.7 ± 0.2 | No | 456 | No/... /... | 2/... /... |
| R Cend | (313.42, +1.21) | 3000 | 4.3 ± 0.5 | 2.6 ± 0.3 | ... | No | 251 | No/Yes/No | 1/1/1 |
| RU Ari | (161.47, −41.90) | 3000 | No | 4.5 ± 0.7 | <2.6 ± 0.2 | No | 357 | Yes/Yes/Yes | 3/1/1 |
Notes.
The abundance uncertainties represent the formal errors due to the sensitivity of the derived abundances to slight changes in the model atmosphere parameters (ΔTeff = ± 100 K, Δ[M/H] = ±0.3, Δξ = ± 1 km s-1, Δlog g = +0.5, ΔFWHM = 50 mÅ) for each star.
R Cen was not observed around the ZrO 6474 Å bandhead, but its spectrum around the weaker (and less sensitive to the Zr content) ZrO bands near 6925 Å is identical to the other stars.
Reference. (1) Benson et al. (1990); (2) Spencer et al. (1981); (3) Deguchi et al. (2012).
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