Table 2.
Atmosphere parameters and best-fit Li and Ca pseudo-dynamical abundances for the sample of massive AGB stars.
| IRAS name | Teff (K) | log g | β | Ṁ (M⊙ yr−1) | νexp(OH) (km s−1) | log ε(Li)static | log ε(Li)dyn | log ε(Ca)static | log ε(Ca)dyn |
|---|---|---|---|---|---|---|---|---|---|
| 01085+3022* | 3300 | −0.5 | 0.2 | 1.0 × 10−7 | 13 | 2.4 | 2.2 | … | … |
| 02095−2355 | 3300** | −0.5 | 0.8 | 1.0 × 10−9 | 12† | 1.6 | 1.6 | 6.3 | 6.3 |
| 05027−2158 | 2800 | −0.5 | 0.4 | 1.0 × 10−7 | 8 | 1.1 | 1.1 | 5.8 | 5.8 |
| 05098−6422 | 3000 | −0.5 | 1.4 | 1.0 × 10−8 | 6 | ≤−1.0 | ≤0.0 | 6.1 | 6.1 |
| 05151+6312 | 3000 | −0.5 | 1.0 | 1.0 × 10−8 | 15 | ≤0.0 | ≤0.2 | 6.0 | 6.0 |
| 05559+3825 | 2900 | −0.5 | 1.6 | 1.0 × 10−7 | 12† | 0.6 | 0.5 | 5.8 | 5.8 |
| 06300+6058 | 3000 | −0.5 | 0.2 | 1.0 × 10−7 | 12 | 0.7 | 0.8 | ≤5.8 | ≤5.8 |
| 07304−2032 | 2700 | −0.5 | 0.4 | 1.0 × 10−7 | 7 | 0.9 | 1.0 | ≤5.8 | ≤5.8 |
| 09429−2148 | 3300** | −0.5 | 1.6 | 1.0 × 10−8 | 12 | 2.2 | 2.2 | 5.3 | 5.3 |
| 10261−5055 | 3000 | −0.5 | 0.2 | 1.0 × 10−9 | 4 | ≤−1.0 | ≤0.0 | 5.8 | 5.8 |
| 11081−4203 | 3000 | −0.5 | 1.6 | 5.0 × 10−8 | 8† | 1.3 | 1.1 | 5.8 | 5.8 |
| 14266−4211 | 2900 | −0.5 | 0.2 | 5.0 × 10−8 | 9 | ≤0.0 | 0.2 | ≤5.3 | ≤5.3 |
| 14337−6215* | 3300 | −0.5 | 0.2 | 5.0 × 10−8 | 20 | 2.41 | 2.41 | … | … |
| 15193+3132 | 2800 | −0.5 | 1.6 | 1.0 × 10−9 | 3 | ≤0.0 | ≤0.0 | ≤5.8 | ≤5.8 |
| 15211−4254 | 3300** | −0.5 | 1.6 | 1.0 × 10−9 | 11 | 2.3 | 2.3 | 5.8 | 5.8 |
| 15255+1944 | 2900 | −0.5 | 0.2 | 5.0 × 10−7 | 7 | 1.0 | 0.9 | 6.0 | 6.0 |
| 15576−1212 | 3000 | −0.5 | 0.2 | 1.0 × 10−8 | 10 | 1.1 | 1.2 | 5.7 | 5.7 |
| 16030−5156* | 3000 | −0.5 | 0.2 | 1.0 × 10−8 | 10† | 1.5 | 1.5 | … | … |
| 16037+4218 | 2900 | −0.5 | 1.2 | 1.0 × 10−8 | 4 | ≤−1.0 | ≤0.0 | 6.3 | 6.3 |
| 16260+3454 | 3300** | −0.5 | 0.2 | 1.0 × 10−9 | 12 | 2.7 | 2.6 | 5.4 | 5.4 |
| 17034−1024 | 3300** | −0.5 | 0.8 | 1.0 × 10−8 | 8† | ≤0.0 | ≤0.0 | 6.2 | 6.2 |
| 18413+1354 | 3300** | −0.5 | 1.2 | 1.0 × 10−8 | 15 | 1.8 | 1.7 | ≤5.3 | ≤5.3 |
| 18429−1721 | 3000 | −0.5 | 0.2 | 1.0 × 10−8 | 7 | 1.2 | 1.1 | 5.8 | 5.8 |
| 19129+2803 | 3300** | −0.5 | 0.2 | 1.0 × 10−8 | 11† | 3.11 | 3.11 | 5.5 | 5.5 |
| 19361−1658 | 3000 | −0.5 | 0.2 | 1.0 × 10−9 | 8 | 1.9 | 2.0 | 5.8 | 5.8 |
| 20052+0554* | 3300 | −0.5 | 0.2 | 1.0 × 10−7 | 16 | 2.6 | 2.3 | … | … |
| 20343−3020 | 3000 | −0.5 | 1.2 | 1.0 × 10−9 | 8 | ≤−1.0 | ≤0.0 | 6.0 | 6.0 |
| RU Cyg | 3000 | −0.5 | 1.6 | 1.0 × 10−7 | 12† | 2.0 | 1.7 | 6.2 | 6.2 |
| SV Cas | 3000 | −0.5 | 1.6 | 1.0 × 10−7 | 12† | 3.5 | 3.3 | 6.3 | 6.3 |
| R Cen2 | 3000 | −0.5 | 1.6 | 1.0 × 10−7 | 5† | 4.3 | 4.0 | … | … |
Notes. (†)These stars only display a single peak in the 1612 MHz OH maser, so we adopt an average velocity in the abundance analysis exploring OH expansion velocities of other stars with similar variability periods. (*)The S/N at Ca I 6463 Å is very low to derive any Ca abundance estimate. (**)The best fitting Teff in the Ca I 6463 Å spectral region is cooler (3000 K) than the one around the Li I 6708 Å line. (1)The line is resolved in two components (circumstellar and photospheric) and the abundance obtained corresponds to the photospheric one. (2)R Cen was not observed in the Ca I line region.
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