Table 1
M-type AGB stars with detected AlF line emission.
| Star | Ṁ (10−7 M⊙ yr−1) | d (pc) | VLSR (km s−1 ) | Vexp (kms−1) | R⋆ (mas) | T⋆ (K) | P (days) | M⋆ (M⊙) |
|---|---|---|---|---|---|---|---|---|
| o Ceti | 1 | 102 | 47 | 3 | 15 | 2800 | 332 | 1.0 |
| RLeo | 1 | 130 | 0.5 | 6 | 13.5 | 2800 | 310 | 1.5 |
| WHya | 1 | 104 | 41 | 7 | 20 | 2950 | 388 | 1.0 |
| RDor | 1 | 45 | 6.9 | 6 | 27.5 | 2400 | 175† | 1.0–1.3 |
| IK Tau | 80 | 265 | 34 | 18.5 | 6 | 2100 | 470 | 1.1–1.5 |
Notes. Columns 2–8, for the first four sources, are taken from Vlemmings et al. (2019) and the stellar masses for W Hya, R Dor, and IK Tau are from Danilovich et al. (2017). For o Ceti and R Leo, they are estimated based on the 17O/18O ratio presented by De Nutte et al. (2017) and the O isotopic ratios are taken from Hinkle et al. (2016). For IK Tau, all parameters are taken from Velilla Prieto et al. (2017, and references therein). We note that R⋆ listed here are the measured radii in the near-infrared. †Period of R Dor varies between 175 and 362 days.
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