Table 1
Our sample: M-type AGB stars.
| Star | RA (J2000) | Dec (J2000) | Ṃ (10-7M⊙ yr−1) | d (pc) | VLSR (km s−1) | Vexp (km s-1) | R⋆ (mas) | T⋆ (K) | P (days) | M⋆ (M⊙) |
|---|---|---|---|---|---|---|---|---|---|---|
| o Ceti | 02h19m20s.795 | -02°58′47.313″ | 2.0 | 102 | 47 | 3 | 15 | 2800 | 332 | 1.0 |
| R Leo | 09h47m33s.480 | + 11°25′42.883″ | 1.0 | 130 | 0.5 | 6 | 13.5 | 2800 | 310 | 1.5 |
| W Hya | 13h49m01s.925 | -28°22′04.648″ | 1.3 | 104 | 41 | 7 | 20 | 2950 | 388 | 1.0 |
| R Dor | 04h36m45s.400 | -62°04′39.259″ | 1.6 | 45 | 6.9 | 6 | 27.5 | 2400 | 175 | 1.0-1.3 |
| EP Aqr | 21h46m 31s.880 | -02°12′45.547″ | 1.2 | 114 | -34 | 11 | – | – | – | – |
Notes. Columns 4 to 11 (Same as reported in Saberi et al. 2022), for the first four sources, are taken from Vlemmings et al. (2019). The stellar masses for W Hya and R Dor are from Danilovich et al. (2017a), while those for o Ceti and R Leo 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 EP Aqr, all parameters are taken from Nhung et al. (2015, and references therein). We note that R⋆ listed here are the measured radii in the near-infrared. †The period of R Dor varies between 175 and 362 days.
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