Table 2
H2O maser luminosities, stellar luminosities, and mass-loss rates of the sample.
| Star | Type | D | log |
log S(tot), log Lp | log Lbol | log  |
|||||
|---|---|---|---|---|---|---|---|---|---|---|---|
| (pc) | (L⊙) | (Jy km s−1), (s−1) | (L⊙) | (M⊙ yr−1) | |||||||
| High | Mean | Low | |||||||||
| R Crt | SRV | 236 | −4.88 | 3.5 | 44.0 | 2.9 | 43.4 | 2.3 | 42.8 | 4.03 ± 0.10 | − 5.46 |
| RT Vir | SRV | 226 | −5.16 | 3.3 | 43.8 | 2.8 | 43.3 | 2.3 | 42.8 | 3.70 ± 0.09 | − 6.05 |
| RX Boo | SRV | 136 | −6.23 | 2.6 | 42.7 | 1.9 | 41.9 | 1.5 | 41.5 | 3.58 ± 0.11 | − 6.12 |
| SV Peg | SRV | 333 | −6.42 | 1.6 | 42.4 | 0.9 | 41.7 | <0.8 | <41.6 | 3.93 ± 0.20 | − 6.04 |
Notes. The stellar type is semi-regular variables (SRV). Column “D” lists distances with their references as noted below the Table. Characteristic levels of H2O maser brightness (S(tot) = integrated fluxes) and maser luminosities (
(L⊙);
Lp (photons s−1)) are listed of the objects from Paper I in 1987–2005 and from this paper in 1987–2015. The definition of the levels (high, mean, low) is described in the text. Columns
log Lbol
and
log 
list stellar luminosities and mass-loss rates.
Reference. For distances: R Crt, RT Vir: see Table 1; RX Boo: Kamezaki et al. (2012); SV Peg: Sudou et al. (2019).
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