Table 1.
Stellar and CSE parameters for the five RSGs in RSGC1 for which CO(2–1) emission was detected.
| Stellar parameters |
CSE parameters |
||||||||||
|---|---|---|---|---|---|---|---|---|---|---|---|
| Star | log(Lbol/L⊙) (a)(e) | Teff(a) | Spectral (a) | R⋆(a) | vLSR(b) | Rdust | v∞(b) | ṀCO(b) | ṀSED(c) | ṀCO/v∞ | ṀSED/25 |
| [K] | type | [R⊙] | [km s−1] | [R⋆] | [km s−1] | [10−6 M⊙ yr−1] | [10−6 M⊙ yr−1] | ||||
| F01 | 5.42 |
3450 ± 127 | M5 | 1450 | 117.5 | 3 | 8 | 2.0 (e) | 5.57 |
0.25 | 0.22 |
| F02 | 5.56 |
3660 ± 127 | M2 | 1500 | 120.5 | 3 | 10 | 1.8 | 5.18 |
0.18 | 0.20 |
| F03 | 5.24 |
3450 ± 127 | M5 | 1200 | 123.5 | 3 | 13 | 3.2 (e) | 4.18 |
0.25 | 0.17 |
| F04 | 5.32 |
3752 ± 117 | M1 | 1100 | 123.5 | 3 | 15 | 4.0 | − | 0.27 | − |
| F13 | 5.45 |
3590 ± 45 | M3 (d) | 1430 | 123.5 | 4 | 22 | 42 | − | 1.9 | − |
Notes. Listed are the stellar luminosity Lbol, the effective temperature Teff, the spectral type, the stellar radius R⋆, the local standard of rest velocity vLSR (see discussion in Appendix A), the dust condensation radius Rdust, the terminal wind velocity v∞, and the mass-loss rate as deduced from the CO(2–1) line, ṀCO, and as deduced from an SED analysis by Beasor et al. (2020), ṀSED. The last two columns compare a density measure, Ṁ/v∞, based on the values deduced in this study (Col. 11) and used in Beasor et al. (2020) who assumed a terminal wind velocity of 25 km s−1 (Col. 12).
From Davies et al. (2008).
As deduced from the ALMA CO(2–1) lines. The uncertainties on ṀCO are discussed in Appendices C–D.
From Beasor et al. (2020).
F13 was classified as K2 by Davies et al. (2008). However, later on it became clear that the CO-spectral type correlation is flawed if a star has a strong stellar wind, and that under these circumstances also the spectral-type – Teff relation from Levesque et al. (2006) does not hold. We therefore use the effective temperature and spectral type classification from Messineo et al. (2021).
Beasor et al. (2020) have updated the luminosities of the RSGC1 sources published by Davies et al. (2008). In particular, Beasor et al. (2020) derived log Lbol(F01) = 5.58 and log Lbol(F03) = 5.33. Changing the luminosities to the values from Beasor et al. (2020) induces an increase in ṀCO of 10% for F01 and of 3% for F03.
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