Table G.1.
Stellar and CSE parameters for the red supergiants observed in various CO rotational lines by De Beck et al. (2010).
| Stellar parameters | CSE parameters | |||||||||||
|---|---|---|---|---|---|---|---|---|---|---|---|---|
| Star | log(Lbol/L⊙) | Teff | Spectral | R⋆ | Mini | D | vLSR(c) | v∞(c) | Rout(c) |
 |
Ṁ(c) | ṀBeasor |
| type | Eq. (8) | Eq. (3) | ||||||||||
| [K] | [R⊙] | [M⊙] | [pc] | [km s−1] | [km s−1] | [R⋆] | [10−6 M⊙/yr] | [10−6 M⊙/yr] | [10−6 M⊙/yr] | |||
| α Ori | 4.94(a) | 3600(a) | M2Iab(b) | 764(a) | 19.5(a) | 168(a) | 3.4 | 13 | 800(j) | 0.4 | 0.6 | 0.07 |
| μ Cep | 5.13(d) | 3551(d) | M2Ia(b) | 974(d) | 17.5(d) | 790(i) | 31 | 21 | 600(k) | 3.0 | 6 | 1.6 |
| VX Sgr | 5.01(b) | 3535(b) | M4eIa(b) | 855(b) | 11(e) | 1570(b) | 6.5 | 22 | 3400(l) | 25 | 28 | 13 |
| VY CMa | 5.48(g) | 2800(g) | M2/4II(b) | 1680(f) | 25(h) | 1200(h) | 22.6(g) | 35(g) | 950(g) | 80(g) | 5 | 1.4 |
Notes. Listed are the stellar luminosity L⋆, the effective temperature Teff, the spectral type, the stellar radius R⋆, the initial mass Mini, the distance D, the local standard of rest velocity vLSR, the terminal wind velocity v∞, the radius of the CO envelope Rout, the gas mass-loss rate ṀCO, the mass-loss rate as predicted from Eq. (8), and the mass-loss rate predicted using the luminosity-Ṁ-relation of Beasor et al. (2020) (Eq. (3)).
From Joyce et al. (2020). Initial mass estimate ranges between 18–21 M⊙.
From De Beck et al. (2010).
From Montargès et al. (2019). Initial mass estimate ranges between 15-20 M⊙.
From Tabernero et al. (2021). Initial mass estimate ranges between 10-12 M⊙.
From Zhang et al. (2012).
From Decin et al. (2006); current mass-loss rate. For fitting the complex CO line profiles, Decin et al. (2006) invoked different shells with varying mass-loss rate.
From Wittkowski et al. (2012). Initial mass estimate ranges between 15-35 M⊙.
Estimates of μ Cep’s distance vary between 390±140 and 1818±661 pc (Montargès et al. 2019, and references therein). We here take the average value of the distance estimate of Montargès et al. (2021) (based on physical considerations on the relative size of the MOLsphere, D = 
pc) and of Davies & Beasor (2020) (based on the average parallax of neighbouring OB stars, under the assumption that the RSG is part of the same association; D = 
pc). I.e., D = 790 pc. For a change of distance from 790 pc to 390 pc, the retrieved ṀCO changes from 3×10−6 to 1×10−6 M⊙/yr.
The wind of Betelgeuse has various components. O’Gorman et al. (2012) proposes that the S2 flow of α Ori extends out to a radius of 17″ (or 800 R⋆), although the measured intensity distribution of CO emission as a function of projected radius extends to ∼8.5″ (∼400 R⋆). Changing the radius of the CO envelope from 800 R⋆ to 400 R⋆ changes the retrieved ṀCO from 0.4×10−6 M⊙/yr to 0.5×10−6 M⊙/yr.
Montargès et al. (2019) have used the NOEMA interferometer to get a channel map of the CO(2-1) emission of μ Cep at a spatial resolution of 0
92×0
72, with maximum recoverable scale (MRS) being 8″. Emission is detected up to ∼3
5 from the central star (or ∼600 R⋆).
For a mass-loss rate around 2×10−5 M⊙/yr, the predicted CO photodissociation radius is ∼3500 R⋆ (Groenewegen & Saberi 2021) or a full extent of 17″. The only CO interferometric data currently available for VX Sgr have been obtained in the framework of the ALMA ATOMIUM large program. However, the MRS of those data is only ∼8–10″ and hence cannot be used to estimate the CO envelope size. For that reason, we resort to the predictions of Groenewegen & Saberi (2021).
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