Table A.2.
Radio mass-loss rates in the C-band epoch (2018) and in the two X-band epochs (2016, 2018).
| Source | Spectral | v∞c | μc | Ṁ2018 | Ṁ2016 | Ṁ2018 | ṀLang 2005 |
|---|---|---|---|---|---|---|---|
| type b | (km/s) | (#) | 6.0 GHz | 10.0 GHz | 10.0 GHz | 22.5 GHz d | |
| qG1 (QR6 a) | B1-2 Ia+ | 500 | 1.3 | (2.0 ± 0.4) × 10−5 | (3.8 ± 0.8) × 10−5 | (2.1 ± 0.5) × 10−5 | 1.2 × 10−5 |
| qG2 (QR5 a) | WN11h | 300 | 1.8 | (1.3 ± 0.3) × 10−5 | (1.8 ± 0.4) × 10−5 | (1.8 ± 0.4) × 10−5 | 3.0 × 10−5 |
| qG3 (QR9 a) | LBV | 170 | 1.9 | (5.9 ± 1.3) × 10−6 | (1.1 ± 0.2) × 10−5 | (1.3 ± 0.3) × 10−5 | 5.2 × 10−6 |
| Pistol Star | LBV | 105 | 2.2 | (2.8 ± 0.6) × 10−6 | (5.8 ± 1.0) × 10−6 | (7.1 ± 1.0) × 10−6 | 3.1 × 10−5 |
| qG4 | WN10h | 400 | 1.8 | (9.2 ± 2.0) × 10−6 | (1.3 ± 0.3) × 10−5 | (1.2 ± 0.3) × 10−5 | |
| qG5 | < B0 I | 500 | 1.3 | (1.5 ± 0.3) × 10−5 | (1.2 ± 0.3) × 10−5 | (1.0 ± 0.2) × 10−5 | |
| qG6 (QR8 a) | WN9h | 700 | 2.78 | (2.7 ± 0.6) × 10−5 | (3.5 ± 0.7) × 10−5 | (3.5 ± 0.7) × 10−5 | 4.2 × 10−5 |
| qG7 | O7-8 Ia+/WNLh | 1500 | 1.3 | (3.3 ± 0.7) × 10−5 | (2.9 ± 0.6) × 10−5 | (3.0 ± 0.7) × 10−5 | |
| qG8 | WC8-9(d? + OB?) | 1250 | 4.7 | (9.8 ± 2.0) × 10−5 | (7.9 ± 2.0) × 10−5 | (1.1 ± 0.2) × 10−4 | |
| qG9 | WC9d (+OB) | 1250 | 4.7 | (5.4 ± 1.0) × 10−5 | (6.7 ± 1.0) × 10−5 | (5.8 ± 1.0) × 10−5 | |
| qG10 | WN8-9ha | 900 | 2.0 | (1.2 ± 0.3) × 10−5 | (2.0 ± 0.4) × 10−5 | (1.7 ± 0.4) × 10−5 | |
| qG11 (QR7 a) | WC9d(+OB) | 1250 | 4.7 | (5.4 ± 1.0) × 10−5 | (5.8 ± 1.0) × 10−5 | (4.5 ± 1.0) × 10−5 | 2.8 × 10−4 |
| qG12 | O7-8 Ia | 1500 | 1.3 | (1.5 ± 0.3) × 10−5 | (1.9 ± 0.4) × 10−5 | (2.3 ± 0.5) × 10−5 | |
| qG13 (QR4 a) | B1-2 Ia+/WNLh | 300 | 1.3 | (2.6 ± 0.6) × 10−6 | (3.6 ± 0.8) × 10−6 | (3.3 ± 0.7) × 10−6 | 2.9 × 10−5 |
| qG14 | B1-2 Ia+ | 500 | 1.3 | (4.9 ± 1.0) × 10−6 | (6.0 ± 1.0) × 10−6 | (6.0 ± 1.0) × 10−6 | |
| qG15 | WC8(d? +OB?) | 1250 | 4.7 | (3.5 ± 0.7) × 10−5 | (4.9 ± 1.0) × 10−5 | (4.9 ± 1.0) × 10−5 | |
| qG16 | WC8(d? +OB?) | 1250 | 4.7 | (5.4 ± 1.0) × 10−5 | (4.9 ± 1.0) × 10−5 | (5.8 ± 1.0) × 10−5 | |
| qG17 | B0-1 Ia+/WNLh | 500 | 1.3 | (3.2 ± 0.8) × 10−6 | (5.1 ± 1.0) × 10−6 | (4.8 ± 2.0) × 10−6 | |
| qG18 | WN6 | 1600 | 4.1 | (2.6 ± 0.7) × 10−5 | (5.1 ± 1.0) × 10−5 | (4.8 ± 2.0) × 10−5 | |
| qG19 | |||||||
| qG20 | B2-3Ia+ | 500 | 1.3 | (3.2 ± 0.9) × 10−6 | (4.4 ± 1.0) × 10−6 | (2.1 ± 0.6) × 10−6 | |
| qG21 | WC8-9(d? +OB?) | 1250 | 4.7 | (2.9 ± 0.8) × 10−5 | (3.5 ± 0.8) × 10−5 | (3.5 ± 0.8) × 10−5 | |
| qG22 | WN8-9ha | 900 | 2.0 | (9.0 ± 2.0) × 10−6 | (1.1 ± 0.2) × 10−5 | (1.1 ± 0.3) × 10−5 | |
| qG23 | O7-8 Ia | 1500 | 1.3 | (9.7 ± 3.0) × 10−6 | (1.2 ± 0.3) × 10−5 | (1.3 ± 0.3) × 10−5 | |
| qG24 | B0-1 Ia+ | 500 | 1.3 | (2.6 ± 0.8) × 10−6 | (3.8 ± 0.9) × 10−6 | (4.4 ± 1.0) × 10−6 | |
| qG25 | WC9d(+OB) | 1250 | 4.7 | (2.4 ± 0.7) × 10−5 | (3.2 ± 0.7) × 10−5 | (2.8 ± 0.7) × 10−5 | |
| qG26 | |||||||
| qG27 | WC9d(+OB) | 1250 | 4.7 | (1.7 ± 0.6) × 10−5 | (2.5 ± 0.6) × 10−5 | (2.4 ± 0.6) × 10−5 | |
| qG28 | |||||||
| qG29 |
Notes. Shown is a comparison to estimations done by Lang et al. (2005) from their 22.5 GHz when possible, and otherwise from their 8.5 GHz observations, rescaled to take into account their assumed v∞ = 1000 km s−1 and μ = 2. All mass-loss rates, Ṁ, are in units of M⊙ yr−1.
a Nomenclature for cluster members adopted by Lang et al. (2005).
b Spectral classification by Clark et al. (2018b).
c Wind parameters for qG3 and the Pistol Star from Table 1 in Najarro et al. (2009); values for qG8, qG9, qG11, qG15, qG16, qG21, qG25, and qG27 based on measurements for the GSC4 star by Najarro et al. (2017); parameters for qG2, qG4, qG6, qG10, and qG22 by Liermann et al. (2010), except μ for qG2 and qG4 estimated by Najarro (private communication); for sources of spectral types WN6, B supergiants, and OIa we adopted values of stars of similar type.
d Derived from the 22.5 GHz flux density for sources qG1 (QR6), qG2 (QR5), qG6 (QR8), and the Pistol Star, and from the 8.5 GHz flux density for qG13 (QR4), qG11 (QR7), and qG3 (QR9), as described in Table 4 by Lang et al. (2005). Values have been rescaled (see above).
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