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Table 3

M˙[YY]fcl[band] $\[\dot{M}^{[\mathrm{YY}]} \sqrt{f_{\mathrm{cl}}^{[\text {band] }}}\]$ factors for our sources.

ID M˙16fclX$\[\dot{M}^{16} \sqrt{f_{\mathrm{cl}}^{X}}\]$ M˙18fclX$\[\dot{M}^{18} \sqrt{f_{\mathrm{cl}}^{X}}\]$ M˙18fclC$\[\dot{M}^{18} \sqrt{f_{\mathrm{cl}}^{C}}\]$ M˙22fclX$\[\dot{M}^{22} \sqrt{f_{\mathrm{cl}}^{X}}\]$ M˙22fclC$\[\dot{M}^{22} \sqrt{f_{\mathrm{cl}}^{C}}\]$ M˙05fclK$\[\dot{M}^{05} \sqrt{f_{\mathrm{cl}}^{K}}\]$(a)
F6 11.1 ± 2.3
F7 5.6 ± 0.9 5.5 ± 0.9 5.1 ± 0.9 6.4 ± 1.0 5.4 ± 0.9 5.7 ± 1.1
F3 3.4 ± 0.5 3.4 ± 0.5 3.4 ± 0.5 3.5 ± 0.5 3.2 ± 0.5 4.4 ± 0.8
Dong19 (b) 4.4 ± 0.7 4.3 ± 0.7 4.2 ± 0.7 4.6 ± 0.7 4.2 ± 0.7
F4 4.5 ± 0.7 4.6 ± 0.7 3.9 ± 0.6 5.1 ± 0.8 4.6 ± 0.7
F5 3.7 ± 0.6 3.6 ± 0.5 3.6 ± 0.6 3.8 ± 0.6 3.5 ± 0.6 4.7 ± 1.0
F8 4.5 ± 0.8 4.2 ± 0.7 4.5 ± 0.9 4.4 ± 0.7 4.3 ± 0.9 6.7 ± 1.2
Dong96 (b) 3.7 ± 0.6 3.7 ± 0.6 3.5 ± 0.6 3.9 ± 0.6 3.5 ± 0.6
F1 2.6 ± 0.4 2.7 ± 0.4 2.3 ± 0.4 2.8 ± 0.4 2.4 ± 0.5
F2 3.3 ± 0.5 3.4 ± 0.5 3.4 ± 0.6 3.2 ± 0.5 3.2 ± 0.6
F9 4.4 ± 0.7 2.6 ± 0.4 2.1 ± 0.4 2.4 ± 0.4 1.8 ± 0.4
B1 1.4 ± 0.2 1.6 ± 0.3 1.4 ± 0.3 1.5 ± 0.3 1.4 ± 0.3
F14 1.3 ± 0.2 0.9 ± 0.3 1.2 ± 0.3
F16 0.9 ± 0.2 0.8 ± 0.2 0.6 ± 0.1
F10 0.8 ± 0.2 1.1 ± 0.3 0.8 ± 0.2
F15 0.9 ± 0.2 0.9 ± 0.2
F28 0.9 ± 0.2

Notes. All mass-loss rates and their uncertainties are in 10−5 M yr−1 units. (a)We used the K-band old VLA data from Lang et al. (2005). (b)For these sources we used μ = 2 and v = 1200 km s−1, which are typical for stars of their stellar type (see, e.g. Andrews et al. 2019).

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