X-Shooting ULLYSES: Massive stars at low metallicity - XII. Clumped winds of O-type (super)giants in the Large Magellanic Cloud

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Volume 697 (May 2025)

A&A, 697 (2025) A54

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Table F.2

As Table F.1 but for the stars with signs of binarity.

Source	T_eff [K]	$log \dot{M}$ $\log \dot{M}$ [M_⊙ yr^-1]	$log (\dot{M} \sqrt{f_{cl}})$ $\log (\dot{M}\sqrt{f_\mathrm{cl}})$ [M_⊙ yr^-1]	Reference	Comments
VFTS-267	42500	−6.15	−5.30	This work	Best fitting clumping factor: f_cl = 51
	44700	−5.93	−5.43	Bestenlehner et al. (2025)	Optical spectral fit, v_∞, from UV, f_cl = 10
	44100	−5.00	−5.00	Ramírez-Agudelo et al. (2017)	Optical spectral fit
	44700	−5.60	−5.10	Bestenlehner et al. (2014)	Optical spectral fit, f_cl = 10
Sk −71°46	37750	−5.68	−4.95	This work	Best fitting clumping factor: f_cl = 29
	40100	−5.90	−5.40	Bestenlehner et al. (2025)	Optical spectral fit, v_∞ from UV, f_cl = 10
	38000	−4.93	−4.43	Ramachandran et al. (2018a)	Optical + UV spectral fit, f_cl = 10
	38000	−5.72	−5.06	Ramachandran et al. (2018a)	Optical + UV spectral fit, f_cl = 20
	41809	−4.89	−4.89	Massa et al. (2017)	T_eff from spectral type, $\dot{M}$ $\dot{M}$ from mid-IR excess
Sk −67°108	43500	−6.37	−5.59	This work	Best fitting clumping factor: f_cl = 36
	44700	−6.20	−5.70	Bestenlehner et al. (2025)	Optical spectral fit, v_∞ from UV, f_cl = 10
	43985	−5.29	−5.29	Massa et al. (2017)	T_eff from spectral type, $\dot{M}$ $\dot{M}$ from mid-IR excess
Sk −71°19	39750	−7.20	−6.39	This work	Best fitting clumping factor: f_cl = 40
	40400	−7.15	−6.65	Bestenlehner et al. (2025)	Optical spectral fit, v_∞ from UV, f_cl = 10
Sk −70°115	34750	−5.73	−4.97	This work	Best fitting clumping factor: f_cl = 33
	35400	−5.80	−5.30	Bestenlehner et al. (2025)	Optical spectral fit, v_∞ from UV, f_cl = 10
	39121	−5.24	−5.24	Massa et al. (2017)	T_eff from spectral type, $\dot{M}$ $\dot{M}$ from mid-IR excess
BI 173	34500	−6.71	−6.71	This work	f_cl not constrained
	33400	−6.53	−6.03	Bestenlehner et al. (2025)	Optical spectral fit, v_∞ from UV, f_cl = 10
	33639	−5.18	−5.18	Massa et al. (2017)	T_eff from spectral type, $\dot{M}$ $\dot{M}$ from mid-IR excess
	34500	−5.80	−5.80	Massey et al. (2009)	Optical spectral fit,
Sk −68°155	31500	−5.85	−5.23	This work	Best fitting clumping factor: f_cl = 17
	29900	−6.19	−5.69	Bestenlehner et al. (2025)	Optical spectral fit, v_∞ from UV, f_cl = 10
	29000	−6.19	−5.45	Alkousa et al. (2025)	Optical + UV spectral fit, f_cl = 30

Notes. In this overview we include only analyses in which both mass-loss rate and effective temperature were derived. For LH 114-7 there were no such studies. For computing $\dot{M} \sqrt{f_{cl}}$ $\dot{M}\sqrt{f_\mathrm{cl}}$ , we assume f_cl = 1 unless another clumping factor was adopted or derived from the fitting process.

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