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

Home

All issues

Volume 697 (May 2025)

A&A, 697 (2025) A54

Full HTML

Open Access

Table F.1

Overview of literature values of T_eff, $\dot{M}$ $\dot{M}$ , and $\dot{M} \sqrt{f_{cl}}$ $\dot{M}\sqrt{f_\textrm{cl}}$ for the presumed single stars of our sample (see also Table F.2).

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
W61-28-23	45750	−6.25	−6.25	This work	f_cl not constrained
	50600	−6.15	−5.65	Bestenlehner et al. (2025)	Optical spectral fit, v_∞ from UV, f_cl = 10
	47500	−5.60	−5.60	Massey et al. (2005)	Optical spectral fit, v_∞ from UV
	47000	−5.80	−5.80	Rivero González et al. (2012a)	Optical spectral fit
Sk −67°167	38500	−5.66	−4.84	This work	Best fitting clumping factor: f_cl = 42
	39700	−5.80	−5.30	Bestenlehner et al. (2025)	Optical spectral fit, from UV, f_cl = 10
	41809	−4.69	−4.69	Massa et al. (2017)	T_eff from spectral type, $\dot{M}$ $\dot{M}$ from mid-IR excess
	47500	−4.85	−4.85	Puls et al. (1996)	Optical spectral fit
	44100	−5.35	−5.35	Leitherer (1988)	T_eff from spectral type, $\dot{M}$ $\dot{M}$ from Hα luminosity
ST 92-4-18	41500	−6.08	−5.33	This work	Best fitting clumping factor: f_cl = 32.
	53300	−6.20	−5.70	Bestenlehner et al. (2025)	Optical spectral fit, v_∞ from UV, f_cl = 10
Sk −67°69	41500	−6.18	−5.65	This work	Best fitting clumping factor: f_cl = 11
	48200	−6.20	−5.70	Bestenlehner et al. (2025)	Optical spectral fit, v_∞ from UV, f_cl = 10
	43985	−5.33	−5.33	Massa et al. (2017)	T_eff from spectral type, $\dot{M}$ $\dot{M}$ from mid-IR excess
	45500	−5.56	−5.56	Leitherer (1988)	T_eff from spectral type, $\dot{M}$ $\dot{M}$ from Hα luminosity
Farina-88	43750	−6.35	−5.85	This work	Best fitting clumping factor: f_cl = 10.
	57200	−6.55	−6.05	Bestenlehner et al. (2025)	Optical spectral fit, v_∞ from UV, f_cl = 10
LMCE 078-1	37750	−6.01	−5.16	This work	Best fitting clumping factor: f_cl = 50.
	42400	−6.12	−5.62	Bestenlehner et al. (2025)	Optical spectral fit, v_∞ from UV, f_cl = 10
Sk −67°111	35000	−6.01	−5.26	This work	Best fitting clumping factor: f_cl = 31
	37700	−6.05	−5.55	Bestenlehner et al. (2025)	Optical spectral fit, from v_∞, f_cl = 10
	37415	−5.15	−5.15	Massa et al. (2017)	T_eff from spectral type, $\dot{M}$ $\dot{M}$ from mid-IR excess
	33000	−5.70	−5.70	Fullerton et al. (2000)	UV spectral fit
	37000	−5.60	−5.60	Leitherer (1988)	T_eff from spectral type, $\dot{M}$ $\dot{M}$ from Hα luminosity
N11-018	37000	−6.03	−5.19	This work	Best fitting clumping factor: f_cl = 48.
	37700	−6.27	−5.77	Bestenlehner et al. (2025)	Optical spectral fit, v_∞ from UV, f_cl = 10
Sk −69°50	34500	−6.16	−5.39	This work	Best fitting clumping factor: f_cl = 35
	35400	−6.53	−6.03	Bestenlehner et al. (2025)	Optical spectral fit, v_∞ from UV, f_cl = 10
Sk −71°50	36250	−6.43	−5.61	This work	Best fitting clumping factor: f_cl = 43
	35400	−6.53	−6.03	Bestenlehner et al. (2025)	Optical spectral fit, from v_∞, f_cl = 10
	39121	−5.38	−5.38	Massa et al. (201?)	T_eff from spectral type, $\dot{M}$ $\dot{M}$ from mid-IR excess
Sk −69°104	34500	−5.93	−5.11	This work	Best fitting clumping factor: f_cl = 44
	33400	−5.90	−5.40	Bestenlehner et al. (2025)	Optical spectral fit, from v_∞, f_cl = 10
	37415	−5.19	−5.19	Massa et al. (2017)	T_eff from spectral type, $\dot{M}$ $\dot{M}$ from mid-IR excess
Sk −68°16	37000	−6.22	−5.39	This work	Best fitting clumping factor: f_cl = 45
	35400	−6.23	−5.73	Bestenlehner et al. (2025)	Optical spectral fit, from v_∞, f_cl = 10
	36689	−5.32	−5.32	Massa et al. (2017)	T_eff from spectral type, $\dot{M}$ $\dot{M}$ from mid-IR excess
LH 9-34	32250	−5.80	−5.41	This work	Best fitting clumping factor: f_cl = 6.
	29900	−6.03	−5.53	Bestenlehner et al. (2025)	Optical spectral fit, v_∞ from UV, f_cl = 10
Sk −66°171	32250	−6.18	−6.18	This work	Clumping parameters not constrained
	29900	−5.99	−5.49	Bestenlehner et al. (2025)	Optical spectral fit, from UV, f_cl = 10
	30824	−5.15	−5.15	Massa et al. (2017)	T_eff from spectral type, $\dot{M}$ $\dot{M}$ from mid-IR excess
	29854	−6.07	−5.33	Alkousa et al. (2025)	Optical + UV spectral fit, f_cl = 30
Sk −71°41	31000	−6.55	−5.81	This work	Best fitting clumping factor: f_cl = 30
	29900	−6.22	−5.72	Bestenlehner et al. (2025)	Optical spectral fit, v_∞ from UV, f_cl = 10
	33021	−5.15	−5.15	Massa et al. (2017)	T_eff from spectral type, $\dot{M}$ $\dot{M}$ from mid-IR excess
	30000	−6.09	−5.59	Ramachandran et al. (2018b)	Optical + UV spectral fit, f_cl = 10
	29200	−6.03	−5.53	Alkousa et al. (2025)	Optical + UV spectral fit, f_cl = 10
Sk −67°5	27500	−6.64	−5.87	This work	Best fitting clumping factor: f_cl = 34
	26800	−5.95	−5.45	Bestenlehner et al. (2025)	Optical spectral fit, v_∞ from UV, f_cl = 10
	25600	−6.05	−5.55	Alkousa et al. (2025)	Optical + UV spectral fit, f_cl = 10

Notes. In this overview we include only analyses in which both mass-loss rate and effective temperature were derived. 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.

Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.

Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.

Initial download of the metrics may take a while.