X-Shooting ULLYSES: Massive stars at low metallicity - X. Physical parameters and feedback of massive stars in the LMC N11 B star-forming region

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Volume 695 (March 2025)

A&A, 695 (2025) A197

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Table 3

Broadening parameters of the O-type stars in N11 B.

ID PGMW	v sin i (km s^–1) (previous)	v sin i (km s^–1) (here)	v_mac (km s^–1) (here)	metal line used (here)
(1)	(2)	(3)	(4)	(5)
3053	…	$88_{- 18}^{+ 9}$ $88_{ - 18}^{ + 9}$	15±4	N III λ4515
3058	106/68	$66_{- 13}^{+ 25}$ $66_{ - 13}^{ + 25}$	80±16	N V λ4603.8
3061	116	$120_{- 24}^{+ 20}$ $120_{ - 24}^{ + 20}$	80±16	N V λλ4604/20
3100	145	$99_{- 20}^{+ 30}$ $99_{ - 20}^{ + 30}$	92±18	C IV λ5801
3120a	…	$143_{- 29}^{+ 70}$ $143_{ - 29}^{ + 70}$	150±30	C IV λ5801
3168	96	$55_{- 11}^{+ 40}$ $55_{ - 11}^{ + 40}$	89±18	Si IV λ4088.9
3204	130	$58_{- 12}^{+ 45}$ $58_{ - 12}^{ + 45}$	97±19	C IV λ5801
3223	147	$108_{- 22}^{+ 35}$ $108_{ - 22}^{ + 35}$	93±19	O III λ5592.3

Notes. (1) PGMW # ID (Parker et al. 1992); (2) projected rotational velocity (3 sin i) reported by Evans et al. (2006); broadening parameters reported in the present work: (3) v sin i obtained with iacob- broad (Simón-Díaz & Herrero 2014) using the FT; (4) non-rotational parameter, the so-called macroturbulence (v_mac), considering the v sin i obtained with FT methodology; (5) metal line used to determine the broadening parameters.

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