X-Shooting ULLYSES: Massive Stars at Low Metallicity X. Physical Parameters and Feedback of Massive Stars in the LMC N11 B Star-Forming Region

Abstract

Massive stars lead the ionization and mechanical feedback within young star-forming regions. The Large Magellanic Cloud (LMC) is an ideal galaxy for studying individual massive stars and quantifying their feedback contribution to the environment. We analyze eight exemplary targets in LMC N11 B from the Hubble UV Legacy Library of Young Stars as Essential Standards (ULLYSES) program, using novel spectra from HST (COS and STIS) in the UV, and from VLT (X-shooter) in the optical. We model the spectra of early to late O-type stars by using state-of-the-art PoWR atmosphere models. We determine the stellar and wind parameters (e.g., $T_{\star }$, $\log g$, $L_{\star }$, $\dot{M}$, $v_{\infty }$) of the analyzed objects, chemical abundances (C, N, O), ionizing and mechanical feedback ($Q_{\mathrm{H}}$, $Q_{\mathrm{He}\mathrm{I}}$, $Q_{\mathrm{He}\mathrm{II}}$, $L_{\mathrm{mec}}$) and X-rays. We report ages of $2-4.5$ Myr and masses of $30-60$ $M_{\odot }$ for the analyzed stars in N11 B, consistent with a scenario of sequential star formation. We note that the observed wind-momentum luminosity relation is consistent with theoretical predictions. We detect nitrogen enrichment in most of the stars, up to a factor of seven. However, we do not find a correlation between nitrogen enrichment and projected rotational velocity. Finally, based on their spectral type, we estimate the total ionizing photons injected from the O-type stars in N11 B into its environment. We report $\log$ ($\sum$ $Q_{\mathrm{H}}$)$=50.5$ ph s${}^{-1}$, $\log$ ($\sum$ $Q_{\mathrm{He}\mathrm{I}}$)$=49.6$ ph s${}^{-1}$ and $\log$ ($\sum$ $Q_{\mathrm{He}\mathrm{II}}$)$=44.4$ ph s${}^{-1}$, consistent with the total ionizing budget in N11.

Accepted in Astronomy and Astrophysics

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