# University of Hertfordshire

## Feedback from massive stars at low metallicities: MUSE observations of N44 and N180 in the Large Magellanic Cloud

Research output: Contribution to journalArticle

### Documents

• dale-cs

Accepted author manuscript, 5 MB, PDF-document

• A. F. McLeod
• J. E. Dale
• C. J. Evans
• A. Ginsburg
• J. M. D. Kruijssen
• E. W. Pellegrini
• S. K. Ramsay
• L. Testi
Original language English Monthly Notices of the Royal Astronomical Society 5 Oct 2018 10.1093/mnras/sty2696 Accepted/In press - 5 Oct 2018

### Abstract

We present MUSE integral field data of two HII region complexes in the Large Magellanic Cloud (LMC), N44 and N180. Both regions consist of a main superbubble and a number of smaller, more compact HII regions that formed on the edge of the superbubble. For a total of 11 HII regions, we systematically analyse the radiative and mechanical feedback from the massive O-type stars on the surrounding gas. We exploit the integral field property of the data and the coverage of the HeII$\lambda$5412 line to identify and classify the feedback-driving massive stars, and from the estimated spectral types and luminosity classes we determine the stellar radiative output in terms of the ionising photon flux $Q_{0}$. We characterise the HII regions in terms of their sizes, morphologies, ionisation structure, luminosity and kinematics, and derive oxygen abundances via emission line ratios. We analyse the role of different stellar feedback mechanisms for each region by measuring the direct radiation pressure, the pressure of the ionised gas, and the pressure of the shock-heated winds. We find that stellar winds and ionised gas are the main drivers of HII region expansion in our sample, while the direct radiation pressure is up to three orders of magnitude lower than the other terms. We relate the total pressure to the star formation rate per unit area, $\Sigma_{SFR}$, for each region and find that stellar feedback has a negative effect on star formation, and sets an upper limit to $\Sigma_{SFR}$ as a function of increasing pressure.

### Notes

Accepted for publication in MNRAS, 27 pages, 21 figures

ID: 15817912