dc.contributor.author McLeod, A. F. dc.contributor.author Dale, J. E. dc.contributor.author Evans, C. J. dc.contributor.author Ginsburg, A. dc.contributor.author Kruijssen, J. M. D. dc.contributor.author Pellegrini, E. W. dc.contributor.author Ramsay, S. K. dc.contributor.author Testi, L. dc.date.accessioned 2019-09-13T00:06:38Z dc.date.available 2019-09-13T00:06:38Z dc.date.issued 2018-10-05 dc.identifier.citation McLeod , A F , Dale , J E , Evans , C J , Ginsburg , A , Kruijssen , J M D , Pellegrini , E W , Ramsay , S K & Testi , L 2018 , ' Feedback from massive stars at low metallicities : MUSE observations of N44 and N180 in the Large Magellanic Cloud ' , Monthly Notices of the Royal Astronomical Society . https://doi.org/10.1093/mnras/sty2696 dc.identifier.issn 0035-8711 dc.identifier.other PURE: 15817912 dc.identifier.other PURE UUID: 686fb303-4b84-408d-8773-e89e27af95ff dc.identifier.other ArXiv: http://arxiv.org/abs/1810.01433v1 dc.identifier.other Scopus: 85067926561 dc.identifier.other ORCID: /0000-0001-5252-5771/work/62751073 dc.identifier.uri http://hdl.handle.net/2299/21671 dc.description Accepted for publication in MNRAS, 27 pages, 21 figures dc.description.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. en dc.language.iso eng dc.relation.ispartof Monthly Notices of the Royal Astronomical Society dc.subject astro-ph.GA dc.subject astro-ph.SR dc.title Feedback from massive stars at low metallicities : MUSE observations of N44 and N180 in the Large Magellanic Cloud en dc.contributor.institution Centre for Astrophysics Research dc.contributor.institution School of Physics, Astronomy and Mathematics dc.description.status Peer reviewed rioxxterms.version AM rioxxterms.versionofrecord https://doi.org/10.1093/mnras/sty2696 rioxxterms.type Journal Article/Review herts.preservation.rarelyaccessed true
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