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Studying the ISM at ∼10 pc scale in NGC 7793 with MUSE: II. Constraints on the oxygen abundance and ionising radiation escape

Della Bruna, Lorenza; Adamo, Angela; Lee, Janice C.; Smith, Linda J.; Krumholz, Mark; Bik, Arjan; Calzetti, Daniela; Fox, Anne; Fumagalli, Michele; Grasha, Kathryn; Messa, Matteo; Östlin, Göran; Walterbos, Rene; Wofford, Aida

Studying the ISM at ∼10 pc scale in NGC 7793 with MUSE: II. Constraints on the oxygen abundance and ionising radiation escape Thumbnail


Authors

Lorenza Della Bruna

Angela Adamo

Janice C. Lee

Linda J. Smith

Mark Krumholz

Arjan Bik

Daniela Calzetti

Anne Fox

Kathryn Grasha

Matteo Messa

Göran Östlin

Rene Walterbos

Aida Wofford



Abstract

Context. Feedback from massive stars affects the interstellar medium (ISM) from the immediate surroundings of the stars (parsec scales) to galactic (kiloparsec) scales. High-spatial resolution studies of H II regions are critical to investigate how this mechanism operates. Aims. We study the ionised ISM in NGC 7793 with the MUSE instrument at ESO Very Large Telescope (VLT), over a field of view (FoV) of ∼2 kpc2 and at a spatial resolution of ∼10 pc. The aim is to link the physical conditions of the ionised gas (reddening, ionisation status, abundance measurements) within the spatially resolved H II regions to the properties of the stellar populations producing Lyman continuum photons. Methods. The analysis of the MUSE dataset, which provides a map of the ionised gas and a census of Wolf Rayet stars, is complemented with a sample of young star clusters (YSCs) and O star candidates observed with the Hubble Space Telescope (HST) and of giant molecular clouds traced in CO(2–1) emission with the Atacama Large Millimeter/submillimeter Array (ALMA). We estimated the oxygen abundance using a temperature-independent strong-line method. We determined the observed total amount of ionising photons (Q(H0)) from the extinction corrected Hα luminosity. This estimate was then compared to the expected Q(H0) obtained by summing the contributions of YSCs and massive stars. The ratio of the two values gives an estimate for the escape fraction (fesc) of photons in the region of interest. We used the [S II]/[O III] ratio as a proxy for the optical depth of the gas and classified H II regions into ionisation bounded, or as featuring channels of optically thin gas. We compared the resulting ionisation structure with the computed fesc. We also investigated the dependence of fesc on the age spanned by the stellar population in each region. Results. We find a median oxygen abundance of 12 + log(O/H) ∼ 8.37, with a scatter of 0.25 dex, which is in agreement with previous estimates for our target. We furthermore observe that the abundance map of H II regions is rich in substructures, surrounding clusters and massive stars, although clear degeneracies with photoionisation are also observed. From the population synthesis analysis, we find that YSCs located in H II regions have a higher probability of being younger and less massive as well as of emitting a higher number of ionising photons than clusters in the rest of the field. Overall, we find fesc,HII = 0.67−0.12+0.08 for the population of H II regions. We also conclude that the sources of ionisation observed within the FoV are more than sufficient to explain the amount of diffuse ionised gas (DIG) observed in this region of the galaxy. We do not observe a systematic trend between the visual appearance of H II regions and fesc, pointing to the effect of 3D geometry in the small sample probed.

Citation

Della Bruna, L., Adamo, A., Lee, J. C., Smith, L. J., Krumholz, M., Bik, A., …Wofford, A. (2021). Studying the ISM at ∼10 pc scale in NGC 7793 with MUSE: II. Constraints on the oxygen abundance and ionising radiation escape. Astronomy & Astrophysics, 650, Article A103. https://doi.org/10.1051/0004-6361/202039402

Journal Article Type Article
Acceptance Date Apr 15, 2021
Online Publication Date Jun 15, 2021
Publication Date 2021-06
Deposit Date Aug 17, 2021
Publicly Available Date Aug 17, 2021
Journal Astronomy and astrophysics.
Print ISSN 0004-6361
Electronic ISSN 1432-0746
Publisher EDP Sciences
Peer Reviewed Peer Reviewed
Volume 650
Article Number A103
DOI https://doi.org/10.1051/0004-6361/202039402

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Copyright Statement
L. Della Bruna et al., A&A, vol. 650, A103, 2021, reproduced with permission, © ESO.







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