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Linking stellar populations to H II regions across nearby galaxies. I. Constraining pre-supernova feedback from young clusters in NGC 1672

Barnes, A. T. and Chandar, R. and Kreckel, K. and Glover, S. C. O. and Scheuermann, F. and Belfiore, F. and Bigiel, F. and Blanc, G. A. and Boquien, M. and den Brok, J. and Congiu, E. and Chevance, M. and Dale, D. A. and Deger, S. and Kruijssen, J. M. D. and Egorov, O. V. and Eibensteiner, C. and Emsellem, E. and Grasha, K. and Groves, B. and Klessen, R. S. and Hannon, S. and Hassani, H. and Lee, J. C. and Leroy, A. K. and Lopez, L. A. and McLeod, A. F. and Pan, H. and Sánchez-Blázquez, P. and Schinnerer, E. and Sormani, M. C. and Thilker, D. A. and Ubeda, L. and Watkins, E. J. and Williams, T. G. (2022) Linking stellar populations to H II regions across nearby galaxies. I. Constraining pre-supernova feedback from young clusters in NGC 1672. Astronomy and Astrophysics, 662 . Art. No. L6. ISSN 0004-6361. doi:10.1051/0004-6361/202243766. https://resolver.caltech.edu/CaltechAUTHORS:20220721-8833000

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Abstract

Context. Stellar feedback is one of the fundamental factors regulating the evolution of galaxies. However, we still do not have access to strong observational constraints on the relative importance of the different feedback mechanisms (e.g. radiation, ionised gas pressure, stellar winds) in driving H II region evolution and molecular cloud disruption. To quantify and compare the different feedback mechanisms, the size of an H II region is crucial, whereas samples of well-resolved H II regions are scarce. Aims. We constrain the relative importance of the various feedback mechanisms from young massive star populations by resolving H II regions across the disk of the nearby star-forming galaxy NGC 1672. Methods. We combined measurements of ionised gas nebular lines obtained by PHANGS-MUSE, with high-resolution (PSF FWHM ∼ 0.1″; ∼10 pc) imaging from Hubble Space Telescope (HST) in both the narrow-band Hα and broad-band (NUV, U, B, V, I) filters. We identified a sample of 40 isolated, compact H II regions in the HST Hα image. We measured the sizes of these H II regions, which were previously unresolved in seeing-limited ground-based observations. In addition, we identified the ionisation source(s) for each H II region from catalogues produced as part of the PHANGS-HST survey. In doing so, we were able to link young stellar populations with the properties of their surrounding H II regions. Results. The HST observations allowed us to resolve all 40 regions, with radii between 5 and 40 pc. The H II regions investigated here are mildly dominated by thermal or wind pressure, yet their elevation above the radiation pressure is within the expected uncertainty range. We see that radiation pressure provides a substantially higher contribution to the total pressure than previously found in the literature over similar size scales. In general, we find higher pressures within more compact H II regions, which is driven by the inherent size scaling relations of each pressure term, albeit with significant scatter introduced by the variation in the stellar population properties (e.g. luminosity, mass, age, metallicity). Conclusions. For nearby galaxies, the combination of MUSE/VLT observations with stellar population and resolved Hα observations from HST provides a promising approach that could yield the statistics required to map out how the importance of different stellar feedback mechanisms evolve over the lifetime of a H II region.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1051/0004-6361/202243766DOIArticle
https://arxiv.org/abs/2205.05679arXivDiscussion Paper
ORCID:
AuthorORCID
Barnes, A. T.0000-0003-0410-4504
Kreckel, K.0000-0001-6551-3091
Boquien, M.0000-0003-0946-6176
den Brok, J.0000-0002-8760-6157
Dale, D. A.0000-0002-5782-9093
Deger, S.0000-0003-1943-723X
Grasha, K.0000-0002-3247-5321
Groves, B.0000-0002-9768-0246
Lee, J. C.0000-0002-2278-9407
Leroy, A. K.0000-0002-2545-1700
Lopez, L. A.0000-0002-1790-3148
Schinnerer, E.0000-0002-3933-7677
Thilker, D. A.0000-0002-8528-7340
Watkins, E. J.0000-0002-7365-5791
Additional Information:© A. T. Barnes et al. 2022. Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. Received: 12 April 2022 Accepted: 11 May 2022. We would like to thank the referee for their constructive feedback that helped improve the quality of this paper. This work was carried out as part of the PHANGS collaboration, based on observations collected at the European Southern Observatory under ESO programmes 1100.B-0651 (PHANGS–MUSE; PI Schinnerer). ATB and FB would like to acknowledge funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No. 726384/Empire). MB gratefully acknowledges support by the ANID BASAL project FB210003 and from the FONDECYT regular grants 1211000. RSK & SCOG acknowledge funding from the Deutsche Forschungsgemeinschaft (DFG) via SFB 881 ‘The Milky Way System’ (subprojects A1, B1, B2 and B8) and from the Heidelberg Cluster of Excellence STRUCTURES in the framework of Germany’s Excellence Strategy (grant EXC-2181/1 – 390900948). They also acknowledge support from the European Research Council in the ERC synergy grant ‘ECOGAL’ Understanding our Galactic ecosystem: From the disk of the Milky Way to the formation sites of stars and planets’ (project ID 855130). HAP acknowledges support by the Ministry of Science and Technology of Taiwan under grant 110-2112-M-032-020-MY3. EC acknowledges support from ANID project Basal AFB-170002. MC and JMDK gratefully acknowledge funding from the German Research Foundation (DFG) in the form of an Emmy Noether Research Group (grant number KR4801/1-1), as well as from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme via the ERC Starting Grant MUSTANG (grant agreement No. 714907). KK, FS and OE gratefully acknowledge funding from the German Research Foundation (DFG) in the form of an Emmy Noether Research Group (grant No. KR4598/2-1, PI Kreckel). ES and TGW acknowledge funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No. 694343).
Group:TAPIR
Funders:
Funding AgencyGrant Number
European Research Council (ERC)726384
Agencia Nacional de Investigación y Desarrollo (ANID)FB210003
Fondo Nacional de Desarrollo Científico y Tecnológico (FONDECYT)1211000
Deutsche Forschungsgemeinschaft (DFG)SFB 881
Bundesministerium für Bildung und Forschung (BMBF)EXC-2181/1 - 390900948
European Research Council (ERC)855130
Ministry of Science and Technology (Taipei)110-2112-M-032-020-MY3
BASAL-CATAAFB-170002
Deutsche Forschungsgemeinschaft (DFG)KR4801/1-1
European Research Council (ERC)714907
Deutsche Forschungsgemeinschaft (DFG)KR4598/2-1
European Research Council (ERC)694343
Subject Keywords:H II regions / galaxies: evolution / galaxies: star clusters: general
DOI:10.1051/0004-6361/202243766
Record Number:CaltechAUTHORS:20220721-8833000
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20220721-8833000
Official Citation:Linking stellar populations to H II regions across nearby galaxies - I. Constraining pre-supernova feedback from young clusters in NGC 1672 A. T. Barnes, R. Chandar, K. Kreckel, S. C. O. Glover, F. Scheuermann, F. Belfiore, F. Bigiel, G. A. Blanc, M. Boquien, J. den Brok, E. Congiu, M. Chevance, D. A. Dale, S. Deger, J. M. D. Kruijssen, O. V. Egorov, C. Eibensteiner, E. Emsellem, K. Grasha, B. Groves, R. S. Klessen, S. Hannon, H. Hassani, J. C. Lee, A. K. Leroy, L. A. Lopez, A. F. McLeod, H. Pan, P. Sánchez-Blázquez, E. Schinnerer, M. C. Sormani, D. A. Thilker, L. Ubeda, E. J. Watkins and T. G. Williams A&A, 662 (2022) L6 DOI: https://doi.org/10.1051/0004-6361/202243766
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:115743
Collection:CaltechAUTHORS
Deposited By: George Porter
Deposited On:22 Jul 2022 20:57
Last Modified:29 Jul 2022 21:56

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