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Evidence for supernova feedback sustaining gas turbulence in nearby star-forming galaxies

Published online by Cambridge University Press:  09 June 2023

C. Bacchini Open the ORCID record for C. Bacchini [Opens in a new window] ,
F. Fraternali ,
G. Pezzulli ,
G. Iorio ,
A. Marasco  and
V. Nipoti
C. Bacchini
Affiliation:
INAF - Astronomical Observatory of Padova, Vicolo dell’Osservatorio 5, IT-35122, Padova, Italy email: cecilia.bacchini@inaf.it Kapteyn Astronomical Institute, University of Groningen, Landleven 12, 9747 AD Groningen, The Netherlands Department of Physics and Astronomy, University of Bologna, via Gobetti 93/2, IT-40129, Bologna, Italy
F. Fraternali
Affiliation:
Kapteyn Astronomical Institute, University of Groningen, Landleven 12, 9747 AD Groningen, The Netherlands
G. Pezzulli
Affiliation:
Kapteyn Astronomical Institute, University of Groningen, Landleven 12, 9747 AD Groningen, The Netherlands
G. Iorio
Affiliation:
Department of Physics and Astronomy, University of Padova, Vicolo dell’Osservatorio 3, IT-35122, Padova, Italy
A. Marasco
Affiliation:
INAF - Astronomical Observatory of Padova, Vicolo dell’Osservatorio 5, IT-35122, Padova, Italy email: cecilia.bacchini@inaf.it
V. Nipoti
Affiliation:
Department of Physics and Astronomy, University of Bologna, via Gobetti 93/2, IT-40129, Bologna, Italy
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Abstract

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HI and CO observations indicate that the cold gas in galaxies is very turbulent. However, the turbulent energy is expected to be quickly dissipated, implying that some energy source is needed to explain the observations. The nature of such turbulence was long unclear, as even the main candidate, supernova (SN) feedback, seemed insufficient. Other mechanisms have been proposed, but without reaching a general consensus. The key novelty of our work is considering that the gas disc thickness and flaring increase the dissipation timescale of turbulence, thus reducing the energy injection rate required to sustain it. In excellent agreement with the theoretical expectations, we found that the fraction of the SN energy (a.k.a. SN coupling efficiency) needed to maintain the cold gas turbulence is ∼ 1%, solving a long-standing conundrum.

Keywords

Turbulencestellar feedbacksupernovaeISM structurestar-forming galaxies
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 17 , Symposium S373: Resolving the Rise and Fall of Star Formation in Galaxies , August 2021 , pp. 199 - 202
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Creative Commons
Creative Common License - CCCreative Common License - BY
This is an Open Access article, distributed under the terms of the Creative Commons Attribution licence (https://creativecommons.org/licenses/by/4.0/), which permits unrestricted re-use, distribution, and reproduction in any medium, provided the original work is properly cited.
Copyright
© The Author(s), 2023. Published by Cambridge University Press on behalf of International Astronomical Union

References

Bacchini, C., Fraternali, F., Iorio, G., & Pezzulli, G. 2019a, A&A, 622a, A64.Google Scholar
Bacchini, C., Fraternali, F., Iorio, G., Pezzulli, G., Marasco, A., & Nipoti, C. 2020a, A&A, 641a, A70.Google Scholar
Bacchini, C., Fraternali, F., Pezzulli, G., & Marasco, A. 2020b, A&A, 644b, A125.Google Scholar
Bacchini, C., Fraternali, F., Pezzulli, G., Marasco, A., Iorio, G., & Nipoti, C. 2019b, A&A, 632b, A127.Google Scholar
Chevalier, R. A. 1974, ApJ, 188, 501–516.CrossRefGoogle Scholar
Di Teodoro, E. M. & Fraternali, F. 2015, MNRAS, 451, 3021–3033.CrossRefGoogle Scholar
Iorio, G. 2018,. PhD Thesis, University of Bologna, (2018).Google Scholar
Kolmogorov, A. 1941, Akademiia Nauk SSSR Doklady, 30, 301–305.Google Scholar
Mac Low, M.-M. & Klessen, R. S. 2004, Reviews of Modern Physics, 76(1), 125–194.CrossRefGoogle Scholar
Martizzi, D., Faucher-Giguère, C.-A., & Quataert, E. 2015, MNRAS, 450(1), 504–522.CrossRefGoogle Scholar
Ostriker, E. C., McKee, C. F., & Leroy, A. K. 2010, ApJ, 721, 975–994.CrossRefGoogle Scholar
Tamburro, D., Rix, H.-W., Leroy, A. K., Mac Low, M.-M., Walter, F., Kennicutt, R. C., Brinks, E., & de Blok, W. J. G. 2009, AJ, 137, 4424–4435.CrossRefGoogle Scholar
Utomo, D., Blitz, L., & Falgarone, E. 2019, ApJ, 871(1), 17.CrossRefGoogle Scholar