Simulating nearby disc galaxies on the main star formation sequence : II. The gas structure transition in low and high stellar mass discs
(2025) In Astronomy and Astrophysics 700.- Abstract
Recent hydrodynamical simulations of isolated barred disc galaxies have suggested a structural change in the distribution of the interstellar medium (ISM) around a stellar mass M∗ of 1010 M⊙. In the higher-mass regime (M∗ ≤ 1010 M⊙), we observe the formation of a central gas and stellar disc with a typical size of a few hundred parsecs connected through lanes to the ends of the stellar bar. In the lower-mass regime (M∗ < 1010 M⊙), such an inner disc is absent and the gas component exhibits a more chaotic distribution. Observations of nearby star-forming galaxies support the existence of such a change. These inner gas discs may represent... (More)
Recent hydrodynamical simulations of isolated barred disc galaxies have suggested a structural change in the distribution of the interstellar medium (ISM) around a stellar mass M∗ of 1010 M⊙. In the higher-mass regime (M∗ ≤ 1010 M⊙), we observe the formation of a central gas and stellar disc with a typical size of a few hundred parsecs connected through lanes to the ends of the stellar bar. In the lower-mass regime (M∗ < 1010 M⊙), such an inner disc is absent and the gas component exhibits a more chaotic distribution. Observations of nearby star-forming galaxies support the existence of such a change. These inner gas discs may represent an important intermediate scale connecting the large kiloparsec-scale structures with the nuclear (sub-parsec) region, transporting gas inwards to fuel the central supermassive black hole (SMBH). For this work we used an extended set of high-resolution hydrodynamical simulations of isolated disc galaxies with initial properties (i.e. stellar mass, gas fraction, stellar disc scale length, and the bulge mass fraction) with properties covering the range of galaxies in the PHANGS sample to investigate this change of regime. We studied the physical properties of the star-forming ISM in both stellar mass regimes and extracted a few physical tracers: the inner Lindblad resonance (ILR), the probability distribution function (PDF), the virial parameter, and the Mach number. In line with observations, we confirm a structure transition in the simulations that occurs between a stellar mass of 109.5 and 1010 M⊙. We show that the physical origin of this change of regime is driven by stellar feedback and its contribution relative to the underlying gravitational potential. With their shallower potential and typically higher gas mass fraction, lower-mass disc PHANGS galaxies combine two ingredients that significantly delay or even prevent the formation of a central gas (and stellar) disc. These results shed some light on the observed properties of star-forming barred galaxies and have implications for the star formation regimes, the growth of central structures, and the overall secular evolution of disc galaxies.
(Less)
- author
- organization
- publishing date
- 2025-08-01
- type
- Contribution to journal
- publication status
- published
- subject
- keywords
- Galaxies: evolution, Galaxies: spiral, Galaxies: star formation, Galaxies: structure
- in
- Astronomy and Astrophysics
- volume
- 700
- article number
- A3
- publisher
- EDP Sciences
- external identifiers
-
- scopus:105011847753
- ISSN
- 0004-6361
- DOI
- 10.1051/0004-6361/202554056
- language
- English
- LU publication?
- yes
- additional info
- Publisher Copyright: © The Authors 2025.
- id
- 2bfd6996-db76-46fd-a185-2e209afce20d
- date added to LUP
- 2025-12-12 14:56:31
- date last changed
- 2025-12-12 14:57:28
@article{2bfd6996-db76-46fd-a185-2e209afce20d,
abstract = {{<p>Recent hydrodynamical simulations of isolated barred disc galaxies have suggested a structural change in the distribution of the interstellar medium (ISM) around a stellar mass M<sub>∗</sub> of 10<sup>10</sup> M<sub>⊙</sub>. In the higher-mass regime (M<sub>∗</sub> ≤ 10<sup>10</sup> M<sub>⊙</sub>), we observe the formation of a central gas and stellar disc with a typical size of a few hundred parsecs connected through lanes to the ends of the stellar bar. In the lower-mass regime (M<sub>∗</sub> < 10<sup>10</sup> M<sub>⊙</sub>), such an inner disc is absent and the gas component exhibits a more chaotic distribution. Observations of nearby star-forming galaxies support the existence of such a change. These inner gas discs may represent an important intermediate scale connecting the large kiloparsec-scale structures with the nuclear (sub-parsec) region, transporting gas inwards to fuel the central supermassive black hole (SMBH). For this work we used an extended set of high-resolution hydrodynamical simulations of isolated disc galaxies with initial properties (i.e. stellar mass, gas fraction, stellar disc scale length, and the bulge mass fraction) with properties covering the range of galaxies in the PHANGS sample to investigate this change of regime. We studied the physical properties of the star-forming ISM in both stellar mass regimes and extracted a few physical tracers: the inner Lindblad resonance (ILR), the probability distribution function (PDF), the virial parameter, and the Mach number. In line with observations, we confirm a structure transition in the simulations that occurs between a stellar mass of 10<sup>9.5</sup> and 10<sup>10</sup> M<sub>⊙</sub>. We show that the physical origin of this change of regime is driven by stellar feedback and its contribution relative to the underlying gravitational potential. With their shallower potential and typically higher gas mass fraction, lower-mass disc PHANGS galaxies combine two ingredients that significantly delay or even prevent the formation of a central gas (and stellar) disc. These results shed some light on the observed properties of star-forming barred galaxies and have implications for the star formation regimes, the growth of central structures, and the overall secular evolution of disc galaxies.</p>}},
author = {{Verwilghen, Pierrick and Emsellem, Eric and Renaud, Florent and Agertz, Oscar and Valentini, Milena and Fraser-Mckelvie, Amelia and Meidt, Sharon and Neumann, Justus and Schinnerer, Eva and Klessen, Ralf S. and Glover, Simon C.O. and Barnes, Ashley T. and Dale, Daniel A. and Gleis, Damian R. and Smith, Rowan J. and Stuber, Sophia K. and Williams, Thomas G.}},
issn = {{0004-6361}},
keywords = {{Galaxies: evolution; Galaxies: spiral; Galaxies: star formation; Galaxies: structure}},
language = {{eng}},
month = {{08}},
publisher = {{EDP Sciences}},
series = {{Astronomy and Astrophysics}},
title = {{Simulating nearby disc galaxies on the main star formation sequence : II. The gas structure transition in low and high stellar mass discs}},
url = {{http://dx.doi.org/10.1051/0004-6361/202554056}},
doi = {{10.1051/0004-6361/202554056}},
volume = {{700}},
year = {{2025}},
}