The diversity of rotation curves of galaxies in the <scp>NewHorizon</scp> cosmological simulation

ABSTRACT We use the cosmological hydrodynamical simulation NewHorizon to study the effects of the baryonic component on the inner mass profile of dark matter haloes of isolated galaxies ($10^6&amp;lt; M_*/\mathrm{ M}_\odot &amp;lt; 10^{11.5}$). Dark matter deficits (‘cores’) develop only in galaxies in a narrow range of stellar mass, $5\times 10^7&amp;lt; M_*/\mathrm{ M}_\odot &amp;lt; 3\times 10^9$. The lower stellar mass limit arises because a minimum amount of star formation is required to drive the baryonic outflows that redistribute dark matter and create a core. The upper limit roughly coincides with the total amount of dark matter initially contained within the innermost 2 kpc ($1 \pm 0.5 \times 10^{9}\, \mathrm{ M}_\odot$), which roughly coincides with the stellar half-mass radius of these dwarfs. This enclosed mass is quite insensitive to the total virial mass of the system. The same upper limit applies to other simulations, like NIHAO and EAGLE-CHT10, despite their rather different galaxy formation efficiencies. This suggests that it is the galaxy total stellar mass that determines when a core is formed, and not the galaxy-to-dark halo mass ratio, as argued in earlier work. This is consistent with a back-of-the-envelope estimate for a SN-induced rate of orbital diffusion. Although NewHorizon dwarfs reproduce the observed diversity of rotation curves better than other simulations, there are significant differences in the gravitational importance of baryons in the inner regions of dwarfs compared to observations. These differences prevent us from concluding that cosmological simulations are currently fully able to account for the observed diversity of rotation curve shapes.

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Journal
Monthly Notices of the Royal Astronomical Society
Published
2025-04-24
DOI
https://doi.org/10.1093/mnras/staf667
Primary Topic
Astronomy and Astrophysical Research
Type
article
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0.00

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article

The diversity of rotation curves of galaxies in the NewHorizon cosmological simulation

Julio F. Navarro, Julien Devriendt, Christophe Pichon, Sugata Kaviraj et al.
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Monthly Notices of the Royal Astronomical Society
Astronomy and Astrophysical Research
article

The diversity of rotation curves of galaxies in the NewHorizon cosmological simulation

Julio F. Navarro, Julien Devriendt, Christophe Pichon, Sugata Kaviraj, Taysun Kimm, Adrianne D. Slyz, Sébastien Peirani, Sukyoung K. Yi, Isabel Santos-Santos, R. A. JACKSON, M. Volonteri, Yohan Dubois, Katarina Kraljic, Garreth Martin
article en

Abstract

ABSTRACT We use the cosmological hydrodynamical simulation NewHorizon to study the effects of the baryonic component on the inner mass profile of dark matter haloes of isolated galaxies ($10^6&amp;lt; M_*/\mathrm{ M}_\odot &amp;lt; 10^{11.5}$). Dark matter deficits (‘cores’) develop only in galaxies in a narrow range of stellar mass, $5\times 10^7&amp;lt; M_*/\mathrm{ M}_\odot &amp;lt; 3\times 10^9$. The lower stellar mass limit arises because a minimum amount of star formation is required to drive the baryonic outflows that redistribute dark matter and create a core. The upper limit roughly coincides with the total amount of dark matter initially contained within the innermost 2 kpc ($1 \pm 0.5 \times 10^{9}\, \mathrm{ M}_\odot$), which roughly coincides with the stellar half-mass radius of these dwarfs. This enclosed mass is quite insensitive to the total virial mass of the system. The same upper limit applies to other simulations, like NIHAO and EAGLE-CHT10, despite their rather different galaxy formation efficiencies. This suggests that it is the galaxy total stellar mass that determines when a core is formed, and not the galaxy-to-dark halo mass ratio, as argued in earlier work. This is consistent with a back-of-the-envelope estimate for a SN-induced rate of orbital diffusion. Although NewHorizon dwarfs reproduce the observed diversity of rotation curves better than other simulations, there are significant differences in the gravitational importance of baryons in the inner regions of dwarfs compared to observations. These differences prevent us from concluding that cosmological simulations are currently fully able to account for the observed diversity of rotation curve shapes.

Monthly Notices of the Royal Astronomical SocietyVol. 539(4)
Korea Institute for Advanced Study (KR), Centre National de la Recherche Scientifique (FR), University of Arizona (US), University of Hertfordshire (GB), University of Nottingham (GB), Kavli Institute for the Physics and Mathematics of the Universe (JP), Durham University (GB), Yonsei University (KR), University of Victoria (CA), Korea Astronomy and Space Science Institute (KR), Institut d'Astrophysique de Paris (FR), Observatoire astronomique de Strasbourg (FR), Sorbonne Université (FR), University of Oxford (GB), Université de Strasbourg (FR), The University of Tokyo (JP)
National Science Foundation, National Research Foundation, Agence Nationale de la Recherche, Korea Institute of Science and Technology Information, National Research Foundation of Korea, Grand Équipement National De Calcul Intensif, Korea Research Environment Open Network, Science and Technology Facilities Council
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