The impact of galactic feedback on the shapes of dark matter haloes

Author:

Chua Kun Ting Eddie1ORCID,Vogelsberger Mark2ORCID,Pillepich Annalisa3ORCID,Hernquist Lars4

Affiliation:

1. Institute of High Performance Computing , 1 Fusionopolis Way, 138632, Singapore

2. Department of Physics, Massachusetts Institute of Technology , 77 Massachusetts Avenue, Cambridge, MA 02139, USA

3. Max-Planck-Institut für Astronomie , Königstuhl 17, D-69117 Heidelberg, Germany

4. Harvard-Smithsonian Center for Astrophysics , 60 Garden Street, Cambridge, MA 02138, USA

Abstract

ABSTRACT We quantify the impact of galaxy formation on dark matter halo shapes using cosmological simulations at redshift z = 0. Using magnetohydrodynamic simulations from the IllustrisTNG project, we focus on haloes of mass $10^{10\!-\!14} \, \rm M_{\odot }$ from the 50 Mpc (TNG50) and 100 Mpc (TNG100) boxes and compare them to dark matter-only (DMO) analogues and other simulations, e.g. Numerical Investigation of a Hundred Astrophysical Objects (NIHAO) and Evolution and Assembly of GaLaxies and their Environments (EAGLE). We further quantify the prediction uncertainty by varying the feedback models using smaller 25 ${\rm Mpc}\, h^{-1}$ boxes. We find that (i) galaxy formation results in rounder haloes compared to DMO simulations, in qualitative agreement with past results. Haloes of mass ${\approx }2\times 10^{12} \, \rm M_{\odot }$ are most spherical, with an average minor-to-major axial ratio of $\langle s \rangle$ ≈ 0.75 in the inner halo, an increase of 40 per cent compared to their DMO counterparts. No significant difference is present for low-mass $10^{10} \, \rm M_{\odot }$ haloes; (ii) stronger feedback, e.g. increasing galactic wind speed, reduces the impact of baryons; (iii) the inner halo shape correlates with the stellar mass fraction, explaining the dependence of halo shapes on feedback models; and (iv) the fiducial and weaker feedback models are most consistent with observational estimates of the Milky Way halo shape. At fixed halo mass, very diverse and possibly unrealistic feedback models all predict inner shapes closer to one another than to the DMO results. Because of the large halo-to-halo variation in halo shape, a larger observational sample is required to statistically distinguish different baryonic prescriptions.

Funder

NASA

NSF

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

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1. How do baryonic effects on the cosmic matter distribution vary with scale and local density environment?;Monthly Notices of the Royal Astronomical Society;2024-01-23

2. A differentiable model of the evolution of dark matter halo concentration;Monthly Notices of the Royal Astronomical Society;2023-09-20

3. Shaping the unseen: the influence of baryons and environment on low-mass, high-redshift dark matter haloes in the SIEGE simulations;Monthly Notices of the Royal Astronomical Society;2023-09-12

4. EDGE: the shape of dark matter haloes in the faintest galaxies;Monthly Notices of the Royal Astronomical Society;2023-08-21

5. Baryonic imprints on DM haloes: the concentration–mass relation in the C amels simulations;Monthly Notices of the Royal Astronomical Society;2023-06-01

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