NIHAO – IV: core creation and destruction in dark matter density profiles across cosmic time

We use the NIHAO (Numerical Investigation of Hundred Astrophysical Objects) cosmological simulations to investigate the effects of baryonic physics on the time evolution of dark matter central density profiles. The sample is made of ≈70 independent high-resolution hydrodynamical simulations of galax...

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Bibliographic Details
Published in:Monthly notices of the Royal Astronomical Society 2016-03, Vol.456 (4), p.3542-3552
Main Authors: Tollet, Edouard, Macciò, Andrea V., Dutton, Aaron A., Stinson, Greg S., Wang, Liang, Penzo, Camilla, Gutcke, Thales A., Buck, Tobias, Kang, Xi, Brook, Chris, Di Cintio, Arianna, Keller, Ben W., Wadsley, James
Format: Article
Language:English
Subjects:
Astronomy
Astrophysics
Computer simulation
Dark matter
Density
Dwarf galaxies
Galactic halos
Galaxy formation
Halos
M stars
Physics
Simulation
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Summary:We use the NIHAO (Numerical Investigation of Hundred Astrophysical Objects) cosmological simulations to investigate the effects of baryonic physics on the time evolution of dark matter central density profiles. The sample is made of ≈70 independent high-resolution hydrodynamical simulations of galaxy formation and covers a wide mass range: 1010 ≲ M halo/M⊙ ≲ 1012, i.e. from dwarfs to L ⋆. We confirm previous results on the dependence of the inner dark matter density slope, α, on the ratio between stellar-to-halo mass, M star/M halo. We show that this relation holds approximately at all redshifts (with an intrinsic scatter of ∼0.18 in α measured between 1 and 2 per cent of the virial radius). This implies that in practically all haloes the shape of their inner density profile changes quite substantially over cosmic time, as they grow in stellar and total mass. Thus, depending on their final M star/M halo ratio, haloes can either form and keep a substantial density core (R core ∼ 1 kpc), or form and then destroy the core and recontract the halo, going back to a cuspy profile, which is even steeper than cold-dark-matter predictions for massive galaxies (1012 M⊙). We show that results from the NIHAO suite are in good agreement with recent observational measurements of α in dwarf galaxies. Overall our results suggest that the notion of a universal density profile for dark matter haloes is no longer valid in the presence of galaxy formation.
ISSN:0035-8711
1365-2966
DOI:10.1093/mnras/stv2856