NIHAO - IV

Core creation and destruction in dark matter density profiles across cosmic time

Edouard Tollet, Andrea Maccio, Aaron A. Dutton, Greg S. Stinson, Liang Wang, Camilla Penzo, Thales A. Gutcke, Tobias Buck, Xi Kang, Chris Brook, Arianna Di Cintio, Ben W. Keller, James Wadsley

Research output: Contribution to journalArticle

Abstract

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 ≲ Mhalo/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, Mstar/Mhalo. 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 Mstar/Mhalo ratio, haloes can either form and keep a substantial density core (Rcore ~ 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 Overall our results suggest that the notion of a universal density profile for dark matter haloes is no longer valid in the presence of galaxy formation.

Original languageEnglish (US)
Pages (from-to)3542-3552
Number of pages11
JournalMonthly Notices of the Royal Astronomical Society
Volume456
Issue number4
DOIs
StatePublished - Jan 9 2016

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destruction
halos
dark matter
astrophysics
profiles
galactic evolution
dwarf galaxies
stellar mass
simulation
physics
slopes
galaxies
radii
high resolution
prediction
predictions

Keywords

  • Dark matter
  • Galaxies: Evolution
  • Hydrodynamics

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

NIHAO - IV : Core creation and destruction in dark matter density profiles across cosmic time. / Tollet, Edouard; Maccio, Andrea; 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.

In: Monthly Notices of the Royal Astronomical Society, Vol. 456, No. 4, 09.01.2016, p. 3542-3552.

Research output: Contribution to journalArticle

Tollet, E, Maccio, A, Dutton, AA, Stinson, GS, Wang, L, Penzo, C, Gutcke, TA, Buck, T, Kang, X, Brook, C, Di Cintio, A, Keller, BW & Wadsley, J 2016, 'NIHAO - IV: Core creation and destruction in dark matter density profiles across cosmic time', Monthly Notices of the Royal Astronomical Society, vol. 456, no. 4, pp. 3542-3552. https://doi.org/10.1093/mnras/stv2856
Tollet, Edouard ; Maccio, Andrea ; 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. / NIHAO - IV : Core creation and destruction in dark matter density profiles across cosmic time. In: Monthly Notices of the Royal Astronomical Society. 2016 ; Vol. 456, No. 4. pp. 3542-3552.
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AU - Maccio, Andrea

AU - Dutton, Aaron A.

AU - Stinson, Greg S.

AU - Wang, Liang

AU - Penzo, Camilla

AU - Gutcke, Thales A.

AU - Buck, Tobias

AU - Kang, Xi

AU - Brook, Chris

AU - Di Cintio, Arianna

AU - Keller, Ben W.

AU - Wadsley, James

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AB - 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 ≲ Mhalo/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, Mstar/Mhalo. 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 Mstar/Mhalo ratio, haloes can either form and keep a substantial density core (Rcore ~ 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.

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