Strongly coupled dark energy cosmologies: preserving ΛCDM success and easing low-scale problems – II. Cosmological simulations

Macciò, Andrea V.; Mainini, Roberto; Penzo, Camilla; Bonometto, S. A.

doi:10.1093/mnras/stv1680

Cited by 37 publications

(36 citation statements)

References 77 publications

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“…The discovery of a flat dark matter distribution will then be an indication of a different nature for dark matter: warm (but see Macciò et al 2012a), self interacting (Vogelsberger et al 2014b;Elbert et al 2015) or even more exotic models (e.g. Macciò et al 2015). Figure 11.…”

Section: Evolution Of the Dark Matter Profilementioning

confidence: 99%

The edge of galaxy formation – II. Evolution of Milky Way satellite analogues after infall

Frings

Macciò

Buck

et al. 2017

Monthly Notices of the Royal Astronomical Society

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In the first paper we presented 27 hydrodynamical cosmological simulations of galaxies with total masses between 5 × 10 8 and 10 10 M . In this second paper we use a subset of these cosmological simulations as initial conditions (ICs) for more than forty hydrodynamical simulations of satellite and host galaxy interaction. Our cosmological ICs seem to suggest that galaxies on these mass scales have very little rotational support and are velocity dispersion (σ) dominated. Accretion and environmental effects increase the scatter in the galaxy scaling relations (e.g. size -velocity dispersion) in very good agreement with observations. Star formation is substantially quenched after accretion. Mass removal due to tidal forces has several effects: it creates a very flat stellar velocity dispersion profiles, and it reduces the dark matter content at all scales (even in the centre), which in turn lowers the stellar velocity on scales around 0.5 kpc even when the galaxy does not lose stellar mass. Satellites that start with a cored dark matter profile are more prone to either be destroyed or to end up in a very dark matter poor galaxy. Finally, we found that tidal effects always increase the "cuspyness" of the dark matter profile, even for haloes that infall with a core.

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Section: Evolution Of the Dark Matter Profilementioning

confidence: 99%

The edge of galaxy formation – II. Evolution of Milky Way satellite analogues after infall

Frings

Macciò

Buck

et al. 2017

Monthly Notices of the Royal Astronomical Society

Self Cite

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“…DM halos, despite their being balanced as a whole not by rotation but by velocity dispersion, can have non-zero integral angular momentum. Analysis of various non-dissipative cosmological simulations suggests that more 'spherical' halos rotate significantly slower than non-spherical ones (see, e.g., papers [182,191] and Fig. 23).…”

Section: Halo Form From Numerical Modelsmentioning

confidence: 99%

Dark matter in galaxies

Засов¹,

Saburova²,

Хоперсков³

et al. 2017

Phys.-Usp.

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Dark matter in galaxies, its abundance, and its distribution remain a subject of long-standing discussion, especially in view of the fact that neither dark matter particles nor dark matter bodies have yet been found. Experts' opinions range from a very large number of completely dark galaxies exist to nonbaryonic dark matter does not exist at all in any significant amounts. We discuss astronomical evidence for the existence of dark matter and its connection with visible matter and examine attempts to estimate its mass and distribution in galaxies from photometry, dynamics, gravitational lensing, and other observations (the cosmological aspects of the existence of dark matter are not considered in this review). In our view, the presence of dark matter in and around galaxies is a well-established fact. We conclude with an overview of mechanisms by which a dark halo can influence intragalactic processes.Comment: 82 pages, 35 figure

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“…Macciò et al 2015). Alternatively, it could simply mean that baryonic processes play a key role in shaping the inner parts of halos and galaxies.…”

Section: Introductionmentioning

confidence: 99%

Density profile of dark matter haloes and galaxies in the horizon–agn simulation: the impact of AGN feedback

Peirani

Dubois

Volonteri

et al. 2017

Monthly Notices of the Royal Astronomical Society

148

141

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Using a suite of three large cosmological hydrodynamical simulations, HORIZON-AGN, HORIZON-NOAGN (no AGN feedback) and HORIZON-DM (no baryons), we investigate how a typical sub-grid model for AGN feedback affects the evolution of the inner density profiles of massive dark matter haloes and galaxies. Based on direct object-to-object comparisons, we find that the integrated inner mass and density slope differences between objects formed in these three simulations (hereafter, H AGN , H noAGN and H DM ) significantly evolve with time. More specifically, at high redshift (z ∼ 5), the mean central density profiles of H AGN and H noAGN dark matter haloes tend to be much steeper than their H DM counterparts owing to the rapidly growing baryonic component and ensuing adiabatic contraction. By z ∼ 1.5, these mean halo density profiles in H AGN have flattened, pummelled by powerful AGN activity ("quasar mode"): the integrated inner mass difference gaps with H noAGN haloes have widened, and those with H DM haloes have narrowed. Fast forward 9.5 billion years, down to z = 0, and the trend reverses: H AGN halo mean density profiles drift back to a more cusped shape as AGN feedback efficiency dwindles ("radio mode"), and the gaps in integrated central mass difference with H noAGN and H DM close and broaden respectively. On the galaxy side, the story differs noticeably. Averaged stellar profile central densities and inner slopes are monotonically reduced by AGN activity as a function of cosmic time, resulting in better agreement with local observations.

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Strongly coupled dark energy cosmologies: preserving ΛCDM success and easing low-scale problems – II. Cosmological simulations

Cited by 37 publications

References 77 publications

The edge of galaxy formation – II. Evolution of Milky Way satellite analogues after infall

The edge of galaxy formation – II. Evolution of Milky Way satellite analogues after infall

Dark matter in galaxies

Density profile of dark matter haloes and galaxies in the horizon–agn simulation: the impact of AGN feedback

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