Hydrodynamical simulations of coupled and uncoupled quintessence models – II. Galaxy clusters

Carlesi, Edoardo; Knebe, Alexander; Lewis, Geraint F.; Yepes, Gustavo

doi:10.1093/mnras/stu151

Cited by 17 publications

(12 citation statements)

References 76 publications

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“…Simulation-based investigations beyond spin-alignment have also proven useful in drawing distinctions between ΛCDM and alternative models: Carlesi et al (2014a) finds, using hydrodynamical simulations, that a self-interacting quintessence model provides a higher concentration of haloes within the LSS as compared to their fiducial ΛCDM and other cosmologies compared. Carlesi et al (2014b) find a weak coupling between the spin, triaxiality and virialisation and the cosmology dark sector types. Although Elahi et al (2015) shows little to no difference between ΛCDM and the coupled cosmologies judging by the lack of systematic differences between spin parameter and satellite alignment distributions across cosmologies.…”

Section: Introductionmentioning

confidence: 79%

Cosmological signatures of dark sector physics: the evolution of haloes and spin alignment

Jibrail

Elahi

Lewis

2020

Monthly Notices of the Royal Astronomical Society

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The standard cosmological paradigm currently lacks a detailed account of physics in the dark sector, the dark matter and energy that dominate cosmic evolution. In this paper, we consider the distinguishing factors between three alternative models -warm dark matter, quintessence and coupled dark matter-energy -and ΛCDM through numerical simulations of cosmological structure formation. Key halo statistics -halo spin/velocity alignment between large-scale structure and neighboring haloes, halo formation time and migration -were compared across cosmologies within the redshift range 0≤z≤2.98. We found the alignment of halo motion and spin to large-scale structures and neighbouring haloes to be similar in all cosmologies for a range of redshifts. The search was extended to low density regions, avoiding non-linear disturbances of halo spins, yet very similar alignment trends were found between cosmologies which are difficult to characterize and use as a probe of cosmology. We found haloes in quintessence cosmologies form earlier than their ΛCDM counterparts. Relating this to the fact that such haloes originate in high density regions, such findings could hold clues to distinguishing factors for the quintessence cosmology from the standard model. Although in general, halo statistics are not an accurate probe of the dark sector physics.

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Section: Introductionmentioning

confidence: 79%

Cosmological signatures of dark sector physics: the evolution of haloes and spin alignment

Jibrail

Elahi

Lewis

2020

Monthly Notices of the Royal Astronomical Society

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“…To compute the potential energy, we use weak lensing observational fittings of NFW profiles. These fittings, justified by the observers confidence in their reliability (Okabe et al 2010;Ettori et al 2013), are further vindicated by interacting DE models from simulations (e. g. Baldi et al 2010;Carlesi et al 2014) which all agree with the NFW shape. We want to have all NFW profiles parametrised by M 200 and c. In general, within a radius r ∆ , i.e.…”

Section: Uniforming the Nfw Profilesmentioning

confidence: 94%

Non-virialized clusters for detection of dark energy–dark matter interaction

Delliou

Marcondes

Neto

et al. 2015

Mon. Not. R. Astron. Soc.

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The observation of galaxy and gas distributions, as well as cosmological simulations in a ΛCDM Universe, suggests that clusters of galaxies are still accreting mass and are not expected to be in equilibrium. In this work, we investigate the possibility to evaluate the departure from virial equilibrium in order to detect, in that balance, effects from a Dark Matter-Dark Energy interaction. We continue, from previous works, using a simple model of interacting dark sector, the Layzer-Irvine equation for dynamical virial evolution, and employ optical observations in order to obtain the mass profiles through weak lensing and X-ray observations giving the intracluster gas temperatures. Through a Monte Carlo method, we generate, for a set of clusters, measurements of observed virial ratios, interaction strength, rest virial ratio and departure from equilibrium factors. We found a compounded interaction strength of −1.99 +2.56 −16.00 , compatible with no interaction, but also a compounded rest virial ratio of −0.79 ± 0.13, which would entail a 2σ detection. We confirm quantitatively that clusters of galaxies are out of equilibrium but further investigation is needed to constrain a possible interaction in the dark sector.

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“…More recently, Carlesi et al. ( 2014a , b ) have employed a specific suite of high-resolution N -body simulations to investigate how some of the above mentioned effects depend on the cosmic environment in which CDM halos reside, showing that most of the characteristic observational features of interacting dark energy are significantly enhanced for halo populations residing in underdense regions of the Universe. Furthermore, Carlesi et al.…”

Section: Part I Dark Energymentioning

confidence: 99%

Cosmology and fundamental physics with the Euclid satellite

Amendola¹,

Appleby²,

Avgoustidis³

et al. 2018

Living Rev Relativ

936

869

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Euclid is a European Space Agency medium-class mission selected for launch in 2020 within the cosmic vision 2015–2025 program. The main goal of Euclid is to understand the origin of the accelerated expansion of the universe. Euclid will explore the expansion history of the universe and the evolution of cosmic structures by measuring shapes and red-shifts of galaxies as well as the distribution of clusters of galaxies over a large fraction of the sky. Although the main driver for Euclid is the nature of dark energy, Euclid science covers a vast range of topics, from cosmology to galaxy evolution to planetary research. In this review we focus on cosmology and fundamental physics, with a strong emphasis on science beyond the current standard models. We discuss five broad topics: dark energy and modified gravity, dark matter, initial conditions, basic assumptions and questions of methodology in the data analysis. This review has been planned and carried out within Euclid’s Theory Working Group and is meant to provide a guide to the scientific themes that will underlie the activity of the group during the preparation of the Euclid mission.

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Hydrodynamical simulations of coupled and uncoupled quintessence models – II. Galaxy clusters

Cited by 17 publications

References 76 publications

Cosmological signatures of dark sector physics: the evolution of haloes and spin alignment

Cosmological signatures of dark sector physics: the evolution of haloes and spin alignment

Non-virialized clusters for detection of dark energy–dark matter interaction

Cosmology and fundamental physics with the Euclid satellite

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