Large-Scale Structure Formation: From the First Non-linear Objects to Massive Galaxy Clusters

Planelles, S.; Schleicher, Dominik R. G.; Bykov, A. M.

doi:10.1007/978-1-4939-3547-5_4

Cited by 7 publications

(6 citation statements)

References 314 publications

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“…In reality, both post-Newtonian and cosmological perturbations should be expected to exist in any realistic model of the Universe [36]. In this section we review and extend the two-parameter framework developed in [23] that simultaneously performs a perturbative expansion in both sectors.…”

Section: Two-parameter Perturbation Theorymentioning

confidence: 99%

Perturbation theory for cosmologies with nonlinear structure

Goldberg¹,

Gallagher²,

Clifton³

2017

Phys. Rev. D

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The next generation of cosmological surveys will operate over unprecedented scales, and will therefore provide exciting new opportunities for testing general relativity. The standard method for modelling the structures that these surveys will observe is to use cosmological perturbation theory for linear structures on horizon-sized scales, and Newtonian gravity for non-linear structures on much smaller scales. We propose a two-parameter formalism that generalizes this approach, thereby allowing interactions between large and small scales to be studied in a self-consistent and well-defined way. This uses both post-Newtonian gravity and cosmological perturbation theory, and can be used to model realistic cosmological scenarios including matter, radiation and a cosmological constant. We find that the resulting field equations can be written as a hierarchical set of perturbation equations. At leading-order, these equations allow us to recover a standard set of Friedmann equations, as well as a Newton-Poisson equation for the inhomogeneous part of the Newtonian energy density in an expanding background. For the perturbations in the large-scale cosmology, however, we find that the field equations are sourced by both non-linear and mode-mixing terms, due to the existence of small-scale structures. These extra terms should be expected to give rise to new gravitational effects, through the mixing of gravitational modes on small and large scales -effects that are beyond the scope of standard linear cosmological perturbation theory. We expect our formalism to be useful for accurately modelling gravitational physics in universes that contain non-linear structures, and for investigating the effects of non-linear gravity in the era of ultra-large-scale surveys.

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Section: Two-parameter Perturbation Theorymentioning

confidence: 99%

Perturbation theory for cosmologies with nonlinear structure

Goldberg¹,

Gallagher²,

Clifton³

2017

Phys. Rev. D

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“…On the other hand, if magnetic fields have been released by processes triggered during galaxy formation, they might have affected the transport of heat, entropy, metals and cosmic rays in forming cosmic structures (e.g. Planelles et al, 2016). Additional processes such as the "Biermannbattery" mechanism (Kulsrud et al, 1997), aperiodic plasma fluctuations in the inter-galactic plasma (Schlickeiser et al, 2012), resistive mechanisms (Miniati and Bell, 2011) or ionization fronts around the first stars (Langer et al, 2005) might provide additional amplification to the primordial fields.…”

Section: Introductionmentioning

confidence: 99%

Simulations of extragalactic magnetic fields and of their observables

Vazza

Brüggen

Gheller³

et al. 2017

Class. Quantum Grav.

136

228

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Abstract. The origin of extragalactic magnetic fields is still poorly understood. Based on a dedicated suite of cosmological magneto-hydrodynamical simulations with the ENZO code we have performed a survey of different models that may have caused present-day magnetic fields in galaxies and galaxy clusters. The outcomes of these models differ in cluster outskirts, filaments, sheets and voids and we use these simulations to find observational signatures of magnetogenesis. With these simulations, we predict the signal of extragalactic magnetic fields in radio observations of synchrotron emission from the cosmic web, in Faraday Rotation, in the propagation of Ultra High Energy Cosmic Rays, in the polarized signal from Fast Radio Bursts at cosmological distance and in spectra of distant blazars. In general, primordial scenarios in which present-day magnetic fields originate from the amplification of weak (≤ nG) uniform seed fields result more homogeneous and relatively easier to observe magnetic fields than than astrophysical scenarios, in which present-day fields are the product of feedback processes triggered by stars and active galaxies. In the near future the best evidence for the origin of cosmic magnetic fields will most likely come from a combination of synchrotron emission and Faraday Rotation observed at the periphery of large-scale structures.

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“…Galaxy clusters, characterized by deep gravitational potential wells, retain crucial information on the different physical and dynamical processes affecting their stellar, gaseous and dark matter components (see Kravtsov and Borgani 2012;Planelles et al 2016, for reviews). Therefore, a thorough understanding of the redshift evolution and the distribution of the different cluster components is essential to deepen our comprehension of observed cluster properties.…”

Section: Introductionmentioning

confidence: 99%

The origin of ICM enrichment in the outskirts of present-day galaxy clusters from cosmological hydrodynamical simulations

Biffi

Planelles

Borgani

et al. 2018

Monthly Notices of the Royal Astronomical Society

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The uniformity of the intra-cluster medium (ICM) enrichment level in the outskirts of nearby galaxy clusters suggests that chemical elements were deposited and widely spread into the intergalactic medium before the cluster formation. This observational evidence is supported by numerical findings from cosmological hydrodynamical simulations, as presented in Biffi et al. (2017), including the effect of thermal feedback from active galactic nuclei. Here, we further investigate this picture, by tracing back in time the spatial origin and metallicity evolution of the gas residing at z = 0 in the outskirts of simulated galaxy clusters. In these regions, we find a large distribution of iron abundances, including a component of highly-enriched gas, already present at z = 2. At z > 1, the gas in the present-day outskirts was distributed over tens of virial radii from the the main cluster and had been already enriched within highredshift haloes. At z = 2, about 40% of the most Fe-rich gas at z = 0 was not residing in any halo more massive than 10 11 h −1 M in the region and yet its average iron abundance was already 0.4, w.r.t. the solar value by Anders and Grevesse (1989). This confirms that the in situ enrichment of the ICM in the outskirts of present-day clusters does not play a significant role, and its uniform metal abundance is rather the consequence of the accretion of both low-metallicity and pre-enriched (at z > 2) gas, from the diffuse component and through merging substructures. These findings do not depend on the mass of the cluster nor on its core properties.

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Large-Scale Structure Formation: From the First Non-linear Objects to Massive Galaxy Clusters

Cited by 7 publications

References 314 publications

Perturbation theory for cosmologies with nonlinear structure

Perturbation theory for cosmologies with nonlinear structure

Simulations of extragalactic magnetic fields and of their observables

The origin of ICM enrichment in the outskirts of present-day galaxy clusters from cosmological hydrodynamical simulations

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