Fixing a rigorous formalism for the accurate analytic derivation of halo properties

Juan, Enric; Salvador-Solé, E.; Domènech, Guillem; Manrique, Alberto

doi:10.1093/mnras/stt2493

Cited by 15 publications

(15 citation statements)

References 28 publications

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“…(Ascasibar and Gottlo ¨ber 2008;Neto et al 2007;Brown et al 2020). Despite its importance and several proposed explanations that involve, for instance, a fundamental connection with the mass accretion history (Ludlow et al 2014(Ludlow et al , 2016, maximum entropy or adiabatic invariance arguments (Taylor and Navarro 2001;Dalal et al 2010a;Pontzen and Governato 2013;El Zant 2013;Juan et al 2014), or even the role of numerical noise as the main driver (Baushev 2015), there is not yet a consensus on the physical explanation behind this result. This is even more puzzling when contrasted with analytic predictions, which suggest single power laws as the result of gravitational collapse [see e.g., the self-similar solution of secondary infall by Bertschinger (1985)].…”

Section: Weakly-interacting Massive Particlesmentioning

confidence: 99%

Large-scale dark matter simulations

Angulo

Hahn

2022

Living Rev Comput Astrophys

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We review the field of collisionless numerical simulations for the large-scale structure of the Universe. We start by providing the main set of equations solved by these simulations and their connection with General Relativity. We then recap the relevant numerical approaches: discretization of the phase-space distribution (focusing on N-body but including alternatives, e.g., Lagrangian submanifold and Schrödinger–Poisson) and the respective techniques for their time evolution and force calculation (direct summation, mesh techniques, and hierarchical tree methods). We pay attention to the creation of initial conditions and the connection with Lagrangian Perturbation Theory. We then discuss the possible alternatives in terms of the micro-physical properties of dark matter (e.g., neutralinos, warm dark matter, QCD axions, Bose–Einstein condensates, and primordial black holes), and extensions to account for multiple fluids (baryons and neutrinos), primordial non-Gaussianity and modified gravity. We continue by discussing challenges involved in achieving highly accurate predictions. A key aspect of cosmological simulations is the connection to cosmological observables, we discuss various techniques in this regard: structure finding, galaxy formation and baryonic modelling, the creation of emulators and light-cones, and the role of machine learning. We finalise with a recount of state-of-the-art large-scale simulations and conclude with an outlook for the next decade.

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Section: Weakly-interacting Massive Particlesmentioning

confidence: 99%

Large-scale dark matter simulations

Angulo

Hahn

2022

Living Rev Comput Astrophys

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“…AMIGA follows this growth in a well-contrasted analytic manner with no free parameters (Salvador-Solé et al 1998, 2007Raig et al 2001). This allows us to accurately calculate, at any given moment, their abundance (Juan et al 2014a(Juan et al , 2014b and inner structure and kinematics (Salvador-Solé et al 2012a, which in turn sets the structure and temperature of their hot gas (Solanes et al 2005). The amount and metallicity of such a hot gas and the properties of the central galaxy and its satellites are monitored in AMIGA from the individual halo aggregation history.…”

Section: Luminous Sourcesmentioning

confidence: 99%

CONSTRAINING THE EPOCH OF REIONIZATION FROM THE OBSERVED PROPERTIES OF THE HIGH-z UNIVERSE

Salvador-Solé

Manrique

Guzmán

et al. 2016

ApJ

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We combine observational data on a dozen independent cosmic properties at high-z with the information on reionization drawn from the spectra of distant luminous sources and the cosmic microwave background (CMB) to constrain the interconnected evolution of galaxies and the intergalactic medium since the dark ages. The only acceptable solutions are concentrated in two narrow sets. In one of them reionization proceeds in two phases: a first one driven by Population III stars, completed atz 10, and after a short recombination period a second one driven by normal galaxies, completed atz 6. In the other set both kinds of sources work in parallel until full reionization atz 6. The best solution with double reionization gives excellent fits to all the observed cosmic histories, but the CMB optical depth is 3σ larger than the recent estimate from the Planck data. Alternatively, the best solution with single reionization gives less good fits to the observed star formation rate density and cold gas mass density histories, but the CMB optical depth is consistent with that estimate. We make several predictions, testable with future observations, that should discriminate between the two reionization scenarios. As a byproduct our models provide a natural explanation to some characteristic features of the cosmic properties at high-z, as well as to the origin of globular clusters.

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“…There is a one-to-one correspondence between virialized haloes with mass M at the cosmic time t and non-nested peaks with density contrast δ at the scale S in the Gaussian-filtered Gaussian random density field at an arbitrary initial time t i given by (Juan et al 2014a )…”

Section: Haloes and Peaks (I) Halo-peak Correspondencementioning

confidence: 99%

“…CUSP makes the link between haloes and their seeds, peaks (or maxima), in the primordial Gaussian random field of density perturbations in any given hierarchical cosmology (Juan et al 2014a ). Thus, following the collapse and virialization of those seeds, with well-known properties according to Gaussian statistics, one can accurately derive from first principles and with no single free parameter the properties of virialized haloes.…”

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confidence: 99%

An accurate comprehensive approach to substructure – I. Accreted subhaloes

Salvador-Solé

Manrique

Botella

2021

Monthly Notices of the Royal Astronomical Society

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This is the first of a series of three Papers devoted to the study of halo substructure in hierarchical cosmologies by means of the CUSP formalism. In the present Paper we derive the properties of subhaloes and diffuse dark matter (dDM) accreted onto haloes and their progenitors. Specifically, we relate the dDM present at any time in the inter-halo medium of the real Universe or a cosmological simulation with the corresponding free-streaming mass or the halo resolution mass, respectively, and establish the link between subhaloes and their seeds in the initial density field. By monitoring the collapse and virialisation of haloes, we derive from first principles and with no single free parameter the abundance and radial distribution of dDM and subhaloes accreted onto them. Our predictions are in excellent agreement with the results of simulations, but for the predicted fraction of accreted dDM, which is larger than reported in previous works as they only count the dDM accreted onto the final halo, not onto its progenitors. The derivation pursued here clarifies the origin of some key features of substructure. Overall, our results demonstrate that CUSP is a powerful tool for understanding halo substructure and extending the results of simulations to haloes with arbitrary masses, redshifts and formation times in any hierarchical cosmology endowed with random Gaussian density perturbations.

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Fixing a rigorous formalism for the accurate analytic derivation of halo properties

Cited by 15 publications

References 28 publications

Large-scale dark matter simulations

Large-scale dark matter simulations

CONSTRAINING THE EPOCH OF REIONIZATION FROM THE OBSERVED PROPERTIES OF THE HIGH-z UNIVERSE

An accurate comprehensive approach to substructure – I. Accreted subhaloes

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