The Schrödinger-Poisson method for Large-Scale Structure

Garny, Mathias; Konstandin, Thomas; Rubira, Henrique

doi:10.1088/1475-7516/2020/04/003

Cited by 23 publications

(12 citation statements)

References 64 publications

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“…For this reason, the Schro ¨dinger-Poisson analogue has the advantage that it provides a full phase space theory with only a threedimensional field (the wave function) that needs to be evolved. Following the first implementation by Widrow and Kaiser (1993), this model has found renewed interest recently (Uhlemann et al 2014;Schaller et al 2014;Kopp et al 2017;Eberhardt et al 2020;Garny et al 2020). It is important to note that the underlying equations are identical to those of 'fuzzy dark matter' (FDM) models of ultralight axion-like particles, which we discuss in more detail in Sect.…”

Section: Schro ¨Dinger-poisson As a Discretisation Of Vlasov-poissonmentioning

confidence: 96%

Large-scale dark matter simulations

Angulo

Hahn

2022

Living Rev Comput Astrophys

111

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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: Schro ¨Dinger-poisson As a Discretisation Of Vlasov-poissonmentioning

confidence: 96%

Large-scale dark matter simulations

Angulo

Hahn

2022

Living Rev Comput Astrophys

111

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“…The wave description effectively reshuffles information in a phase-space Boltzmann distribution into a position-space wavefunction. It offers a number of insights that might otherwise be obscure (Uhlemann et al 2014, Garny et al 2020.…”

Section: Wave Dynamics and Phenomenologymentioning

confidence: 99%

Wave Dark Matter

Hui

2021

Preprint

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We review the physics and phenomenology of wave dark matter: a bosonic dark matter candidate lighter than about 30 eV. Such particles have a de Broglie wavelength exceeding the average inter-particle separation in a galaxy like the Milky Way, thus well described as a set of classical waves. We outline the particle physics motivations for them, including the QCD axion as well as ultra-light axion-like-particles such as fuzzy dark matter. The wave nature of the dark matter implies a rich phenomenology:• Wave interference gives rise to order unity density fluctuations on de Broglie scale in halos. One manifestation is vortices where the density vanishes and around which the velocity circulates. There is one vortex ring per de Broglie volume on average. • For sufficiently low masses, soliton condensation occurs at centers of halos. The soliton oscillates and random walks, another manifestation of wave interference. The halo and subhalo abundance is expected to be suppressed at small masses, but the precise prediction from numerical wave simulations remains to be determined. • For ultra-light ∼ 10 −22 eV dark matter, the wave interference substructures can be probed by tidal streams/gravitational lensing. The signal can be distinguished from that due to subhalos by the dependence on stream orbital radius/image separation. • Axion detection experiments are sensitive to interference substructures for wave dark matter that is moderately light. The stochastic nature of the waves affects the interpretation of experimental constraints and motivates the measurement of correlation functions.Current constraints and open questions, covering detection experiments and cosmological/galactic/black-hole observations, are discussed.

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“…So one can simulate either one of those models using these system of equations 43 . For the simulation that solve the Schrödinger-Poisson equations, also called wave simulations, there are many groups that are attempting to solve this system using different methods (Schive et al 2014a;Schwabe et al 2016;Mocz et al 2017Mocz et al , 2018Edwards et al 2018;Garny et al 2020). In general, this approach is very good to describe the small-scales, being able to resolve the small structures and taking into account the wave nature of the condensate, as we can see in the left panel of Fig.…”

Section: Schrödinger-poissonmentioning

confidence: 99%

Ultra-light dark matter

Ferreira

2021

Astron Astrophys Rev

259

126

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Ultra-light dark matter is a class of dark matter models (DM), where DM is composed by bosons with masses ranging from $$10^{-24}\, \mathrm {eV}< m < \mathrm {eV}$$ 10 - 24 eV < m < eV . These models have been receiving a lot of attention in the past few years given their interesting property of forming a Bose–Einstein condensate (BEC) or a superfluid on galactic scales. BEC and superfluidity are some of the most striking quantum mechanical phenomena that manifest on macroscopic scales, and upon condensation, the particles behave as a single coherent state, described by the wavefunction of the condensate. The idea is that condensation takes place inside galaxies while outside, on large scales, it recovers the successes of $$\varLambda $$ Λ CDM. This wave nature of DM on galactic scales that arise upon condensation can address some of the curiosities of the behaviour of DM on small-scales. There are many models in the literature that describe a DM component that condenses in galaxies. In this review, we are going to describe those models, and classify them into three classes, according to the different non-linear evolution and structures they form in galaxies: the fuzzy dark matter (FDM), the self-interacting fuzzy dark matter (SIFDM), and the DM superfluid. Each of these classes comprises many models, each presenting a similar phenomenology in galaxies. They also include some microscopic models like the axions and axion-like particles. To understand and describe this phenomenology in galaxies, we are going to review the phenomena of BEC and superfluidity that arise in condensed matter physics, and apply this knowledge to DM. We describe how ULDM can potentially reconcile the cold DM picture with the small-scale behaviour. These models present a rich phenomenology that is manifest in different astrophysical consequences. We review here the astrophysical and cosmological tests used to constrain those models, together with new and future observations that promise to test these models in different regimes. For the case of the FDM class, the mass where this model has an interesting phenomenology on small-scales $$ \sim 10^{-22}\, \mathrm {eV}$$ ∼ 10 - 22 eV , is strongly challenged by current observations. The parameter space for the other two classes remains weakly constrained. We finalize by showing some predictions that are a consequence of the wave nature of this component, like the creation of vortices and interference patterns, that could represent a smoking gun in the search of these rich and interesting alternative class of DM models.

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The Schrödinger-Poisson method for Large-Scale Structure

Cited by 23 publications

References 64 publications

Large-scale dark matter simulations

Large-scale dark matter simulations

Wave Dark Matter

Ultra-light dark matter

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