Galaxy formation with BECDM – I. Turbulence and relaxation of idealized haloes

Mocz, Philip; Vogelsberger, Mark; Robles, Victor H.; Zavala, Jesús; Boylan-Kolchin, Michael; Fialkov, Anastasia; Hernquist, Lars

doi:10.1093/mnras/stx1887

Cited by 318 publications

(421 citation statements)

References 93 publications

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“…Using analytic tools, Hu, Barkana & Gruzinov (2000) showed that perturbations grow linearly on scales much larger than the Jeans scale at equality, kJeq = 9 m/10 −22 eV 1/2 Mpc −1 , but oscillate on smaller scales leading to a suppression of clustering power and the subsequent deficit of dwarf galaxies. BECDMonly numerical simulations confirmed this picture: modestresolution simulations verified the suppression of low-mass haloes (Woo & Chiueh 2009), while higher resolution simulations characterized the formation of solitonic cores (e.g., Schwabe, Niemeyer & Engels 2016a;Mocz et al 2017); although, we remark that these simulations did not use self-consistent initial conditions predicted by the BECDM model (Hlozek et al 2015), but artificial ones instead to highlight/exaggerate growth of structure. Simulations with WDM, although ignoring the quantum effects of BECDM, also serve as a guideline for understanding structure formation in BECDM.…”

Section: Introductionmentioning

confidence: 77%

“…Here we outline the advantages and disadvantages of different methods (spectral, adaptive grid finite difference, and SPH and mesh-free finite-volume methods for the Madelung formulation). Spectral methods are an ideal choice for the Schrödinger-Poisson equations, owing to the smoothness of the wavefunction, and the unitary nature of the discretization (Mocz et al 2017). Spectral accuracy allows for machine-precision control of spatial truncation errors.…”

Section: Discussion Of Various Numerical Approaches For Becdm and Thementioning

confidence: 99%

“…The spectral method proves to be useful at capturing interference patterns and vortex lines, which turn out to be an integral feature of filaments and haloes in these cosmological simulations (Mocz et al 2017). Vortex lines are locations where the density ρ = 0, but are sites of quantized vorticity in the fluid (the rest of the fluid is vortex free, as ∇ × vM = 0 since the velocity is the gradient of a scalarthe phase).…”

Section: Spectral Methodsmentioning

confidence: 99%

“…Hence baryonic physics coupled to the dark matter converges to classical CDM behavior as well in the limit /m → 0. On smaller scales, the SP system is expected to show quantum wave phenomena, such as soliton cores (stable, ground-state eigenmodes where the uncertainty principal/quantum potential opposes the gravitational collapse; , vortex lines and reconnection (Mocz et al 2017), interference patterns, quantum tunneling, and non-classical phenomena if there exist jumps in the wavefunction phase (e.g., colliding cores can bounce off each other; Schwabe, Niemeyer & Engels 2016a).…”

Section: Becdm Cosmologymentioning

confidence: 99%

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Galaxy formation with BECDM – II. Cosmic filaments and first galaxies

Mocz

Fialkov

Vogelsberger

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Bose-Einstein Condensate Dark Matter (BECDM; also known as Fuzzy Dark Matter) is motivated by fundamental physics and has recently received significant attention as a serious alternative to the established Cold Dark Matter (CDM) model. We perform cosmological simulations of BECDM gravitationally coupled to baryons and investigate structure formation at high redshifts (z > ∼ 5) for a boson mass m = 2.5 · 10 −22 eV, exploring the dynamical effects of its wavelike nature on the cosmic web and the formation of first galaxies. Our BECDM simulations are directly compared to CDM as well as to simulations where the dynamical quantum potential is ignored and only the initial suppression of the power spectrum is considered -a Warm Dark Matterlike ("WDM") model often used as a proxy for BECDM. Our simulations confirm that "WDM" is a good approximation to BECDM on large cosmological scales even in the presence of the baryonic feedback. Similarities also exist on small scales, with primordial star formation happening both in isolated haloes and continuously along cosmic filaments; the latter effect is not present in CDM. Global star formation and metal enrichment in these first galaxies are delayed in BECDM/"WDM" compared to the CDM case: in BECDM/"WDM" first stars form at z ∼ 13/13.5 while in CDM star formation starts at z ∼ 35. The signature of BECDM interference, not present in "WDM", is seen in the evolved dark matter power spectrum: although the small scale structure is initially suppressed, power on kpc scales is added at lower redshifts. Our simulations lay the groundwork for realistic simulations of galaxy formation in BECDM.

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Section: Introductionmentioning

confidence: 77%

Section: Discussion Of Various Numerical Approaches For Becdm and Thementioning

confidence: 99%

Section: Spectral Methodsmentioning

confidence: 99%

Section: Becdm Cosmologymentioning

confidence: 99%

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Galaxy formation with BECDM – II. Cosmic filaments and first galaxies

Mocz

Fialkov

Vogelsberger

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…for m ∈ Z. As noted in [3,19], we must choose a time step such that our unitary operators which evolve the system forward in time,…”

Section: Momentum Aliasingmentioning

confidence: 99%

Investigating the use of field solvers for simulating classical systems

et al. 2020

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We explore the use of field solvers as approximations of classical Vlasov-Poisson systems. This correspondence is investigated in both electrostatic and gravitational contexts. We demonstrate the ability of field solvers to be excellent approximations of problems with cold initial condition into the nonlinear regime. We also investigate extensions of the Schrödinger-Poisson system that employ multiple stacked cold streams, and the von Neumann-Poisson equation as methods that can successfully reproduce the classical evolution of warm initial conditions. We then discuss how appropriate simulation parameters need to be chosen to avoid interference terms, aliasing, and wave behavior in the field solver solutions. We present a series of criteria clarifying how parameters need to be chosen in order to effectively approximate classical solutions.

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Stability of multistate configurations of fuzzy dark matter

Guzmán

2021

Astron Nachr

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We study the stability properties of multistate configurations of the Schrödinger-Poisson system without self-interaction, with monopolar and first dipolar components (1,0,0) + (2,1,0). We show that these studied configurations are stable using numerical simulations and using criteria of stationarity, unitarity, and time dependence consistency. The study covers a range of states with a monopolar to dipolar mass ratio of between 47 and 0.17. The astrophysical implication of this result is that this type of configurations is at least stable and can be considered physically sound in multistate ultralight bosonic dark matter.

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Galaxy formation with BECDM – I. Turbulence and relaxation of idealized haloes

Cited by 318 publications

References 93 publications

Galaxy formation with BECDM – II. Cosmic filaments and first galaxies

Galaxy formation with BECDM – II. Cosmic filaments and first galaxies

Investigating the use of field solvers for simulating classical systems

Stability of multistate configurations of fuzzy dark matter

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