Core-halo mass relation of ultralight axion dark matter from merger history

Behrens, Christoph; Niemeyer, J. C.; Schwabe, Bodo

doi:10.1103/physrevd.95.043519

Cited by 46 publications

(44 citation statements)

References 71 publications

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“…We note that a power of η = 1/2 is derived analytically from self-similarity of the potential of the core and halo, which basically is the assumption: Mc/rc ∼ M/R h . On the other hand, η = 1/3 can be derived analytically from self-similarity of the energy of the core and halo: M It has also been suggested, in the literature, that Mc/M essentially follows from the mass loss in subsequent binary mergers (Du et al 2017). That work suggests Mc ∝ M 1.44(β−1) where β ≤ 1 is the descendant-to-originator mass-fraction.…”

Section: Soliton Core Mass Scalingmentioning

confidence: 99%

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

Mocz

Vogelsberger

Robles

et al. 2017

Monthly Notices of the Royal Astronomical Society

318

391

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We present a theoretical analysis of some unexplored aspects of relaxed Bose-Einstein condensate dark matter (BECDM) haloes. This type of ultralight bosonic scalar field dark matter is a viable alternative to the standard cold dark matter (CDM) paradigm, as it makes the same large-scale predictions as CDM and potentially overcomes CDM's small-scale problems via a galaxy-scale de Broglie wavelength. We simulate BECDM halo formation through mergers, evolved under the Schrödinger-Poisson equations. The formed haloes consist of a soliton core supported against gravitational collapse by the quantum pressure tensor and an asymptotic r −3 NFW-like profile. We find a fundamental relation of the core=to-halo mass with the dimensionless invariant Ξ ≡ |E|/M 3 /(Gm/ ) 2 or M c /M 2.6Ξ 1/3 , linking the soliton to global halo properties. For r ≥ 3.5 r c core radii, we find equipartition between potential, classical kinetic, and quantum gradient energies. The haloes also exhibit a conspicuous turbulent behavior driven by the continuous reconnection of vortex lines due to wave interference. We analyse the turbulence 1D velocity power spectrum and find a k −1.1 power-law. This suggests the vorticity in BECDM haloes is homogeneous, similar to thermally-driven counterflow BEC systems from condensed matter physics, in contrast to a k −5/3 Kolmogorov power-law seen in mechanically-driven quantum systems. The mode where the power spectrum peaks is approximately the soliton width, implying the soliton-sized granules carry most of the turbulent energy in BECDM haloes.

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Section: Soliton Core Mass Scalingmentioning

confidence: 99%

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

Mocz

Vogelsberger

Robles

et al. 2017

Monthly Notices of the Royal Astronomical Society

318

391

View full text Add to dashboard Cite

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“…the surrounding, CDM-like halo envelope, and that the size of the soliton and the halo mass are anti-correlated (Schive et al 2014a,b;Du et al 2017) rc = 1.6 kpc ma 10 −22 eV…”

Section: Ultra-light Axion (Ula) Subhaloesmentioning

confidence: 99%

Fluctuations of the gravitational field generated by a random population of extended substructures

Peñarrubia

2017

Monthly Notices of the Royal Astronomical Society

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A large population of extended substructures generates a stochastic gravitational field that is fully specified by the function p(F), which defines the probability that a tracer particle experiences a force F within the interval F, F + dF. This paper presents a statistical technique for deriving the spectrum of random fluctuations directly from the number density of substructures with known mass and size functions. Application to the subhalo population found in cold dark matter simulations of Milky Way-sized haloes shows that, while the combined force distribution is governed by the most massive satellites, the fluctuations of the tidal field are completely dominated by the smallest and most abundant subhaloes. In light of this result we discuss observational experiments that may be sufficiently sensitive to Galactic tidal fluctuations to probe the "dark" low-end of the subhalo mass function and constrain the particle mass of warm and ultra-light axion dark matter models.

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“…The function f (ν) comes from the Sheth-Thormen model (Sheth and Tormen 1999) and it is given by f (ν (Marsh and Silk 2014;Bozek et al 2015) (in Marsh (2016b) a numerical fitting for this function was found). There are many other modifications of this HMF and alternative formulations that can be seen in Sheth and Tormen (1999), Bozek et al (2015), Du et al (2017b) and .…”

Section: Halo Density Profilementioning

confidence: 99%

Ultra-light dark matter

Ferreira

2021

Astron Astrophys Rev

257

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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Core-halo mass relation of ultralight axion dark matter from merger history

Cited by 46 publications

References 71 publications

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

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

Fluctuations of the gravitational field generated by a random population of extended substructures

Ultra-light dark matter

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