Constraints on anharmonic corrections of fuzzy dark matter

Cembranos, J. A. R.; Maroto, Antonio L.; Jareño, S. J. Núñez; Villarrubia-Rojo, Hector

doi:10.1007/jhep08(2018)073

Cited by 30 publications

(32 citation statements)

References 61 publications

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“…Although ultralight scalars, i.e., spin-zero fields with very small masses (m ∼ 10 −22 eV), such as axionlike particles, have been among the most studied proposals [2][3][4], fuzzy dark matter can be extended to higherspin fields. In that sense, ultralight vector fields (ULVFs) [5][6][7][8][9][10], spin-1 bosons with very small masses (m ≪ 1 eV) and very weak interactions, have been growing in popularity throughout the last years, also making a good candidate for dark matter.…”

Section: Introductionmentioning

confidence: 99%

Imprint of ultralight vector fields on gravitational wave propagation

Miravet

Maroto

2021

Phys. Rev. D

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We study the effects of ultralight vector field (ULVF) dark matter on gravitational wave propagation. We find that the coherent oscillations of the vector field induce an anisotropic suppression of the gravitational wave amplitude as compared to the standard cosmology prediction. The effect is enhanced for smaller vector field masses and peaks for modes aroundThe suppression is negligible for astrophysically generated gravitational waves but could be sizable for primordial gravity waves. We discuss the possibility of detecting such an effect on the tensor power spectrum with future cosmic microwave background B-mode polarization detectors. We find that for the sensitivity of the upcoming LiteBIRD mission, the correction to the tensor power spectrum at decoupling time could be distinguishable from that of ΛCDM for ULVF masses m ≲ 10 −26 eV and sufficiently large abundances.

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Section: Introductionmentioning

confidence: 99%

Imprint of ultralight vector fields on gravitational wave propagation

Miravet

Maroto

2021

Phys. Rev. D

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“…A similar study of the quartic self-interaction model for a real scalar field can be found in[90], although the initial conditions were seemingly chosen so that the early stiff and radiation like behaviors were avoided. In such a case, the nucleosynthesis constraints are not important, and both the mass and self-interaction parameters can be varied more freely than in the case considered in[25].…”

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confidence: 99%

Scalar field dark matter with a cosh potential, revisited

Ureña–López

2019

J. Cosmol. Astropart. Phys.

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Dark matter models in which the constituent particle is an ultra-light boson have become part of the mainstream discussion in cosmology and astrophysics. At the classical level, the models are represented by the dynamics of a (real or complex) scalar field endowed with a potential that contains its self-interactions, and for this reason are generically known as scalar field dark matter models. Here, we revisit the properties of such a model with a cosh potential and compare it with other known examples in the literature. Within the cosmological context, the self-interaction in the potential induces a radiation-like behavior at early times of the scalar field density, which is followed by a proper matter-like behavior at the onset of rapid field oscillations around the minimum of the potential. The solutions are found by numerical means, and from them we obtain information about the cosmological observables up to the level of linear density perturbations. We also study the general properties of selfgravitating objects in the non-relativistic limit and determine the role in them of the selfinteraction obtained from the cosh potential. An overall conclusion is that, for the range of values in its parameters allowed by different constraints, a cosh potential behaves almost indistinguishable from the simpler quadratic one, which also means that the two models suffer the same tight constraints from cosmological and astrophysical observations.

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“…The main stages of the formation of scalar dark-matter clumps for the tachyonic scenario (31). Cosmic time grows from the left column to the right column, and from the upper panel to the lower panel within each column.…”

Section: A Polynomial Self-interactionsmentioning

confidence: 99%

“…In the simplest case, called fuzzy dark matter [12,13], a massive scalar field oscillating around its vacuum expectation value (vev), and with a sufficiently low mass m ≲ 10 −21 eV, could play the role of dark matter. The resulting properties of these scalar dark-matter models are similar to the standard cold dark matter (CDM) for the formation of large-scale structures [14][15][16][17][18][19][20][21], but not for small scales, where distinctive features such as a nonvanishing speed of sound can leave different observational signatures [19,20,[22][23][24][25][26][27][28][29][30][31][32][33][34][35].…”

Section: Introductionmentioning

confidence: 99%

Nonrelativistic formation of scalar clumps as a candidate for dark matter

2020

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We propose a new mechanism for the formation of dark matter clumps in the radiation era. We assume that a light scalar field is decoupled from matter and oscillates harmonically around its vacuum expectation value. We include self-interactions and consider the nonrelativistic regime. The scalar dynamics are described by a fluid approach where the fluid pressure depends on both quantum and self-interaction effects. When the squared speed of sound of the scalar fluid becomes negative, an instability arises and the fluctuations of the scalar energy-density field start growing. They eventually become nonlinear and clumps form. Subsequently, the clumps aggregate and reach a universal regime. Afterwards, they play the role of cold dark matter. We apply this mechanism first to a model with a negative quartic term stabilized by a positive self-interaction of order six, and then to axion monodromy, where a subdominant cosine potential corrects a mass term. In the first case, the squared speed of sound becomes negative when the quartic term dominates, leading to a tachyonic instability. For axion monodromy, the instability starts very slowly after the squared speed of sound first becomes negative and then oscillates around zero. Initially the density perturbations perform acoustic oscillations due to the quantum pressure. Eventually, they start growing exponentially due to a parametric resonance. The shape and the scaling laws of the clumps depend on their formation mechanism. When the tachyonic phase takes place, the core density of the clumps is uniquely determined by the energy density at the beginning of the instability. On the other hand, for axion monodromy, the core density scales with the soliton mass and radius. This difference comes from the crucial role that the quantum pressure plays in both the parametric resonance in the linear regime and in the nonlinear formation regime of static scalar solitons. In both scenarios, the scalar-field clumps span a wide range of scales and masses, running from the size of atoms to that of galactic molecular clouds, and from 10 −3 gram to thousands of solar masses. Because of finite-size effects, both from the source and the lens, these dark matter clumps are far beyond the reach of microlensing observations. We find that the formation redshift of the scalar clumps can span a large range in the radiation era; the associated background temperature can vary from 10 eV to 10 5 GeV, and the scalar-field mass from 10 −26 GeV to 10 GeV.

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Constraints on anharmonic corrections of fuzzy dark matter

Cited by 30 publications

References 61 publications

Imprint of ultralight vector fields on gravitational wave propagation

Imprint of ultralight vector fields on gravitational wave propagation

Scalar field dark matter with a cosh potential, revisited

Nonrelativistic formation of scalar clumps as a candidate for dark matter

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