Cosmological inhomogeneities with Bose-Einstein condensate dark matter

Kain, Ben; Ling, Hong Y.

doi:10.1103/physrevd.85.023527

Cited by 31 publications

(32 citation statements)

References 64 publications

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“…These include cored density profiles in dwarf-spheroidal galaxies [31,120,133,[137][138][139][140], suppressed number densities of Milky Way satellites [139] (providing a possible solution to well-known discrepancies between small-scale observations and the ΛCDM model, reviewed in Ref. [141]), vortices/caustics in DM halos [133,142], altered reionization due to delayed high-redshift galaxy formation [143], and pulsar-timing searches for gravitational wave emission caused by coherently oscillating density profiles in DM halos [144].…”

Section: Ula Perturbationsmentioning

confidence: 99%

A search for ultralight axions using precision cosmological data

et al. 2015

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Ultralight axions (ULAs) with masses in the range 10 −33 eV ≤ m a ≤ 10 −20 eV are motivated by string theory and might contribute to either the dark-matter or dark-energy densities of the Universe. ULAs could suppress the growth of structure on small scales, lead to an altered integrated Sachs-Wolfe effect on cosmic microwave-background (CMB) anisotropies, and change the angular scale of the CMB acoustic peaks. In this work, cosmological observables over the full ULA mass range are computed and then used to search for evidence of ULAs using CMB data from the Wilkinson Microwave Anisotropy Probe (WMAP), Planck satellite, Atacama Cosmology Telescope, and South Pole Telescope, as well as galaxy clustering data from the WiggleZ galaxy-redshift survey. In the mass range 10 −32 eV ≤ m a ≤ 10 −25.5 eV, the axion relicdensity Ω a (relative to the total dark-matter relic density Ω d ) must obey the constraints Ω a =Ω d ≤ 0.05 and Ω a h 2 ≤ 0.006 at 95% confidence. For m a ≳ 10 −24 eV, ULAs are indistinguishable from standard cold dark matter on the length scales probed, and are thus allowed by these data. For m a ≲ 10 −32 eV, ULAs are allowed to compose a significant fraction of the dark energy.

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Section: Ula Perturbationsmentioning

confidence: 99%

A search for ultralight axions using precision cosmological data

et al. 2015

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“…Noninteracting DM has been considered by, e.g., [27], [28], [29][30][31] ("fuzzy dark matter"), [32] ("quantum wave dark matter"), [33,34] ("ultralight axions"), [35,36] ("scalar field dark matter"), [37]. On the other hand, self-interacting DM has been studied in, e.g., [38] ("fluid dark matter"), [39,40] ("repulsive dark matter"), and [41][42][43][44][45][46][47]. In the self-interacting 1 DM case (including our SFDM model with a quartic potential [21][22][23], referred to there as BEC-CDM), the suppression of small-scale structure can also result from the pressure force associated with its repulsive potential, rather than solely from the "quantum pressure" associated with large de Broglie wavelength as in the non-interacting case.…”

Section: Introductionmentioning

confidence: 99%

Bose-Einstein-condensed scalar field dark matter and the gravitational wave background from inflation: New cosmological constraints and its detectability by LIGO

Shapiro

Rindler-Daller

2017

Phys. Rev. D

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We consider an alternative to WIMP cold dark matter (CDM), ultralight bosonic dark matter (m 10 −22 eV/c 2 ) described by a complex scalar field (SFDM) with a global U (1) symmetry, for which the comoving particle number density, or charge density, is conserved after particle production during standard reheating. We allow for a repulsive self-interaction. In a ΛSFDM universe, SFDM starts relativistic, evolving from stiff (w = 1) to radiation-like (w = 1/3), before becoming nonrelativistic at late times (w = 0). Thus, before the familiar radiation-dominated era, there is an earlier era of stiff-SFDM-domination. During both the stiff-SFDM-dominated and radiation-dominated eras, the expansion rate is higher than in ΛCDM. SFDM particle mass m and quartic self-interaction coupling strength λ, are therefore constrained by cosmological observables, particularly N eff , the effective number of neutrino species during BBN, and zeq, the redshift of matter-radiation equality. Furthermore, since the stochastic gravitational wave background (SGWB) from inflation is amplified during the stiff-SFDM-dominated era, it can contribute a radiationlike component large enough to affect these observables, by further boosting the expansion rate after the stiff era ends. Remarkably, this same amplification makes detection of the SGWB possible at high frequencies by current laser interferometer experiments, e.g., aLIGO/Virgo and LISA. For SFDM particle parameters that satisfy these cosmological constraints, the amplified SGWB is detectable by LIGO for a broad range of reheat temperatures T reheat , for values of the tensor-to-scalar ratio r currently allowed by CMB polarization measurements. For a given r and λ/(mc 2 ) 2 , the marginally-allowed ΛSFDM model for each T reheat has the smallest m that satisfies the cosmological constraints, and maximizes the present SGWB energy density for that T reheat . This SGWB is then maximally detectable for values of T reheat for which modes that reenter the horizon when reheating ended have frequencies today that lie within the LIGO sensitive band. For example, for the family of marginally-allowed models with r = 0.01 and λ/(mc 2 ) 2 = 10 −18 eV −1 cm 3 , the maximally detectable ΛSFDM model has T reheat ≃ 2 × 10 4 GeV and m ≃ 1.6 × 10 −19 eV/c 2 , for which we predict an aLIGO O1 run detection with signal-to-noise ratio of ∼ 10. We show that the null detection of the SGWB recently reported by the aLIGO O1 run excludes the parameter range 8.75 × 10 3 T reheat (GeV) 1.7 × 10 5 for this illustrative family at 95% confidence, thereby demonstrating that GW detection experiments can already place a new kind of cosmological constraint on SFDM. A wider range of SFDM parameters and reheat temperatures should be accessible to aLIGO/Virgo O5, with the potential to detect this unique signature of the ΛSFDM model. For this same illustrative family, for example, a 3σ detection is predicted for 600 T reheat (GeV) 10 7 .

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“…This subject has been mainly JHEP03(2016)013 studied for harmonic potential models that mimic the standard dark matter case [65][66][67][68][69][70][71], as it happens for the axion field [72,73]. It has been proved by using the linear perturbation theory that the axion was equivalent to CDM for high enough masses [74][75][76][77].…”

Section: Introductionmentioning

confidence: 99%

Cosmological perturbations in coherent oscillating scalar field models

Cembranos

Maroto

Jareño

2016

J. High Energ. Phys.

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The fact that fast oscillating homogeneous scalar fields behave as perfect fluids in average and their intrinsic isotropy have made these models very fruitful in cosmology. In this work we will analyse the perturbations dynamics in these theories assuming general power law potentials V (φ) = λ|φ| n /n. At leading order in the wavenumber expansion, a simple expression for the effective sound speed of perturbations is obtained c 2 eff = ω = (n − 2)/(n + 2) with ω the effective equation of state. We also obtain the first order correction in k 2 /ω 2 eff , when the wavenumber k of the perturbations is much smaller than the background oscillation frequency, ω eff . For the standard massive case we have also analysed general anharmonic contributions to the effective sound speed. These results are reached through a perturbed version of the generalized virial theorem and also studying the exact system both in the super-Hubble limit, deriving the natural ansatz for δφ; and for sub-Hubble modes, exploiting Floquet's theorem.

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Cosmological inhomogeneities with Bose-Einstein condensate dark matter

Cited by 31 publications

References 64 publications

A search for ultralight axions using precision cosmological data

A search for ultralight axions using precision cosmological data

Bose-Einstein-condensed scalar field dark matter and the gravitational wave background from inflation: New cosmological constraints and its detectability by LIGO

Cosmological perturbations in coherent oscillating scalar field models

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