Dark disk substructure and superfluid dark matter

Alexander, Stephon; Bramburger, Jason J.; McDonough, Evan

doi:10.1016/j.physletb.2019.134871

Cited by 33 publications

(24 citation statements)

References 52 publications

(121 reference statements)

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“…Some recent work in the literature investigated nonspherical distributions of condensed dark matter [49,50]. Reference [49] considered a nonspherical parametrization of ULDM halos and solitons and applied it to a Jeans analysis of dwarf spheroidal galaxies.…”

Section: Introductionmentioning

confidence: 99%

“…[49]. Reference [50] looked for disk configurations of self-interacting condensed dark matter. However, while Ref.…”

Section: Introductionmentioning

confidence: 99%

“…However, while Ref. [50] looked for nonspherical configurations, at no point do they solve the EOM. Instead, they restrict the solution to certain disklike geometries and define and solve a modified one-dimensional system.…”

Section: Introductionmentioning

confidence: 99%

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Ultralight dark matter in disk galaxies

et al. 2019

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Analytic arguments and numerical simulations show that bosonic ultralight dark matter (ULDM) would form cored density distributions ("solitons") at the center of galaxies. ULDM solitons offer a promising way to exclude or detect ULDM by looking for a distinctive feature in the central region of galactic rotation curves. Baryonic contributions to the gravitational potential pose an obstacle to such analyses, being (i) dynamically important in the inner galaxy and (ii) highly nonspherical in rotation-supported galaxies, resulting in nonspherical solitons. We present an algorithm for finding the ground-state soliton solution in the presence of stationary nonspherical background baryonic mass distribution. We quantify the impact of baryons on the predicted ULDM soliton in the Milky Way and in low-surface-brightness galaxies from the SPARC database.

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Section: Introductionmentioning

confidence: 99%

“…[49]. Reference [50] looked for disk configurations of self-interacting condensed dark matter. However, while Ref.…”

Section: Introductionmentioning

confidence: 99%

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Ultralight dark matter in disk galaxies

et al. 2019

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“…Dark disks are a unique type of substructure in isolated systems, not expected in CDM. Those dark disks can be formed in the models based on the superfluid DM (Alexander et al 2019) and are very distinct signature of those alternative models. Strong gravitational lensing is an important technique to probe these substructures, and one of the techniques that is going to improve the most with the upcoming experiments.…”

Section: Substructure-strong Lensingmentioning

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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“…Besides it being an interesting substance with interesting properties on its own, that can be manufactured in laboratories from known particles, superfluids have been theorised to be potentially relevant even in dark matter context. In particular, in some scenarios dark matter may undergo superfluid phase-transition cosmologically and/or in localised structure [6][7][8][9][10][11][12][13][14][15]. In some other cases, the superfluid He has been proposed as a target material for dark matter detection [16][17][18][19].…”

Section: Introductionmentioning

confidence: 99%

On effective theory of superfluid phonons

Berezhiani

2020

Physics Letters B

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It is shown that the standard effective field theory of non-relativistic superfluids, which includes only the leading order action in derivative expansion, is in general inadequate for studying supersonic processes. Namely, for a proper treatment of the latter the phonons with momenta greater than mc s are relevant at times (with m being the mass of the superfluid constituent and c s denoting the sound-speed), which lie beyond the regime of validity of the naive effective theory mentioned above. This is demonstrated on a concrete example by recovering the known expression for the friction force as a process of radiating phonons by a supersonic perturber. In particular, when the impurity is heavier than superfluid constituents, it is indeed necessary to extend the non-relativistic effective theory of superfluids to include high-derivative corrections. For the light perturber, however, there is a window of velocities for which high-derivative corrections are irrelevant.

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Dark disk substructure and superfluid dark matter

Cited by 33 publications

References 52 publications

Ultralight dark matter in disk galaxies

Ultralight dark matter in disk galaxies

Ultra-light dark matter

On effective theory of superfluid phonons

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