Not so fuzzy: excluding FDM with sizes and stellar kinematics of ultra-faint dwarf galaxies

Dalal, Neal; Kravtsov, Andrey V.

doi:10.48550/arxiv.2203.05750

Cited by 16 publications

(23 citation statements)

References 55 publications

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“…A recent study has looked at constraining the FDM particle mass by considering the effect of dynamical heating on the stellar kinematics in ultra-faint dwarf galaxies [28], and found a tight constraint of m > 3 × 10 −19 eV. Under the VDM assumption this constraint would be similarly relaxed.…”

Section: Dark Matter Substructure and Dynamical Heatingmentioning

confidence: 99%

Small-scale structure in vector dark matter

Amin,

Jain,

Karur

et al. 2022

Preprint

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We investigate the differences in the small-scale structure of vector dark matter (VDM) and scalar dark matter (SDM) using 3+1 dimensional simulations of single/multicomponent Schrödinger-Poisson system. We find that the amount of wave interference, core to halo mass ratio (and its scatter), spin of the core, as well as the shape of the central regions of dark matter halos can distinguish VDM and SDM. Starting with a collection of idealized halos (selfgravitating solitons) as an initial condition, we show that the system dynamically evolves to an approximately spherically symmetric configuration that has a core surrounded by a halo of interference patterns in the mass density. In the vector case, the central soliton in less dense and has a smoother transition to an r −3 tail compared to the scalar case. Wave interference is ∼ 1/ √ 3 times smaller in VDM compared to SDM, resulting in fewer low and high density regions in VDM compared to SDM, with more diffuse granules in the halo. The ratio of VDM core mass to the total halo mass is lower than that in SDM, with a steeper dependence on the total energy of the system and a slightly larger scatter. Finally, we also initiate a study of the evolution of intrinsic spin angular momentum in the VDM case. We see a positive correlation between the total intrinsic spin in the simulation and the spin of the final central core, with significant scatter. We see large intrinsic spin in the core being possible even with vanishing amounts total angular momentum in the initial conditions. Our results point towards the possibility of distinguishing VDM from SDM using astrophysical and terrestrial observations.

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Section: Dark Matter Substructure and Dynamical Heatingmentioning

confidence: 99%

Small-scale structure in vector dark matter

Amin,

Jain,

Karur

et al. 2022

Preprint

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“…V C, solar neutrino oscillations from Sec. IV A, and model independent limits on light DM from ultra faint dwarf (UFD) heating [17]. For points below the gray dotted line, the φ mediated force between right handed neutrinos is weaker than gravity, which is theoretically disfavored by the weak gravity conjecture [18] Right: same as the left panel, only φ now couples only to ν 3 , so the limits are driven by ν µ,τ oscillations for which the solar bound is subdominant to the atmospheric bound described in Sec.…”

Section: Ultralight Dark Matter and Pseudo-dirac Neutrinosmentioning

confidence: 99%

Constraining Feeble Neutrino Interactions with Ultralight Dark Matter

Dev¹,

Krnjaic²,

Machado³

et al. 2022

Preprint

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If ultralight ( eV), bosonic dark matter couples to right handed neutrinos, active neutrino masses and mixing angles depend on the ambient dark matter density. When the neutrino Majorana mass, induced by the dark matter background, is small compared to the Dirac mass, neutrinos are "pseudo-Dirac" fermions that undergo oscillations between nearly degenerate active and sterile states.We present a complete cosmological history for such a scenario and find severe limits from a variety of terrestrial and cosmological observables. For scalar masses in the "fuzzy" dark matter regime (∼ 10 −20 eV), these limits exclude couplings of order 10 −30 , corresponding to Yukawa interactions comparable to the gravitational force between neutrinos and surpassing equivalent limits on time variation in scalar-induced electron and proton couplings.

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“…Comparisons between structure formation in simulations with ULDM and the Lyman-𝛼 forest yield a 95% lower limit 𝑚 𝜓 > 2 × 10 −20 eV (Rogers & Peiris 2021). Dalal & Kravtsov (2022) claimed a constraint 𝑚 𝜓 > 3 × 10 −19 eV at 99% confidence based on stellar dynamics in ultra-faint dwarf galaxies. The constraints on the particle mass from the Lyman-𝛼 forest and stellar dynamics in ultra-faint dwarfs depend on indirect probes of dark matter structure, in the sense that the observable used to constrain the particle mass is associated with baryonic physics.…”

Section: Introductionmentioning

confidence: 95%

Quantum fluctuations masquerade as halos: Bounds on ultra-light dark matter from quadruply-imaged quasars

Alexander¹,

Gilman²,

Li³

et al. 2022

Preprint

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Ultra-light dark matter (ULDM) refers to a class of theories, including ultra-light axions, in which particles with mass 𝑚 𝜓 < 10 −20 eV comprise a significant fraction of the dark matter. A galactic scale de Broglie wavelength distinguishes these theories from cold dark matter (CDM), suppressing the overall abundance of structure on sub-galactic scales, and producing wave-like interference phenomena in the density profiles of halos. With the aim of constraining the particle mass, we analyze the flux ratios in a sample of eleven quadruple-image strong gravitational lenses. We account for the suppression of the halo mass function and concentration-mass relation predicted by ULDM theories, and the wave-like fluctuations in the host halo density profile, calibrating the model for the wave interference against numerical simulations of galactic-scale halos. We show that the granular structure of halo density profiles, in particular, the amplitude of the fluctuations, significantly impacts image flux ratios, and therefore inferences on the particle mass derived from these data. We infer relative likelihoods of CDM to ULDM

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Not so fuzzy: excluding FDM with sizes and stellar kinematics of ultra-faint dwarf galaxies

Cited by 16 publications

References 55 publications

Small-scale structure in vector dark matter

Small-scale structure in vector dark matter

Constraining Feeble Neutrino Interactions with Ultralight Dark Matter

Quantum fluctuations masquerade as halos: Bounds on ultra-light dark matter from quadruply-imaged quasars

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