Dark matter decaying in the late Universe can relieve the 
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 tension

Vattis, Kyriakos; Koushiappas, Savvas M.; Loeb, Abraham

doi:10.1103/physrevd.99.121302

Cited by 198 publications

(172 citation statements)

References 61 publications

(56 reference statements)

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“…The dependence of V 6 appears through a FS in Eq. (13). We show the result of mapping 0.3Mpc < λ FS < 0.5Mpc to (m DM , V 6 ) plane in Fig 2 as the space between the two red solid and dotdashed lines.…”

Section: Constraints From the Free-streaming Lengthmentioning

confidence: 98%

“…where n DM is the number density of the dark matter, s SM is the entropy density of the SM sector, and we used the values, Ω DM,0 = 0.24, H 0 = 70km/sec/Mpc [13] and s SM,0 2.945 × 10 −11 eV 3 (entropy density today). Using the approximation 2n φ 6 = n DM at production time, one obtains…”

Section: A Concrete Scenariomentioning

confidence: 99%

“…Eventually we show there exists a parameter space where the desired physics can be realized in the model. [13] at 1σ level. (On the right panel, we showed the same mapping at 2σ level with the green solid line and green shaded region.)…”

Section: A Concrete Scenariomentioning

confidence: 99%

“…While unknown systematics may affect the discrepancy [10][11][12], it could be a clue for a nature of DM. In particular, a decaying DM (DDM) solution [13] 2 to the tension amongst several resolutions proposes a possibility that the decay of DM with a lifetime ∼35Gyrs can relieve the tension. 3 The advanced starting of the dark energy dominated era due to DM decay enables the faster * gongjun.choi@gmail.com † m0t@icrr.u-tokyo.ac.jp ‡ tsutomu.tyanagida@ipmu.jp 1 See e.g.…”

Section: Introductionmentioning

confidence: 99%

“…(8) and Eq (13). withρ DM (a BBN ) = m 2 DM + m 6 a FS 2a BBN DM s SM (a BBN ) ,(18)yields the parameter space in (m DM , V 6 ) plane satisfying the condition ∆N BBN eff 1.…”

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confidence: 99%

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Degenerate Sub-keV fermion dark matter from a solution to the Hubble tension

2020

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We present a dark sector model addressing both the Hubble tension and the core-cusp problem. The model is based on a hidden Abelian gauge symmetry group with some chiral fermions required by the anomaly cancellation conditions, producing a candidate for the decaying fermion dark matter as a solution to the Hubble tension. Moreover, the sub-keV mass regime and the thermal history of the dark sector help the dark matter candidate resolve the core-cusp problem occurring in the standard ΛCDM cosmology.

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Section: Constraints From the Free-streaming Lengthmentioning

confidence: 98%

Section: A Concrete Scenariomentioning

confidence: 99%

Section: A Concrete Scenariomentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

“…(8) and Eq (13). withρ DM (a BBN ) = m 2 DM + m 6 a FS 2a BBN DM s SM (a BBN ) ,(18)yields the parameter space in (m DM , V 6 ) plane satisfying the condition ∆N BBN eff 1.…”

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confidence: 99%

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Degenerate Sub-keV fermion dark matter from a solution to the Hubble tension

2020

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A model of interacting dark matter and dark radiation for H0 and σ8 tensions

Choi

Yanagida

Yokozaki

2021

J. High Energ. Phys.

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We present a model describing the dark sector (DS) featured by two interactions remaining efficient until late times in the matter-dominated era after recombination: the interaction among dark radiations (DR), and the interaction between a small fraction of dark matter and dark radiation. The dark sector consists of (1) a dominant component cold collisionless DM (DM1), (2) a sub-dominant cold DM (DM2) and (3) a self-interacting DR. When a sufficient amount of DR is ensured and a few percent of the total DM density is contributed by DM2 interacting with DR, this set-up is known to be able to resolve both the Hubble and σ8 tension. In light of this, we propose a scenario which is logically natural and has an intriguing theoretical structure with a hidden unbroken gauge group SU(5)X ⊗ U(1)X. Our model of the dark sector does not introduce any new scalar field, but contains only massless chiral fermions and gauge fields in the ultraviolet (UV) regime. As such, it introduces a new scale (DM2 mass, mDM2) based on the confinement resulting from the strong dynamics of SU(5)X. Both DM2-DR and DR-DR interactions are attributed to an identical long range interaction of U(1)X. We show that our model can address the cosmological tensions when it is characterized by gX = $$ \mathcal{O} $$ O (10−3)–$$ \mathcal{O} $$ O (10−2), mDM2 = $$ \mathcal{O} $$ O (1)–$$ \mathcal{O} $$ O (100) GeV and TDS/TSM ≃ 0.3–0.4 where gX is the gauge coupling of U(1)X and TDS(TSM) is a temperature of the DS (Standard Model sector). Our model explains candidates of DM2 and DR, and DM1 can be any kind of CDM.

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Freeze-in dark matter via lepton portal: Hubble tension and stellar cooling

Xu,

Zhang

et al. 2023

J. High Energ. Phys.

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We propose a new freeze-in dark matter candidate which feebly couples to the standard model charged leptons. The feeble interactions allow it (i) to freeze-in from the Standard Model thermal bath with its relic density being either a fraction or the entirety of the observed dark matter density and (ii) to radiatively decay to two photons in the dark matter mass ranges of order keV scale with lifetime larger than the age of Universe. These features make this model a realistic realization of dark matter with late-time decay to reduce Hubble tension. We show the best-fit value of H0 = 68.31(69.34) km s−1Mpc−1 in light of Planck 2018+BAO(+LSS)+Pantheon data sets. We then use stellar cooling data to place constraints on the parameter space favored by the Hubble tension. While the universal coupling scenario is excluded, the hierarchical coupling scenario can be tested by future observations of white dwarfs after a careful look into photon inverse decay, Primakoff and Bremsstrahlung emission of the dark matter in various stellar systems. The viable parameter space may be linked to anomalies in future X-ray telescopes.

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Dark matter decaying in the late Universe can relieve the H0 tension

Cited by 198 publications

References 61 publications

Degenerate Sub-keV fermion dark matter from a solution to the Hubble tension

Degenerate Sub-keV fermion dark matter from a solution to the Hubble tension

A model of interacting dark matter and dark radiation for H0 and σ8 tensions

Freeze-in dark matter via lepton portal: Hubble tension and stellar cooling

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