Cosmological constraints on dark scalar

Ibe, Masahiro; Kobayashi, Shin; Nakayama, Yuhei; Shirai, Satoshi

doi:10.1007/jhep03(2022)198

Cited by 17 publications

(16 citation statements)

References 75 publications

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“…For the mixing angle in the range of interest for the supernova limits, with T R = 5 MeV, the limit is m S > 1 MeV. With T R 100 GeV, the cosmological limit is very sensitive to the mixing angle sin θ, excluding scalar mass even above GeV [99,103,104]. However, there is a "blind spot" left unconstrained at m S ∼ 2 MeV and sin θ ∼ 10 −5 [99], which is labeled as the shaded green region in the right panel of Fig.…”

Section: Resultsmentioning

confidence: 99%

“…All these bounds assume that the luminosity L S < 3 × 10 52 erg/sec. Right panel: Complementarity of the supernova limits with those from collider searches (shaded gray) [96][97][98] and the cosmological blind spot with a high reheating temperature of 100 GeV (shaded green) [99]. The orange, pink and red lines indicate the future prospects of S at SBN [100], DUNE [101] and FASER 2 [102].…”

Section: Resultsmentioning

confidence: 99%

“…However, it is expected that, within standard cosmology, the whole parameter space in Fig. 9 has been excluded by the cosmological constraints [99,103,104].…”

Section: Resultsmentioning

confidence: 99%

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Improved stellar limits on a light CP-even scalar

Balaji,

Dev,

Silk

et al. 2022

Preprint

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We derive improved stellar luminosity limits on a generic light CP-even scalar field S mixing with the Standard Model (SM) Higgs boson from the supernova SN1987A, the Sun, red giants (RGs) and white dwarfs (WDs). For the first time, we include the geometric effects for the decay and absorption of S particles in the stellar interior. For SN1987A and the Sun, we also take into account the detailed stellar profiles. We find that a broad range of the scalar mass and mixing angle can be excluded by our updated astrophysical constraints. For instance, SN1987A excludes 1.0 × 10 −7 sin θ 4.0 × 10 −5 and scalar mass up to 290 MeV, which covers the cosmological blind spot with a high reheating temperature. The updated solar limit excludes the mixing angle in the range of 3.8 × 10 −11 < sin θ < 0.27, with scalar mass up to 39 keV. The RG and WD limits are updated to 4.3 × 10 −13 < sin θ < 8.6 × 10 −5 and 2.3×10 −18 < sin θ < 3.5×10 −8 , with scalar mass up to 398 keV and 292 keV, respectively.

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Section: Resultsmentioning

confidence: 99%

Section: Resultsmentioning

confidence: 99%

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Improved stellar limits on a light CP-even scalar

Balaji,

Dev,

Silk

et al. 2022

Preprint

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“…We exclude parameters where ρ d > 0.1ρ SM at any time during BBN (light red region). Moreover, if the additional ρ d is deposited into the photon bath through γ d decays after neutrino decoupling (T SM 2 MeV), the photon temperature is increased relative to neutrinos, lowering the value of N eff measured by the CMB [32]. The 95% CL lower bound from Planck [14], N eff > 2.55, excludes the dark red region in the figure . Finally, the freeze-out scenario also allows for sizable self-interaction cross sections.…”

Section: Freeze-outmentioning

confidence: 97%

Dark Higgs dark matter

et al. 2021

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A new U (1) "dark" gauge group coupled to the Standard Model (SM) via the kinetic mixing portal provides a natural dark matter candidate in the form of the Higgs field, h d , responsible for generating the mass of the dark photon, γ d . We show that the condition m h d ≤ mγ d , together with smallness of the kinetic mixing parameter, , and/or dark gauge coupling, g d , leads the dark Higgs to be sufficiently metastable to constitute dark matter. We analyze the Universe's thermal history and show that both freeze-in, SM → {γ d , h d }, and freeze-out, {γ d , h d } → SM, processes can lead to viable dark Higgs dark matter with a sub-GeV mass and a kinetic mixing parameter in the range 10 −13 10 −6 . Observable signals in astrophysics and cosmology include modifications to primordial elemental abundances, altered energetics of supernovae explosions, dark Higgs decays in the late Universe, and dark matter self-interactions.

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“…[73,74] for review on these issues, and phenomenological constraints on dark Higgs boson in Refs. [75,76]). The underlying point is that DM phenomenology can change drastically if dark Higgs boson is included.…”

Section: Introductionmentioning

confidence: 99%

Muon $(g-2)$ and Thermal WIMP DM in ${\rm U(1)}_{L_μ-L_τ} $ Models

Baek¹,

Kim²,

Ko³

2022

Preprint

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U(1) Lµ−Lτ ≡ U(1) X model is anomaly free within the Standard Model (SM) fermion content, and can accommodate the muon (g−2) data for M Z ∼ O(10−100) MeV and gX ∼ (4−8)×10 −4 . WIMP type thermal dark matter (DM) can be also introduced for M Z ∼ 2MDM, if DM pair annihilations into the SM particles occur only through the s-channel Z exchange. In this work, we show that this tight correlation between M Z and MDM can be completely evaded both for scalar and fermionic DM, if we include the contributions from dark Higgs boson (H1). Dark Higgs boson plays a crucial role in DM phenomenology, not only for generation of dark photon mass, but also opening new channels for DM pair annihilations into the final states involving dark Higgs boson, such as dark Higgs pair as well as Z Z through dark Higgs exchange in the s-channel, and co-annihilation into Z H1 in case of inelastic DM. Thus dark Higgs boson will dissect the strong correlation M Z ∼ 2MDM, and much wider mass range is allowed for U (1)X -charged complex scalar and Dirac fermion DM, still explaining the muon (g − 2). We consider both generic U (1)X breaking as well as U(1) X → Z2 (and also into Z3 only for scalar DM case).

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Cosmological constraints on dark scalar

Cited by 17 publications

References 75 publications

Improved stellar limits on a light CP-even scalar

Improved stellar limits on a light CP-even scalar

Dark Higgs dark matter

Muon $(g-2)$ and Thermal WIMP DM in ${\rm U(1)}_{L_μ-L_τ} $ Models

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