Current bounds and future prospects of light neutralino dark matter in the NMSSM

Barman, Rahool Kumar; Bélanger, G.; Bhattacherjee, Biplob; Godbole, Rohini M.; Sengupta, Dipan; Tata, Xerxes

doi:10.1103/physrevd.103.015029

Cited by 21 publications

(9 citation statements)

References 187 publications

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“…In this (MSSM) scenario, the excluded DM masses span a phenomenologically interesting region in the parameter space of the model, as shown in Fig. 17 These bounds are or the order of the electroweak scale, and are comparable to collider and direct detection limits [142,143]. Note that for a model-fixed LSP mass, the Lyman-α constraint puts a bound on the inflaton-matter couplings.…”

Section: Relic Density and Phenomenologymentioning

confidence: 87%

How warm are non-thermal relics? Lyman-$α$ bounds on out-of-equilibrium dark matter

Ballesteros,

Garcia,

Pierre

2020

Preprint

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We investigate the power spectrum of Non-Cold Dark Matter (NCDM) produced in a state out of thermal equilibrium. We consider dark matter production from the decay of scalar condensates (inflaton, moduli), the decay of thermalized and non-thermalized particles, and from thermal and non-thermal freeze-in. For each case, we compute the NCDM phase space distribution and the linear matter power spectrum, which features a cutoff analogous to that for warm dark matter (WDM). This scale is solely determined by the equation of state of NCDM. We propose a mapping procedure that translates the WDM Lyman-α mass bound to NCDM scenarios. This procedure does not require expensive ad hoc numerical computations of the non-linear matter power spectrum. By applying it, we obtain bounds on several NCDM possibilities, ranging from m DM EeV for DM production from inflaton decay with a low reheating temperature, to sub-keV values for non-thermal freeze-in. We discuss the phenomenological implications of these results for specific examples which include strongly-stabilized and nonstabilized supersymmetric moduli, gravitino production from inflaton decay, Z and spin-2 mediated freeze-in, and non-supersymmetric spin-3/2 DM.

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Section: Relic Density and Phenomenologymentioning

confidence: 87%

How warm are non-thermal relics? Lyman-$α$ bounds on out-of-equilibrium dark matter

Ballesteros,

Garcia,

Pierre

2020

Preprint

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“…[17][18][19][20][21][22][23][24][25][26][27][28] as well as discussions in the context of singlino Dark Matter in Refs. [29][30][31][32][33][34][35][36][37]. For simplicity, we only consider the R-parity, Z 3 -and CP-conserving version of the Lagrangian, but the methods and results that we develop here can easily be extended to variants and even to distinct models.…”

Section: Introductionmentioning

confidence: 99%

Curing tachyonic tree-level syndrome in NMSSM light-singlet scenarios

Domingo

Paßehr

2022

Eur. Phys. J. C

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Models with an extended Higgs sector open up the phenomenological possibility of additional scalars, beyond the SM-like boson observed by the LHC, with mass at or below the electroweak scale. Such scenarios are in particular viable in the presence of electroweak-singlet spin-0 fields, as expected for instance in the context of the NMSSM. Given that the size of radiative corrections can substantially affect the Higgs potential, a negative squared mass at the tree level does not necessarily yield a tachyonic spectrum at the physical level, but only indicates a failure of the tree-level description for calculational purposes. We explain how to tackle this technical issue in the example of the NMSSM, in scenarios with light $$\mathcal {CP}$$ CP -odd or $$\mathcal {CP}$$ CP -even singlet-dominated states and show how loop corrections to the Higgs masses and decay widths can be derived with the regularized Lagrangian. We further explore how the same flexibility in the definition of tree-level parameters can be exploited to circumvent large deviations of the tree-level spectrum from the kinematical setup in Higgs decays, or to estimate the theoretical uncertainty associated with the discrepancy between tree-level and physical Higgs spectra. The latter is of particular relevance for the properties of the SM-like Higgs boson in supersymmetry-inspired models.

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“…1 is most likely to be higgsino-dominated or singlinodominated dark matter [47][48][49][50][51][52][53][54][55][56][57][58][59]. However, dedicated studies on a possible bino-dominated dark matter in the context of the NMSSM are lacking [60].…”

Section: Introductionmentioning

confidence: 99%

Dark matter in the NMSSM with small $λ$ and $κ$

Almarashi¹,

F.²,

R.³

et al. 2022

Preprint

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The NMSSM provides an excellent dark matter candidate, usually the lightest neutralino ( χ0 1 ) being the lightest supersymmetric particle (LSP), in the universe. It is a mixture of the bino, the neutral wino, the neutral higgsinos, and the singlino. In this work, we investigate the features of the lightest neutralino by concentrating on a specific region of the NMSSM parameter space with small values of both λ and κ, taking into account theoretical and experimental constraints, including relic density, direct and indirect detection constraints. We have found that the LSP dark matter is a singlino-dominated neutralino for most of the sample points of the chosen scenario. Thus, contrary to expectations, the NMSSM is not comparable to the MSSM in terms of dark matter properties as λ and κ are very small. The LSP can also be either higgsino-dominated or bino-dominated in some parameter space. The most important parameters affecting the mass and properties of the LSP are κ, λ/κ, and µ eff . Further, we notice that σ SI p ≈ 1.02 σ SI n and σ SD p ≈ 0.76 σ SD n for all the surviving sample points.

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Current bounds and future prospects of light neutralino dark matter in the NMSSM

Cited by 21 publications

References 187 publications

How warm are non-thermal relics? Lyman-$α$ bounds on out-of-equilibrium dark matter

How warm are non-thermal relics? Lyman-$α$ bounds on out-of-equilibrium dark matter

Curing tachyonic tree-level syndrome in NMSSM light-singlet scenarios

Dark matter in the NMSSM with small $λ$ and $κ$

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