Neutralino dark matter detection in split supersymmetry scenarios

Masiero, A.; Profumo, Stefano; Ullio, Piero

doi:10.1016/j.nuclphysb.2005.01.028

Cited by 95 publications

(111 citation statements)

References 88 publications

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“…A thermally generated wino dark matter is underabundant up to ∼ 2 TeV. It satisfies the relic density data for a wino mass of 2-3 TeV 1 [78][79][80][81][82][83][84][85][86][87][88].…”

Section: Jhep09(2017)064mentioning

confidence: 71%

How light a higgsino or a wino dark matter can become in a compressed scenario of MSSM

Chakraborti¹,

Chattopadhyay²,

Poddar³

2017

J. High Energ. Phys.

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Higgsinos and Wino have strong motivations for being Dark Matter (DM) candidates in supersymmetry, but their annihilation cross sections are quite large. For thermal generation and a single component DM setup the higgsinos or wino may have masses of around 1 or 2-3 TeV respectively. For such DM candidates, a small amount of slepton coannihilation may decrease the effective DM annihilation cross section. This, in turn reduces the lower limit of the relic density satisfied DM mass by more than 50%. Almost a similar degree of reduction of the same limit is also seen for squark coannihilations. However, on the contrary, for near degeneracy of squarks and higgsino DM, near its generic upper limit, the associated coannihilations may decrease the relic density, thus extending the upper limit towards higher DM masses. We also compute the direct and indirect detection signals. Here, because of the quasi-mass degeneracy of the squarks and the LSP, we come across a situation where squark exchange diagrams may contribute significantly or more strongly than the Higgs exchange contributions in the spin-independent direct detection cross section of DM. For the higgsino-DM scenario, we observe that a DM mass of 600 GeV to be consistent with WMAP/PLANCK and LUX data for sfermion coannihilations. The LUX data itself excludes the region of 450 to 600 GeV, by a half order of magnitude of the cross-section, well below the associated uncertainty. The similar combined lower limit for a wino DM is about 1.1 TeV. There is hardly any collider bound from the LHC for squarks and sleptons in such a compressed scenario where sfermion masses are close to the mass of a higgsino/wino LSP.

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“…A thermally generated wino dark matter is underabundant up to ∼ 2 TeV. It satisfies the relic density data for a wino mass of 2-3 TeV 1 [78][79][80][81][82][83][84][85][86][87][88].…”

Section: Jhep09(2017)064mentioning

confidence: 71%

How light a higgsino or a wino dark matter can become in a compressed scenario of MSSM

Chakraborti¹,

Chattopadhyay²,

Poddar³

2017

J. High Energ. Phys.

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“…It is clear that the cross section is in general larger in the region |µ| ∼ M 1 , because this is region where the Bino and Higgsino mix strongly. This is also the favored parameter space for the Bino-Higgsino dark matter [5,11,12] corrections to gaugino pair production have been performed [28]. The K factor is about 1.1 − 1.4 depending on SUSY parameters.…”

Section: Production Of Neutralinos and Charginosmentioning

confidence: 99%

Hadronic production and decays of charginos and neutralinos in split supersymmetry

Cheung

Song

2005

Phys. Rev. D

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In the scenario recently proposed by Arkani-Hamed and Dimopoulos, the supersymmetric scalar particles are all very heavy, at least of the order of 10 9 GeV but the gauginos, higgsino, and one of the CP-even neutral Higgs bosons remain light under a TeV. In addition to gluino production, the first SUSY signature would be pair production of neutralinos and/or charginos. Here we study, with explicit CP violation, the production of neutralinos and charginos at hadronic colliders as well as the possible decay modes. We notice that the branching ratio of the neutralino radiative decay can be sizable unlike the case with light sfermions. In particular, the decay of χ 0 3 → χ 0 1 γ has a branching ratio of the order O(1) percent. In colliders, it would give rise to signatures of an isolated single photon plus missing energy.

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“…In the real MSSM, one needs a Higgsino admixture of roughly 25%-30% for the relic density to be within the WMAP range [15,16]. In terms of fundamental MSSM parameters this means M 1 ≈ µ.…”

Section: The Mixed Bino-higgsino Lspmentioning

confidence: 99%