Strong constraints of LUX-2016 results on the natural NMSSM

Abstract

Given the fact that the relatively light Higgsino mass $\mu$ favored in natural supersymmetry usually results in a sizable scattering cross section between the neutralino dark matter and the nucleon, we study the impact of the recently updated direct detection bounds from LUX experiment, including both Spin Independent (SI) and Spin Dependent (SD) measurements, on the parameter space of natural Next-to-Minimal Supersymmetric Standard Model (nNMSSM). Different from the common impression that the SI bound is stronger than the SD one, we find that the SD bound is complementary to the SI bound and in some cases much more powerful than the latter in limiting the nNMSSM scenarios. After considering the LUX results, nNMSSM is severely limited, e.g. for the peculiar scenarios of the NMSSM where the next-to-lightest CP-even Higgs corresponds to the $125 {\rm GeV}$ Higgs boson discovered at the LHC, the samples obtained in our random scan are excluded by more than $85\%$. By contrast, the monojet search at the LHC Run-I can not exclude any sample of nNMSSM. We also investigate the current status of nNMSSM and conclude that, although the parameter points with low fine tuning are still attainable, they are distributed in some isolated parameter islands which are difficult to get. Future dark matter direct search experiments such as XENON-1T will provide a better test of nNMSSM.Comment: 20 pages, 10 figures, meet JHEP published versio

Suppressing the scattering of WIMP dark matter and nucleons in supersymmetric theories

“…Since the Bino field transforms non-trivially under the U (1) Y group of the Standard Model (SM), its coupling with the SM-like Higgs boson is approximated by [9] Cχ0 if the Wino mass is very large, where M 1 and µ are the Bino and Higgsino masses respectively, tan β = v u /v d is the ratio of Higgs vacuum expectation values and α is the mixing angle of CP-even Higgs states. This formula shows that if µ ∼ O(100 GeV), the coupling strength is comparable with that of the electromagnetic interaction, and as a consequence, the cross section of the DM and nucleon scattering is usually above 10 −46 cm 2 for µ 400 GeV [10]. In other words, in order to be consistent with the PandaX-II (2017) experimental results [11], µ should be greater than about 450 GeV at 95% confidence level [12].…”

“…• Finally, if the Singlino and Higgssino fields have a large mass gap in the so-called Singlino-Higgsino scenario [16][17][18], the DM must contain a sizable Higgsino component to enhance its coupling with SM particles, which is necessary to get the correct density. This requires a large enough λ, and consequently leads to a significantly large spin dependent (SD) cross-section for DM-nucleon scattering since [10] σ SD…”

96 GeV diphoton excess in seesaw extensions of the natural NMSSM

“…σ SI ∼ 10 −47 cm 2 for spin-independent (SI) cross section [39] and σ SD ∼ 10 −41 cm 2 for spin-dependent (SD) cross section [40]. Since the t-channel exchange of Higgs bosons (Z boson) is the dominant contribution to the SI (SD) cross section at tree level, the experiment can exclude a large portion of the parameter space in the Higgs sector, especially in case of light Higgsinos and/or light Higgs bosons where strong cancellation between different Higgs contributions must be present to coincide with the experimental results [41,42].…”

Present status and future tests of the higgsino-singlino sector in the NMSSM

“…There mixing between χ 0 1 and the higgsinos χ 0 2,3 cannot be avoided, and the higgsino component of χ 0 1 implies a spin-dependent direct detection rate via Z exchange in conflict with constraints from LUX [22] and PandaX-II [25]. (The importance of recent constraints from spindependent direct detection experiments on the viable parameter space of the NMSSM has recently been underlined in [58].) Also the relic density tends to be too small if χ 0 1 has a -6 - In the blue regions it is impossible to satisfy simultaneously all constraints from a good dark matter relic density, direct dark matter detection cross sections, LEP searches for lighter Higgs bosons and neutralinos, and Higgs signal rates (i.e.…”