Supersymmetric dark matter after LHC run 1

Abstract

Different mechanisms operate in various regions of the MSSM parameter space to bring the relic density of the lightest neutralino, , assumed here to be the lightest SUSY particle (LSP) and thus the dark matter (DM) particle, into the range allowed by astrophysics and cosmology. These mechanisms include coannihilation with some nearly degenerate next-to-lightest supersymmetric particle such as the lighter stau , stop or chargino , resonant annihilation via direct-channel heavy Higgs bosons H / A, the light Higgs boson h or the Z boson, and enhanced annihilation via a larger Higgsino component of the LSP in the focus-point region. These mechanisms typically select lower-dimensional subspaces in MSSM scenarios such as the CMSSM, NUHM1, NUHM2, and pMSSM10. We analyze how future LHC and direct DM searches can complement each other in the exploration of the different DM mechanisms within these scenarios. We find that the coannihilation regions of the CMSSM, NUHM1, NUHM2 can largely be explored at the LHC via searches for events and long-lived charged particles, whereas their H / A funnel, focus-point and coannihilation regions can largely be explored by the LZ and Darwin DM direct detection experiments. We find that the dominant DM mechanism in our pMSSM10 analysis is coannihilation: parts of its parameter space can be explored by the LHC, and a larger portion by future direct DM searches.

Dark Matter Still at Large

“…The expected spectrum of coherent neutrino-nucleus scattering by 8 B solar neutrinos can be fit by a WIMP model as in [48], plotted here as a black dot. Parameters favored by SUSY CMSSM [49] before this result are indicated as dark and light gray (1− and 2 − σ) filled regions.…”

Scenarios for gluino coannihilation

“…The total density of cold dark matter is very tightly constrained by measurements of the cosmic microwave background radiation [13]. It is clear, therefore, that the parameters of generic models are constrained in very specific ways in order to realize the correct dark matter density [14][15][16][17][18][19][20][21][22][23][24][25][26][27][28][29][30][31]. Moreover, this parameter space with the correct density is likely to be found in a region of parameter space where the density varies rapidly with the parameters.…”

Probing SUSY effects in K0 S → μ+μ−

“…In this scenario, the relic density is mostly function of the LSP mass, which fulfills the measured density [83] at m χ 0 1 ≈ 1 TeV [84][85][86][87]. Thus, we perform a scan with |µ| = 1 TeV < M 1 .…”