Leptogenesis and Dark Matter-Nucleon Scattering Cross Section in the SE6SSM

The E6 inspired extension of the minimal supersymmetric (SUSY) standard model (MSSM) with an extra U(1)_N gauge symmetry, under which right-handed neutrinos have zero charge, involves exotic matter beyond the MSSM to ensure anomaly cancellation. We consider the variant of this extension (SE6SSM) in which the cold dark matter is composed of the lightest neutral exotic fermion and gravitino. The observed baryon asymmetry can be induced in this case via the decays of the lightest right-handed neutrino/sneutrino into exotic states even for relatively low reheating temperatures T_R<10^{6-7} GeV. We argue that there are some regions of the SE6SSM parameter space, which are safe from all current constraints, and discuss the implications of this model for collider phenomenology.


Introduction
The observed baryon asymmetry and the presence of cold dark matter in the Universe stimulates the investigation of extensions of the Standard Model (SM). New physics beyond the SM permits to induce the baryon asymmetry if Sakharov conditions are fulfilled [1]. The proposed new physics scenarios include baryogenesis in Grand Unified theories (GUTs) [2]- [8], the Affleck-Dine mechanism [9,10], baryogenesis via leptogenesis [11], electroweak baryogenesis [12]- [13], etc . In the case of thermal leptogenesis [11] lepton asymmetry is generated due to the decays of the lightest right-handed neutrino. The realisation of this mechanism within the type I seesaw models [14], in which CP and lepton number are violated, allows for understanding of the mass hierarchy in the lepton sector if the right-handed neutrinos are superheavy. In this scenario the induced lepton asymmetry gets partially converted into baryon asymmetry via sphaleron processes [15,16].
After inflation in the reheating epoch, which is characterized by a reheat temperature T R , the right-handed neutrinos can be produced by thermal scattering if T R > M 1 . In the SM and minimal supersymmetric (SUSY) standard model (MSSM) such production process results in the appropriate baryon asymmetry only when the lightest right-handed neutrino mass M 1 is larger than 10 9 GeV [17,18]. Therefore thermal leptogenesis in the MSSM and its extensions may take place when T R 10 9 GeV. This lower bound on the reheat temperature leads to the gravitino problem [19,20] in the supergravity (SUGRA) models, that lead to the sparticle mass scale below 10 TeV. Indeed, so high T R gives rise to an overproduction of gravitinos. Since gravitinos are sufficiently longlived they tend to decay after Big Bang Nucleosynthesis (BBN). Such decays destroy the agreement between the predicted and observed light element abundances. To preserve the success of BBN the relic abundance of gravitinos has to be relatively small. It becomes low enough if reheat temperature is lower than 10 6−7 GeV [21]- [23].
In this context it seems to be interesting to study the generation of matter-antimatter asymmetry and formation of cold dark matter in the framework of well motivated E 6 inspired extensions of the SM. In the E 6 inspired composite Higgs model (E 6 CHM) [24,25] the process of the baryon asymmetry generation was explored in [26,27]. The E 6 inspired U(1) extensions of the MSSM implies that near the GUT scale M X the E 6 gauge group is broken down to SU(3) C × SU(2) W × U(1) Y × U(1) ′ (for review see [28,29]) where SU(3) C × SU(2) W × U(1) Y is the SM gauge group and U(1) ′ = U(1) χ cos θ E 6 + U(1) ψ sin θ E 6 . (1) In Equation (1) the U(1) ψ and U(1) χ symmetries are associated with the subgroups E 6 ⊃ SO(10) × U(1) ψ and SO(10) ⊃ SU(5) × U(1) χ . The E 6 inspired U(1) extensions of the MSSM can originate from the heterotic superstring theory with E 8 ×E ′ 8 -gauge symmetry. Some phenomenological consequences of the heterotic string model were considered in [30,31].
Within the SUSY models with extra U(1) ′ the anomalies are canceled if the particle spectrum contains complete representations of E 6 . Because of this the particle spectrum in the models under consideration is usually extended by the supermultiplets of exotics so that it consists of three 27-dimensional representations of E 6 (27 i with i = 1, 2, 3) at low energies. These 27-plets decompose under SU(5) × U(1) ψ × U(1) χ as follows: Here the first, second and third quantities in brackets are the SU(5) representation as well as U(1) ψ and U(1) χ charges. The SM family, which consists of the doublets of left-handed quarks Q i and leptons L i , right-handed up-and down-quarks (u c i and d c i ) as well as right-handed charged leptons (e c i ), corresponds to 10,  [32,33] (for recent review see [34]), the right-handed neutrinos can be rather heavy inducing the mass hierarchy in the lepton sector. The heavy Majorana right-handed neutrinos are allowed to decay into final states with lepton number L = ±1, resulting in lepton and baryon asymmetries in the early Universe [35]- [37]. In the U(1) N extensions of the MSSM the extra exotic states with the TeV scale masses can give rise to rapid proton decay and flavor-changing transitions. The corresponding operators can be suppressed in the E 6 SSM using a set of discrete symmetries [32,33].
In this article we focus on the variant of the E 6 SSM (SE 6 SSM) in which a singlẽ Z H 2 symmetry forbids non-diagonal flavor transitions and most dangerous operators that violate baryon and lepton numbers. In the next section the SE 6 SSM is specified. In section 3 the thermal leptogenesis within this U(1) N extension of the MSSM is considered. The interactions of the dark matter states with the nucleons is explored in section 4. In Section 5 we summarize the results of our studies and discuss the implications of the SUSY model under consideration for collider phenomenology. At very high energies the E 6 orbifold SUSY GUTs can be reduced to an effective rank-6 [38]. If the particle content of this rank-6 model involves just three 27-plets at low energies then the most general renormalisable superpotential comes from the 27 × 27 × 27 decomposition of E 6 and can be written as where the summation over repeated indexes is implied and i, j, k = 1, 2, 3.
From Equation (3) it follows that if all Yukawa couplings in W 1 and W 2 have nonzero values then one cannot define the baryon (B) and lepton (L) numbers so that the Lagrangian of this model is invariant under the corresponding U(1) B and U(1) L global symmetries. Therefore, as in the simplest SUSY extensions of the SM, the gauge symmetry in the E 6 inspired SUSY models does not forbid the operators which violate lepton and baryon numbers. This means that in general these models lead to rapid proton decay.
Moreover, since three pairs of H u i and H d i couple to charged leptons and ordinary quarks the corresponding Yukawa interactions may give rise to unacceptably large flavor changing processes at the tree level. In particular, these interactions can induce new channels of muon decay such as µ → e − e + e − and contribute to the amplitude of where M P l = (8πG N ) −1/2 ≃ 2.4 · 10 18 GeV is the reduced Planck mass. When 16 GeV, the observed pattern of masses and mixing angles of the left-handed neutrinos can be obtained.
In addition to three complete 27-plets the splitting of bulk 27 ′ supermultiplets in the supermultiplets are expected to be odd under this discrete symmetry [39].
TheZ H 2 symmetry forbids all terms in the SE 6 SSM superpotential that come from actions which originate from 27 ′ l × 27 ′ m × 27 ′ n and 27 ′ l × 27 i × 27 k . Here indexes l, m, n are associated with the supermultiplets M l . As a consequenceZ H 2 symmetry forbids all Yukawa interactions in W 1 eliminating the most dangerous operators leading to rapid proton decay. On the other hand this symmetry allows the terms (Q i L 4 )D k in the superpotential that permits the lightest exotic colored state (quark or squark) to decay. In the SE 6 SSM all charged leptons and the down-type quarks couple to just H d while the up-type quarks interact with H u only. Thus at tree-level non-diagonal flavor transitions are suppressed.
Using the results of the analysis presented in [80]- [82], it was shown that within the E 6 SSM and its simplest modifications the lightest SUSY particles (LSPs) are linear superpositions of the fermion components of the superfields S i [60,77]. In the simplest scenarios these states are either massless or have masses which are much smaller than 1 eV forming hot dark matter in our Universe. The presence of very light neutral fermions may have interesting implications for the neutrino physics (see, for example [83].
To avoid the appearance of the exotic fermions with tiny masses it is assumed that the low energy matter content of the SE 6 SSM involves at least four E 6 singlet superfields.
One of these superfields φ is even under theZ H 2 symmetry whereas three others φ i are odd. The SE 6 SSM implies that H u and H d get combined with the superposition of the appropriate components from the 27 i , composing vectorlike states with masses of order M X . At the same time the components of the supermultiplets S and S as well as L 4 and L 4 gain the TeV scale masses. The presence of L 4 and L 4 at low energies facilitates the gauge coupling unification [55] and permits the lightest exotic colored state (quark or squark) to decay within a reasonable time. As a result the components of the supermultiplets survive to low energies, i.e. they have masses which are many orders of magnitude smaller than M X . Here i = 1, 2, 3 and α = 1, 2. The U(1) N and U(1) Y charges of the supermultiplets listed in Equation (5) are given in Table 1. It is worth noting that the superfields φ i , N c i and φ do not participate in the gauge interactions. Therefore these superfields are not included in Table 1. The most general renormalisable superpotential of the SE 6 SSM, which is allowed by

is given by
where In Equations (6)-(8) α, β = 1, 2 and i, j = 1, 2, 3 as before. In the superpotential of the SE 6 SSM the U(1) N symmetry forbids the term µH d H u . However all other terms, which are present in the MSSM superpotential, are allowed. In Equation (6) GeV. These VEVs generate the masses of all SM particles triggering the breakdown of the SU(2) W × U(1) Y symmetry down to U(1) em associated with electromagnetism. Since we further focus on the scenarios with most sparticles at the multi-TeV scale a substantial degree of tuning is needed to stabilize the EW scale.
For the analysis of the phenomenological implications of the SE 6 SSM it is worth to The components of all other supermultiplets are Z E 2 even. Because the Lagrangian of the SE 6 SSM is invariant under bothZ H 2 and Z M 2 symmetries, the Z E 2 symmetry and Rparity are also conserved. This means that the exotic states, which are odd under the Z E 2 symmetry, can only be created in pairs in collider experiments and the lightest exotic particle as well as the lightest R-parity odd state have to be stable and may contribute to the density of dark matter. Here we focus on the scenarios in which gravitino is the lightest R-parity odd state. Recently the cosmological implications of the gravitino with mass m 3/2 ∼ KeV were discussed [84]. It is also assumed that the lightest stable exotic state is predominantly formed by the fermion components of H d α and H u α . In order to find a viable scenarios with stable gravitino one needs to ensure that the lightest unstable R-parity odd (or exotic) state Y decays before BBN, i.e. its lifetime τ Y 1 sec. Otherwise the decay products of Y can alter the abundances of light elements which are induced by the BBN. The lifetime of the particle Y decaying into gravitino and its SM partner (or the lightest Z E 2 odd state) can be estimated as [85] τ Y ∼ 48π where m Y is its mass. For m Y ≃ 1 TeV one can get τ Y 1 sec if m 3/2 1 GeV. When gravitinos originate from scattering of particles in the thermal bath their contribution to the dark matter density is proportional to the reheating temperature T R [86,87] In Equation (10) Mg is a gluino mass. Since Ω 3/2 h 2 ≤ 0.12 [88], for m 3/2 ≃ 1 GeV and Mg 3 TeV one finds an upper bound T R 10 6−7 GeV [89].

Generation of lepton and baryon asymmetries
Even for so low reheating temperatures the appropriate amount of the lepton asymmetry can be induced within the SE 6 SSM via the out-of equilibrium decays of the lightest righthanded neutrino/sneutrino. Due to (B+L)-violating sphaleron interactions the generated lepton asymmetry is converted into the baryon asymmetry.
In the SM the process of the generation of lepton asymmetry is controlled by the three flavor CP (decay) asymmetries ε 1, ℓ k which are associated with three lepton flavors.
These decay asymmetries appear on the right-hand side of Boltzmann equations. They are defined as Here Γ N 1 ℓ k and Γ N 1lk are partial widths of the lightest right-handed neutrino decays At the tree level Γ N 1 ℓ k = Γ N 1lk and CP asymmetries (11) vanish. The non-zero contributions to the decay asymmetries come from the interference between the tree-level amplitudes of the decays of N 1 and one-loop corrections to them if CP invariance is violated in the lepton sector.
In the MSSM the decays of the lightest right-handed neutrino into Higgsino H u and sleptons L k also contribute to the lepton asymmetry generation. The corresponding flavor decay asymmetries are given by Moreover supersymmetry predicts the existence of the lightest right-handed sneutrino N 1 which is a scalar partner of N 1 . The decays of N 1 into slepton and Higgs as well as into lepton and Higgsino provide another possible origin of lepton asymmetry. The corresponding decay asymmetries can be determined similarly to the neutrino ones When the sparticle mass scale M S is considerably smaller than M 1 Assuming the type I seesaw models of neutrino mass generation the decay asymmetries mentioned above were initially computed within the SM [90]- [93] and MSSM [94]- [96].
Flavor effects were ignored in the early studies of leptogenesis (see for example [97]). The importance of these effects was emphasised in [98]- [104].
The non-minimal SUSY models (like the SE 6 SSM) may include additional SU(2) W doublets with quantum numbers of Higgs fields (H d α and H u α ) and extra lepton multiplets (L 4 and L 4 ) at low energies. It is convenient to denote all Higgs like multiplets and SU(2) W lepton doublets, that interact with the right-handed neutrino superfields, as H u k and L x respectively. In the case of the SE 6 SSM H u 3 ≡ H u , k = 1, 2, 3 and x = 1, 2, 3, 4. If the components of additional Higgs like and lepton supermultiplets are lighter than N 1 and N 1 they can give rise to new decay modes of the lightest right-handed neutrino and its superpartner. Each new channel of the decays of N 1 and N 1 should lead to extra CP asymmetry that contributes to the lepton asymmetry generation. In this case the definitions of the decay asymmetries (11)-(13) need to be generalised. In particular the definitions (11)- (12) can be modified in the following way [36] ε where f and f ′ may be either ℓ x or ℓ x whilef andf ′ should be associated with eitherl The CP asymmetries associated with the decays of the lightest right-handed sneutrino ε k 1, f can be defined similarly to ε k 1, f . In order to get the appropriate expressions for ε k 1, f the field of the lightest right-handed neutrino in Equation (15) ought to be replaced by either N 1 or N * 1 . In the limit, when the sparticle mass scale M S is negligibly small as compared with M 1 , all soft SUSY breaking terms can be safely ignored and the relation between different decay asymmetries (14) remains intact, i.e. ε k 1, f = ε k 1, f . Within the SE 6 SSM ε 3 1, ℓn (ε 3 1, ℓn ) with n = 1, 2, 3 are flavor decay asymmetries associated with the decays of N 1 into Higgs doublet H u and ordinary leptons (Higgsino H u and sleptons), whereas ε 3 1, ℓn (ε 3 1, ℓn ) are CP asymmetries corresponding to the decays of N 1 into leptons and Higgsino H u (sleptons and Higgs doublet H u ). Additional decay asymmetries and ε α 1, ℓ 4 in this SUSY model arise due to the extra decay channels of N 1 and N 1 The structure of the part of the SE 6 SSM superpotential W N (8), that describes the in- that control the process of lepton asymmetry generation. At the tree level the partial widths corresponding to the new decay channels (16) are given by and CP asymmetries ε α 1, ℓ 4 , ε α The analytical expressions for the CP asymmetries (18)  h j1 = |h j1 |e iϕ j1 the expressions for other CP asymmetries reduce to [36,37] where ∆ϕ j1 = ϕ j1 − ϕ 11 . From the part of the SE 6 SSM superpotential (8) one can see the supermultiplets H u α may be redefined so that only H u 1 interacts with N c 1 and L 4 . Thus h 12 in W N may be set to zero without loss of generality. It is also worth noting that the scalar and fermion components of the supermultiplet L 4 being produced in the decays of N 1 and N 1 sequentially decay into ordinary leptons inducing lepton number asymmetries.
The evolution of the U(1) B−L number densities is described by the Boltzmann equations. In the scenarios under consideration the results for the baryon and lepton asymmetries obtained within the SM and MSSM can be easily generalised. In particular, the generated total baryon asymmetry may be estimated using an approximate formula [105]: where Y ∆B is the baryon asymmetry relative to the entropy density. In Equation (20) η is an efficiency factor that varies from 0 to 1. The efficiency factor in the so-called strong washout scenario can be estimated as follows Here M P = 1.22 · 10 19 GeV, H is the Hubble expansion rate and g * = n b + 7 8 n f is the number of relativistic degrees of freedom in the thermal bath. In the SE 6 SSM g * ≈ 360.
In order to simplify our numerical analysis we set |h 12 | = |h 31 | = 0. Our results are summarised in Figure 1. The decay asymmetries (19) are determined by |h 21 |, (M 2 /M 1 ) and combination of the CP-violating phases ∆ϕ 21 , but do not depend on |h 11 |.
Here we fix ∆ϕ 21 so that these asymmetries attain their maximum absolute values, i.e.

Dark matter-nucleon scattering cross section
The scalar components of the supermultiplets φ i , S i , H u α and H d α do not acquire VEVs. Their fermion components form the exotic (inert) neutralino and chargino states. The signatures associated with the inert neutralino states were examined in [106,107]. When the components of φ i are significantly heavier than the fermions and bosons from S i , H u α and H d α , they can be integrated out so that W IH reduces to Here and further we work in a field basis in which µ ij = µ i δ ij and λ αβ = λ αα δ αβ .
In this article we explore the scenarios in which the fermion components of the where µ 11 ≃ λ 11 S . Instead of the VEVs of H d and H u , i.e. v 1 and v 2 , it is more The charged fermion components of the supermultiplets H u 1 and H d 1 form the lightest exotic chargino. Its mass is determined by µ 11 , i.e. m χ ± 1 = |µ 11 |. If | µ 1 | is considerably larger than |µ 11 | and v the mass matrix (23) can be diagonalised.
Using the perturbation theory method (see, for example, [108]- [111]), one finds [49] , As follows from Equation (24)  Since in the scenarios under consideration the lightest neutral exotic neutralino χ 1 is stable its contribution to the cold dark matter density may be estimated using formula The approximate formula (25) was derived within the MSSM [112,113]. On the other hand the Planck observations lead to (Ωh 2 ) exp = 0.1188±0.0010 [88]. Therefore in the phenomenologically viable scenarios µ 11 should be lower than 1.1 TeV. When µ 11 < 1.1 TeV, gravitino can account for some or major part of the cold dark matter density.
In the SE 6 SSM the interactions of the cold dark matter with the SM particles are determined by the couplings of χ 1 because the corresponding gravitino couplings are negligibly small. The low energy effective Lagrangian, that describes the interactions of the lightest exotic neutralino with quarks can be written as The first term in the brackets results in a spin-independent interaction whereas the second one gives rise to a spin-dependent interaction.
In the scenarios under consideration the dominant contribution to the parameters d q in the Lagrangian (26) stems from t-channel Z boson exchange. Taking into account that in the field basis (H d0 1 ,H u0 1 ,S 1 ) where N a i is the exotic neutralino mixing matrix defined by the part of the Lagrangian, which describes the interactions of the lightest and second lightest exotic neutralino states with Z, may be presented in the following form: In Equation (28) M ab is 3 × 3 mass matrix (23). Then the parameters d q as well as the corresponding χ 1 -proton and χ 1 -neutron scattering cross sections (σ p and σ n ) are given by σ p,n = 12m 2 r π q=u,d,s Here m N is a nucleon mass and T 3q is the third component of isospin. We set ∆ p u = ∆ n d = 0.842, ∆ p d = ∆ n u = −0.427 and ∆ p s = ∆ n s = −0.085 [113]. In the SE 6 SSM χ 1 does not couple to squarks and quarks. As a consequence the only contributions that parameters a q receive, come from the t-channel exchange of Higgs scalars. Since in the scenarios under consideration all Higgs bosons except the lightest Higgs scalar h 1 are expected to be considerably heavier than 1 TeV, all contributions caused by the heavy Higgs exchange can be neglected. The lightest Higgs boson with mass m h 1 ≈ 125 GeV manifests itself in the interactions with the SM states as a SM-like Higgs in this case so that where m q is a quark mass and g hχχ is the coupling of the lightest exotic neutralino to h 1 .
The spin-independent part of χ 1 -nucleon cross section takes the form [114,115] The value of σ SI depends quite strongly on f N T q , i.e. hadronic matrix elements. We fix f N T s ≃ 0.0447, f N T d ≃ 0.0191 and f N T u ≃ 0.0153 which are the default values used in micrOMEGAs [116] (see also [117]- [120]). Using the perturbation theory method it is straightforward to obtain the approximate expressions for g hχχ and R Z11 . If µ 1 ≫ µ 11 > 0 and µ 11 is substantially larger than f 11 v cos β andf 11 v sin β, one finds In our analysis we restrict our considerations to moderate values of tan β, i.e. Higgs boson have masses beyond the multi-TeV range [32]- [33], [72]- [73]. Therefore they cannot be observed at the LHC. The realisation of such scenarios requires a significant fine-tuning, ∼ 0.01%, of the parameters of the model under consideration [121].
LHC experiments ruled out the U(1) N gauge boson with masses M Z ′ below 4.5 TeV [122,123]. If S ≃ S the mass of the Z ′ boson in the SE 6 SSM is given by where g ′ 1 and Q S are the U(1) N gauge coupling and the U(1) N charge of the superfield S. The low-energy value of g ′ 1 can be calculated assuming the unification of gauge couplings [32]. Then M Z ′ 4.5 TeV can be obtained when S ≃ S 6 TeV. To avoid the lower experimental bound on the lightest exotic chargino mass we assume that µ 11 200 GeV.
To ensure that χ 1 leads to the phenomenologically acceptable density of the cold dark matter the interval of variations of µ 11 is limited from above by 1 TeV so that λ 11 0.17.
In addition, the validity of perturbation theory up to the GUT scale is required that constrains the range of variations of f 11 andf 11 at low energies. We also set µ 1 ≃ 2 TeV.
The results of our numerical analysis are presented in Figures  However as follows from Figures 2 and 3 in order to achieve the desirable suppression of the σ SI and σ p,n the fine-tuning is not needed. In our analysis f 11 is chosen to be positive whilef 11 is fixed to be negative. As a consequence g hχχ , |R Z11 |, the spin-independent and spin-dependent cross sections decrease when f 11 grows and approaches −f 11 tan β. It is worth to point out that in the part of the parameter space of the SE 6 SSM where the couplings |g hχχ | and |R Z11 | become considerably smaller than 10 −3 one cannot neglect the contributions to σ SI and σ p,n which are induced by the heavy Higgs states and Z ′ boson.
Moreover one should take into account the quantum corrections to the Lagrangian (26) that stem from the one-loop diagrams involving the electroweak gauge bosons [124,125].
In the SE 6 SSM the maximal values of the spin-independent and spin-dependent χ 1nucleon scattering cross sections are much larger than σ SI and σ p,n presented in Figures 2 and 3. These cross sections attain their maximal possible values for µ 11 ≃ µ 1 and f 11 ∼ f 11 ∼ 1. In this case σ SI can reach 20 − 30 zb which is considerably larger than the corresponding experimental limit [127]. Since for a given mass of the lightest exotic fermion σ SI vanishes when f 11 = −f 11 tan β, the spin-independent χ 1 -nucleon scattering cross section varies from zero to its maximal value for each m χ 1 . In the scenarios under consideration the suppression of σ SI and σ p,n is caused by the cancellations of different contributions to R Z11 and g hχχ as well as by the large value of µ 1 that should be associated with the sparticle mass scale M S . In the near future the experiments LZ [129], XENONnT [130], DARWIN [131] and DarkSide-20k [132] can set even more stringent limits on σ SI and σ p,n constraining further the parameter space of the SE 6 SSM.

Conclusions
In this article we considered leptogenesis and the interactions of the dark matter with the In the SE 6 SSM the cold dark matter density is formed by two stable neutral states.
Here we focused on the scenarios in which one of these stable particles is gravitino.
In this case all TeV scale states can decay before BBN only when gravitino mass m 3/2 1 GeV. Another stable state tends to be the lightest exotic neutralino χ 1 with mass m χ 1 ≤ 1.1 TeV. Because it is a superposition of the neutral fermion components of the SU(2) W doublets, the lightest exotic chargino χ ± 1 , the second lightest exotic neutralino χ 2 and χ 1 are nearly degenerate around m χ 1 . Such scenarios result in the phenomenologically acceptable dark matter density if the reheating temperatures T R 10 6−7 GeV. Even for so low T R the decays of the lightest right-handed neutrino/sneutrino in the SE 6 SSM can generate the appropriate lepton asymmetry due to the presence of L 4 and L 4 in the particle spectrum. This lepton asymmetry is converted into the observed baryon asymmetry via sphaleron processes. In the scenarios under consideration there is a part of the SE 6 SSM parameter space in which the dark matter-nucleon scattering cross section is substantially smaller than the present experimental limits.
The phenomenological viability of the scenarios under consideration requires χ ± 1 , χ 2 and χ 1 to be lighter than 1.1 TeV. Otherwise the annihilation cross section for χ 1 + χ 1 → SM particles becomes too small giving rise to the cold dark matter density which is considerably larger than its measured value. Relatively light charged and neutral fermions have been searched for in different experiments. If the mass of the lightest exotic chargino m χ ± 1 and the mass of the second lightest exotic neutralino m χ 2 are too close to m χ 1 the decay products of χ ± 1 and χ 2 may escape detection. This happens, for example, within natural SUSY, where the mass splitting between the lightest and second lightest ordinary neutralino states as well as the mass splitting between the lightest ordinary chargino and the lightest ordinary neutralino are at least a few GeV [133]- [135].
In the scenarios under consideration the SE 6 SSM parameters are chosen so that ∆ 1 > 200 MeV while ∆ is larger than 300 MeV [126,136]. Therefore χ ± 1 and χ 2 cannot be long-lived. At the LHC the lightest exotic chargino and neutralino states can be produced in pairs via off-shell W and Z-bosons. Then χ ± 1 and χ 2 subsequently decay into hadrons and χ 1 . For ∆ ≃ 4.7 GeV(2 GeV) ATLAS ruled out χ ± 1 with masses below 193 GeV(140 GeV) [137]. For ∆ = 1 GeV CMS excluded χ ± 1 with masses below 112 GeV [138]. The discovery prospects for such exotic chargino and neutralino states look more promising at future International Linear Collider (for a review see [139]).
The SE 6 SSM also predicts the existence of other exotic neutralino and chargino states.
Two exotic neutralino states and the second lightest exotic chargino are formed by the fermion components of the SU(2) W doublets. These fermions as well as their superpartners might be either light or heavy depending on the SE 6 SSM parameters. Due to the Z E 2 symmetry conservation in the collider experiments all exotic particles can only be created in pairs. Since the exotic neutralino and chargino as well as their scalar partners do not couple to quarks/squarks directly at the LHC these states can be produced via the EW interactions. As a consequence their production cross section remains relatively small even if the corresponding states have masses around 1 TeV. The conservation of R-parity and Z E 2 symmetry implies that the final state in the decay of the exotic fermions involves at least one lightest exotic neutralino while the final state in the decay of its scalar partner should contain at least one lightest exotic neutralino and one gravitino. If both of the produced states decay into on-shell gauge bosons it is expected that they should result in some enhancements in the rates of p p → Z Z + E miss T + X , p p → W Z + E miss T + X , p p → W W + E miss T + X , (35) where E miss T is associated with the lightest exotic fermion (and gravitino) and X should be identified with jets and/or extra charged leptons that may stem from the decays of intermediate states.
As mentioned before, the components of L 4 and L 4 are expected to be relatively light.
When all other exotic states and sparticles except χ ± 1 , χ 2 , χ 1 and gravitino are rather heavy, the scalar (L 4 ) and fermionic (L 4 ) components of the supermultiplets L 4 and L 4 can be produced in pairs via off-shell W and Z-bosons. Their decays always lead to either τ -lepton or electron/muon as well as missing energy in the final state. In the case ofL 4 decays the missing energy in the final state can be associated with only one lightest exotic neutralino while the final state of the L 4 decays has to involve at least one lightest exotic neutralino and one gravitino to ensure the conservation of R-parity and Z E 2 symmetry. More efficiently L 4 and/orL 4 can be produced through the decays of the lightest exotic colored states if these states are relatively light and the corresponding decay channels are kinematically allowed.
Finally it is worth emphasising that the SE 6 SSM predicts the existence of extra quarks and their scalar superpartners that carry lepton and baryon numbers simultaneously [38].
The LHC lower bounds on the scalar leptoquark masses [140]- [142] are not directly applicable in this case. Indeed, ordinary scalar leptoquark with electric charge −1/3 decays either to the left-handed neutrino ν j and down-type quark d i or to charged lepton ℓ j and up-type quark u i . The lightest exotic colored state q 1 in the SE 6 SSM, which is a superposition of either scalar or fermion components of the supermultiplets D i and D i , is odd underZ E 2 symmetry. As a consequence its decays always lead to the missing energy E miss T in the final state The pair production of the lightest exotic colored states at the LHC may result in the enhancement of the cross sections of pp → jj +E miss T +X and/or pp → jjℓ klm +E miss T +X.
The LHC pair production cross section of the lightest exotic quarks changes from 10 fb to 1 fb if the mass of q 1 increases from 1.3 TeV to 1.7 TeV [143]. In the case of the lightest exotic squarks the production cross section is an order of magnitude smaller. The presence of Z ′ boson and exotic multiplets of matter in the particle spectrum is a very peculiar feature that should permit to distinguish the SE 6 SSM from the MSSM and other extensions of the SM.