Supergravity Model of Inflation and Explaining IceCube HESE Data via PeV Dark Matter Decay

We construct a unified model of inflation and PeV dark matter with an appropriate choice of no-scale Kähler potential, superpotential, and gauge kinetic function in terms of MSSM fields and hidden sector Polonyi field. The model is consistent with the CMB observations and can explain the PeV neutrino flux observed at IceCube HESE. A Starobinsky-like Higgssneutrino plateau inflation is obtained from the D-term SUGRA potential while F-term being subdominant during inflation. To get PeV dark matter, SUSY breaking at PeV scale is achieved through Polonyi field. This sets the scale for soft SUSY breaking parameters m0,m1/2, A0 at the GUT scale in terms of the parameters of the model. The low-energy particle spectrum is obtained by running the RGEs. We show that the ~125GeV Higgs and the gauge coupling unification can be obtained in this model. The 6 PeV bino-type dark matter is a subdominant fraction (~11%) of the relic density, and its decay gives the PeV scale neutrino flux observed at IceCube by appropriately choosing the couplings of the R-parity violating operators. Also, we find that there is degeneracy in scalar field parameters ðγ, βÞ and coupling ζ value in producing the correct amplitude of CMB power spectrum. However, the value of parameter tan ðβÞ = 1:8, which is tightly fixed from the requirement of PeV scale SUSY breaking, removes the degeneracy in the values of the scalar field parameters to provide a unique solution for inflation. In this way, it brings the explanation for dark matter, PeV neutrinos, and inflation within the same framework.


Introduction
The 125 GeV Higgs boson found at the Large Hadron Collider (LHC) [1][2][3] completes the spectrum of the standard model but raises the question about what protects the mass of the Higgs at the electroweak scale despite quantum corrections (the gauge hierarchy problem). Supersymmetry [4][5][6] has been widely accepted as the natural symmetry argument for protecting the Higgs and other scalar masses against radiative corrections and in addition provides the unification of the gauge couplings at the GUT scale and WIMP dark matter. The idea of naturalness in SUSY [7,8] requires that to explain the Higgs mass, loop corrections should not be too large compared to the tree level and should not rely on the cancellation of large corrections from different loop corrections. This puts upper bounds on the masses of squarks, gluons, and gauginos for natural SUSY [8]. The searches for SUSY particles at LHC by ATLAS [9] and CMS [10] at 13 TeV and with 15f b −1 of data do not find the SUSY partners and rule out the simplest models of natural SUSY [11,12]. The idea of supersymmetry for explaining the Higgs mass without fine-tuning can be abandoned while still retaining some of the positive features like coupling constant unification and WIMP dark matter in split SUSY [13] scenarios where squarks and gluinos are heavy evading the LHC bounds and the electroweakinos are of the TeV scale providing the WIMP dark matter and coupling constant unification. With the tight bounds from the direct detection experiments [14,15], the bino-higgsino dark matter of a few 100 GeV is getting increasingly difficult [16][17][18][19][20][21][22][23][24][25]. The evidence that there is need for new physics at PeV scale comes from IceCube's High-Energy Starting Events (HESE) observations [26][27][28][29] of PeV energy neutrinos. The nonobservation of neutrinos with deposited energy between 0.4 and 1 PeV and at Glashow resonance energies has called for an extra source of PeV energy neutrinos, and a popular scenario [30][31][32][33][34][35] is the decay of PeV scale dark matter with a sizable branching to neutrinos and with a lifetime of~10 15 sec [36] and 10 28 sec [37][38][39][40][41][42][43][44][45][46][47][48][49][50]. Leptoquarks have been used to explain IceCube PeV events in Refs. [51][52][53][54][55][56]. A PeV scale supersymmetry model with gauge coupling unification, light Higgs (with fine-tuning), and PeV dark matter was introduced in [57,58]. It was found [39] that in order to obtain the large decay time of~10 28 sec as required from the observed IceCube neutrino flux, dimension 6 operators suppressed by the GUT scale had to be introduced in the superpotential.
In this paper, we construct a D-term inflation model with no-scale Kähler potential, MSSM superpotential, and an appropriate choice of gauge kinetic function in MSSM fields, which gives a Starobinsky-like Higgs-sneutrino plateau inflation favored by observations. The SUSY breaking scale is a few PeV which provides a PeV scale bino as dark matter. A fraction of thermal relic density is obtained by turning on a small R-parity violation to give a decaying dark matter whose present density and neutrino flux at IceCube is tuned by choosing the R-parity violating couplings. Superysmmetry breaking is achieved by a hidden sector Polonyi field which takes a nonzero vev at the end of inflation. The gravitino mass is a few PeV which sets the SUSY breaking scale. The mSUGRA model has only five free parameters including soft SUSY breaking parameters. These are the common scalar mass m 0 , the common gaugino mass m 1/2 , the common trilinear coupling parameter A 0 , the ratio of Higgs field vevs tanβ, and the sign of mass parameter μ; all are given at the gauge coupling unification scale. The spectra and the couplings of sparticles at the electroweak symmetry breaking scale are generated by renormalization group equations (RGEs) of the above soft breaking masses and the coupling parameters. The sparticle spectrum at the low-energy scale was generated using the publicly available softwares Flexi-bleSUSY [87,88], SARAH [89,90], and SPheno [91,92] with the mSUGRA input parameter set m 0 , m 1/2 , A 0 , tanβ, and sign(μ). In our analysis, we have used SARAH to generate model files for mSUGRA and relic density of LSP has been calculated using micrOMEGAs [93,94].
The paper is organized as follows. In Section 2, we display the MSSM model and the specific form of a Kähler potential and gauge kinetic function which gives the Starobinsky-like Higgs-sneutrino plateau inflation. The R-parity violating terms contribute to the F-term potential and to the decay of the dark matter for IceCube. We fix the parameter in the gauge kinetic function and show that a D-term inflation model consistent with the CMB observations is obtained. In Section 3, we describe the SUSY breaking mechanism from the Polonyi field and calculate the soft breaking parameters m 0 , m 1/2 , A 0 and gravitino mass m 3/2 as a function of parameters of the Polonyi potential. In Section 4, we give the phenomenological consequences of the PeV scale SUSY model. We show that the coupling constant unification can take place and we obtain~125 GeV Higgs mass by fine-tuning. The relic density of the bino LSP is overdense after thermal decoupling, but due to slow decay from the R-parity violation, a fraction of relic density remains in the present epoch. A different R-parity operator is responsible for the decay of the PeV dark matter into neutrinos. We fix the parameters of the R-parity violating couplings to give the correct flux of the PeV scale neutrino events seen at IceCube. In Section 5, we summarize the main results and give our conclusions.

D-Term mSUGRA Model of Inflation
We consider the model with MSSM matter fields and R-parity violation and choose a Kähler potential Kðϕ i , ϕ * i , Z, Z * Þ and gauge kinetic function f ab ðϕ i , ZÞ with the aim of getting a plateau inflation favored by observations. We choose K and f ab of the form respectively. And the MSSM superpotential Wðϕ i Þ 2 Advances in High Energy Physics where and field Z is the hidden sector Polonyi which is introduced to break supersymmetry. The Polonyi field Z is associated with the fluctuations in the overall size of the compactified dimensions which has to be strongly stabilized at SUSY breaking for the successful implementation of inflation in supergravity. The parameters α, κ, μ z , μ zz , and ζ are coupling constants of the model to be fixed from SUSY breaking and inflation. The other fields bear their standard meanings. Also, the above potentials are in the M p = ð8πGÞ −1 = 1 unit and shall use the same convention throughout the analysis of this model. In addition to the superpotential given in equation (3), we also consider the R-parity violating interaction terms which will play a role in explaining observed DM relic density and PeV neutrino flux at IceCube. In supergravity, the scalar potential depends upon the Kähler function Gðϕ i , ϕ * i Þ given in terms of superpotential Wðϕ i Þ and Kähler potential where ϕ i are the chiral scalar superfields. In D = 4, N = 1 supergravity, the total tree-level supergravity scalar potential is given as the sum of F-term and D-term potentials which is given by respectively, where D a = −gð∂G/∂ϕ k Þðτ a Þ l k ϕ l and g is the gauge coupling constant corresponding to each gauge group and τ a are corresponding generators. For SUð2Þ L symmetry τ a = σ a /2, where σ a are Pauli matrices. And the Uð1Þ Y hypercharges of the fields H u , H d , L, Q,ẽ R ,d R , andũ R given in (3) are Y = ð1/2,−1/2,−1/2, 1/6, 1, 1/3,−2/3Þ, respectively. The quantity f ab is related to the kinetic energy of the gauge fields and is a holomorphic function of superfields ϕ i . The kinetic term of the scalar fields is given by where K i j * is the inverse of the Kähler metric K j * We assume that during inflation, SUSY is unbroken and the hidden sector field is subdominant compared to inflaton field so that we can safely assume Z = 0. Also, for charge conservation, we assume that during inflation the charged fields take zero vev. The D-term and F-term potentials are obtained as It can be seen that the above expressions reduce to MSSM D-term and F-term potentials in the small field limit after the end of inflation as the terms coming from Kähler potential and gauge kinetic function are Planck suppressed. Now, for simplification, we parametrize the neutral component fields as For the above parametrization, the kinetic term turns out to be To obtain the canonical kinetic term for the inflaton field and to better understand the inflation potential, we redefine the field ϕ to χ c via For the above field redefinition, the kinetic term becomes Therefore, if the imaginary part of the field χ c is zero, we obtain the canonical kinetic term in real part of field χ c = χ (say). As the field ϕ is a linear combination of the Higgs and sneutrino field, so is the inflaton field χ, we can call this model a Higgs-sneutrino inflation model. The D-term potential (9) in the canonical inflaton field χ becomes 3 Advances in High Energy Physics where λ = ð3/2Þ ððγ 2 + cos ð2βÞÞ/ð1 + γ 2 ÞÞ and we have made a specific choice ζ = ðγ 2 + 1Þ/ð3 sin ðβÞ cos ðβÞÞ which is critical to obtain a plateau behavior potential at large field values which can fix inflationary observables. Since at the GUT scale, the mass parameter μ~0 and SUð2Þ gauge couplings are g 1 = g 2 = 0:62, the D-term potential dominates over F -term potential during inflation when the field values are at the Planck scale. With the canonical kinetic term and scalar potential obtained in canonical inflaton field χ, the theory is now in the Einstein frame. Therefore, we can use the standard Einstein frame relations to estimate the inflationary observables, namely, amplitude of the curvature perturbation Δ 2 R , scalar spectral index n s and its running α s , and tensor-toscalar ratio r, given by respectively. Here, ε, η, and ξ are the slow-roll parameters, given by In order to have flat universe as observed, the universe must expand at least by more than 60e-folds during infla- The field value χ i is at the onset of inflation, when observable CMB modes start leaving the horizon, which can be determined using the following relation once we fix the field value χ f using the condition εðχ f Þ = 1 which corresponds to the end of inflation. From the Planck 2018 CMB temperature anisotropy data in combination with the EE measurement at low multipoles, we have the scalar amplitude, the spectral index, and its running as ln ð10 10 Δ 2 R Þ = 3:044 ± 0:014, n s = 0:9649 ± 0:0042, and α s = −0:0045 ± 0:0067, respectively (68% CL, PlanckTT,-TE,EE+lowE+lensing) [59 -61]. Also, the Planck 2018 data combined with BK15 CMB polarization data put an upper bound on tensor-to-scalar ratio r 0:002 < 0:056 (95% CL, PlanckTT,TE,EE+lowE+lensing+BK15) [62,63]. Armed with the theoretical and observational results, we perform the numerical analysis of the models. From the condition of the end of inflation ε = 1, we find χ e ≃ 1:927. Therefore, requiring N ≃ 60e-fold expansion during inflation, we obtain χ i ≃ 7:03. At χ i ≃ 7:03, CMB observables are estimated to be r ≃ 0:0035, n s ≃ 0:965, and α s ≃ −6 × 10 −4 , consistent with the observations. The ðn s , rÞ predictions are similar to the Starobinsky inflation. For tan ðβÞ = 1:8 and g 1 = g 2 = 0:62, the observed CMB amplitude can be obtained for λ ≃ 1:703 × 10 −5 . From the specific case considered in (15) for successful inflation, we have sneutrino field parameter γ ≃ 0:727 and coupling ζ of the Planck suppressed operator in the guage kinetic function (2) ζ ≃ 1:2. The evolution of the D-term inflaton potential (15) is shown in Figure 1. During inflation, as the inflaton rolls down from χ i ≃ 7 to χ e ≃ 1:9, the potential along the Z direction stays nearly flat implying χ being much heavier than Z. During slow-roll phase, the mass of inflaton varies from m χ i ≃ 2:1 × 10 13 GeV to m χ e ≃ 9:3 × 1 0 12 GeV, whereas the mass parameter associated with the Polonyi field Z varies from m Z i ≃ 6:1 × 10 10 GeV to m Z e ≃  Figure 1: The D-term inflation potential for tan ðβÞ = 1:8, g 1 = g 2 = 0:62 is shown. During inflation, as the inflaton rolls down from χ i ≃ 7 to χ e ≃ 1:9, the potential along the Z direction stays nearly flat implying inflaton χ being much heavier than the Polonyi field Z. For Z ≳ 1, the potential becomes very steep where slow-roll inflation cannot be achieved. 4 Advances in High Energy Physics 2:1 × 10 8 GeV. Hence, m 2 Z ≪ m 2 χ , our assumption that Z is subdominant during inflation and contributes insignificantly to the supergravity inflation potential.
In the next section, we will see that the value of tan ðβÞ = 1:8 used to fix CMB amplitude is absolutely critical in order to get PeV dark matter whose decay explains PeV neutrino events observed at IceCube and reproducing lowenergy particle mass spectrum as shown in Table 1. It is important to mention here that the scalar field parameter values tan ðβÞ = 1:8 and γ ≃ 0:727 are not a unique set of value to obtain the observed CMB amplitude. Instead, it can be obtained for all the pair of values of ðγ, βÞ which satisfy the relation ð3/2Þððγ 2 + cos ð2βÞÞ/ð1 + γ 2 ÞÞ = λ ≃ 1:703 × 10 −5 defined in (15). However, tan ðβÞ = 1:8 fixed from the requirement of PeV scale SUSY breaking removes this degeneracy in ðγ, βÞ in obtaining the correct CMB amplitude, and at the same time, it brings the successful explanation for inflation, dark matter relic density, and PeV neutrino events at IceCube within the same framework.

SUSY Breaking
We assumed that during inflation all the fields including the hidden sector field Z are subdominant compared to inflaton field and supersymmetry is unbroken at the time of inflation. Once the inflation ends, the scalar fields effectively become vanishing and the soft mass terms are generated via SUSY breaking as the field Z settles down to a finite minimum of the Polonyi potential. The Polonyi field Z is associated with the fluctuations in the overall size of the compactified dimensions. For the successful implementation of inflation in supergravity, the strong stabilization of the Polonyi field is required which can be achieved via appropriate choice of Kähler potential, gauge kinetic function, and superpotential in Z. This also allows for a solution of the cosmological Polonyi problem [114,115] (which is a special case of cosmological moduli problem [116,117]) associated with the problem of cosmological nucleosynthesis. Technically, cosmological Polonyi problem is evaded if Z is heavy m Z~O ð100 − 1000Þ TeV and the Polonyi mass is much larger than the gravitino mass, i.e., m 2 Z ≫ m 2 3/2 [70,118,119]. We will see that this problem does not occur in this model.
The appropriately chosen potentials KðZ, Z * Þ and WðZÞ are shown in equations (1) and (3) and the gauge kinetic function in equation (2). The kinetic term for Polonyi field Z is obtained as ð1 + 2αjZj 2 Þj∂ μ Zj 2 and the Polonyi potential is obtained as We take the hidden sector Polonyi field Z to be real. The parameters α, μ z , and μ zz are fixed from the requirement that Z which breaks supersymmetry acquire a minima where the gravitino mass is~OðPeVÞ scale and the Polony potential is positive V F ðZÞ∥0 with a field minimum at Z = Z min . We find the gravitino mass to be and the scalar masses, using m 2 ϕ = ∂ ϕ ∂ ϕ * ðV F ðϕ,ϕ * ,ZÞÞ /∂ ϕ ∂ ϕ * K evaluated at ϕ = 0, Z = Z min , are obtained as where At the GUT energy scale, μ~0, all the scalar masses are equal m 2 ϕ ðu,dÞ = m 2 ϕ i . Now, we calculate the coefficients of the soft SUSY breaking terms which arise from the Kähler potential (1) and superpotential (3). The effective potential of the observable scalar sector consists of soft mass terms which give scalar masses as given by equations (24) and (25) and trilinear and bilinear soft SUSY breaking terms given by [120][121][122]

Advances in High Energy Physics
Here, the coefficients A ijk and B ij are given by From equations (1) and (3), we haveKðZ, Z * Þ = ZZ * + ðα/2ÞðZZ * Þ 2 andŴðZÞ = μ 2 z Z + μ zz Z 3 . The coefficients of normalized massesμ ij and Yukawa couplingsỸ ijk in the trilinear (26) and bilinear (27) terms, respectively, are obtained as We drop the B ij contribution to the scalar masses by taking correspondingμ ij small. Also, from the fermionic part of the SUGRA Lagrangian, the soft gaugino masses can be obtained as [122][123][124] For the choice of gauge kinetic function f ab = e −κ Z δ ab when ϕ ≈ 0 after inflation, we obtain the gaugino mass We show that the Polonyi potential (22) in Figure 2 for the parameters α = 20, μ z ≃ 2:43 × 10 −6 , μ zz ≃ 2:858 × 1 0 −11 , and κ = 0:56 has a minimum at Z min ≃±0:144. These parameter values are fixed at the GUT scale from the requirement to achieve the soft SUSY breaking parameters with the specific choice of tan β = 1:8 and sign of μ > 0 which gives the Higgs mass~125 GeV at electroweak scale satisfying all experimental (LHC, etc.) and theoretical constraints (stability, unitarity, etc.). The gravitino mass and the mass of the Polonyi field come out to be m 3/2 ≃ 2:32 PeV and m z ≃ 31:8 PeV , respectively, which implies m 2 Z ≫ m 2 3/2 and therefore the OðPeVÞ scale oscillations of the Polonyi field near its minimum decay much before the Big Bang nucleosynthesis. This leads to strong stabilization of Z, and therefore, the cosmological Polonyi problem does not arise in this model.
Knowing the soft breaking parameters at a highenergy scale does not tell us anything about the phenomenology we could observe in the experiments such at LHC, direct detection of DM, and IceCube. We need to find these parameters at the low energy. In general, all parameters appearing in the supersymmetric Lagrangian evolve with RGEs. These RGEs are the intermediator between the unified theory at GUT scale and the lowenergy masses and couplings, which strictly depend on the boundary conditions. We apply RGEs to calculate low-energy masses and different branching ratios for the abovementioned set of mSUGRA parameters as the RGEs are coupled differential equations, which cannot be solved analytically. Also, the low-energy phenomenology is complicated due to mixing angles and dependence of couplings on the high-scale parameters; therefore, one has to rely on numerical techniques to solve RGEs. We calculate all the variables as allowed by the present experimental data. There are various programs publicly available such as SARAH, SPheno, and Suspect which can generate two-loop RGEs and calculate the mass spectrum and the couplings at low energy. For this work, we use SARAH  Advances in High Energy Physics 4.11.0 [89,90] to generate the RGEs and other input files for SPheno 4.0.2 [91,92] which generate the mass spectrum, couplings, branching ratios, and decay widths of supersymmetric particles. To study the neutralino as a dark matter candidate, we link the output files of SPheno and model files from SARAH to micrOMEGAs 3.6.8 [93,94] to calculate the number density for a PeV neutralino dark matter. In the next section, we discuss the consequences of a PeV dark matter.

Bino-Dominated DM in the mSUGRA Model
The neutralinos χ i (i = 1, 2, 3, 4) are the physical superpositions of two gauginos, namely, binoB and winoW 3 , and two higgsinosH u0 andH d0 . The neutralino mass matrix is given by where c b ≡ cos β, c θ ≡ cos θ W , and θ W is the Weinberg mixing angle. M 1 and M 2 are the bino and wino mass parameter at the EWSB scale. The lightest eigenvalue of the above matrix and the corresponding mass eigenstate has good chance of being the LSP. The higgsinos dominantly contribute in LSP for |μ | <M 1,2 , whereas for |μ | > M 1,2 , the LSP can be determined by bino and wino. The lightest neutralino becomes bino-like when M 2 > M 1 . In the mSUGRA model, M 1 and M 2 are equal due to the universality of the gaugino masses at the GUT scale where the value of the gauge coupling constants g 1 , g 2 , and g 3 becomes equal; see Figure 3. However, at low energy, M 2 ≈ ð5g 2 2 ðM Z Þ/3g 2 1 ðM Z ÞÞM 1 [110]. This implies that the LSP is mostly bino-like.

Relic Density and PeV
Excess at IceCube. In this analysis, we present our mSUGRA model with the aim to realize a PeV scale dark matter candidate, which can also explain the IceCube HESE events. IceCube [26][27][28][29] recently reported their observation of high-energy neutrinos in the range 30 TeV-2 PeV. The observation of neutrinos is isotropic in arrival directions. No particular pattern has been identified in arrival times. This implies that the source is not local but broadly distributed. This superheavy neutrino (LSP) might be the dark matter, distributed in the Galactic halo. In this work, we find that the thermally produced LSP can serve as a viable PeV dark matter candidate satisfying the dark matter relic density in the right ball park which also explains the IceCube excess at PeV. However, an annihilating PeV scale dark matter candidate possesses two serious problems.
(1) To maintain the correct relic density using the wellknown thermal freeze-out mechanism requires a very large annihilation cross section, which violates the unitarity bound. The s-wave annihilation cross section of dark matter with a mass M DM is limited by unitarity as [125] (i) The unitarity bound restrict the dark matter mass below 300 TeV [125]. Also, in order to satisfy the unitarity bound, the PeV scale dark matter model produces an overabundance Oð10 8 Þ (depends on the model) of the dark matter (2) The decay time of a particle is in general inversely proportional to its mass. So a PeV scale particle is generically too short-lived to be a dark matter candidate. One has to use fine-tuning [126,127] to stabilize the dark matter as lifetime of the DM particles has to be at least larger than the age of the universe [29,128] Generally, thermal dark matter freeze-out depends on the remaining dark matter in chemical and thermal equilibrium with the SM bath, which leads to depletion of dark matter through Boltzmann suppression [129,130]. We consider the possibility that the dark matter can also decay out of equilibrium to the SM particles via R-parity violation. In the presence of constant s-wave effective annihilation cross section and dark matter decay, the Boltzmann equation is given by Here, we assume that the decay rates of super partner of SM particles other than LSP are much faster than the rate of the expansion of the universe, so that all the particles present at the beginning of the universe have decayed into the lightest neutralino before the freeze-out. Therefore, the density of the lightest neutralino n is the sum of the density of all SUSY particles. τ i,DM is the decay time for the i th process. In nonrelativistic case T < M DM , the equilibrium number density n eq is given by the classical Maxwell-Boltzmann distribution: The entropy density of the universe at temperature T is s = g * T 3 ð2π 2 /45Þ, where parameter g * is the effective degrees of freedom. We use the relation of entropy density and the expansion rate of the universe ðds/dtÞ + 3Hs = 0, in equation (28), to obtain where yield Y is defined as Y ≡ n/s. We solve the above equation for the decaying LSP with large decay time. Before freeze-out annihilation term in equation (30) dominates over the exponential decay term due to very large decay time of LSP. Therefore, integrating equation (30) between the times t = 0 (or T = ∞) the start of the universe and t = t f (or T = T f ) the freeze-out time, the yield Yðt f Þ comes out to be inversely proportional to the thermally averaged effective annihilation cross section hσvi of the dark matter [131]. However, after freeze-out, the annihilation of LSP is no longer large enough and decay term becomes dominant. Therefore, we neglect the annihilation term compared to the decay term and integrate the remaining equation between the freeze-out time t f and the present age of the universe τ U , which, for t U > >t f , gives the yield today as which implies that the number density of LSP reduces with time. Therefore, the relic abundance of LSP in the present universe can be written as where s 0~2 890 cm −3 is the current entropy density and ρ c~1 :05 × 10 −5 h 2 GeV cm −3 is the critical density of the present universe, h = 0:72 is a dimensionless parameter defined through the Hubble parameter H 0 = 100 h km se c −1 Mpc −1 . This implies that the relic density is related to the annihilation cross section and the decay lifetime as Using particle spectrum (see Table 1) in micrOME-GAs, we get σv h i = 6:78 × 10 −26 cm 3 sec −1 : The main contribution to the DM effective annihilation cross section comes from the coannihilation channel (see Figure 4) χ 1 χ ± 1 ⟶ ZW ± which is consistent with unitarity bound [125] and gives the bino-type DM density Ωh 2 ≃ 0:0142 Expð−∑ i ðt U /τ i,DM ÞÞ. The joint results of CMB observations from WMAP and Planck collaboration [132] give Ωh 2 = 0:1198 ± 0:0026. It has been shown that if a subdominant fraction of DM is decaying [36,133], then it can resolve the conflict between σ 8  Advances in High Energy Physics ~5% of DM of mass scale 76 PeV and lifetime 6 × 10 15 seconds is required for explaining the IceCube events [36]. In this paper, we assume that the lifetime of DM decay to leptons via the R-parity violation LLe c operator is 8:9 × 1 0 28 seconds which gives 11% (i.e., Ωh 2 ≃ 0:0142) of the DM relic density and is consistent with the structure formation. The neutrino flux is obtained by this decay channel to give the PeV neutrino flux required to explain the IceCube HESE data [26][27][28][29]. We will explain this result in Section 4.2 in more detail. The presence of R-parity violating coupling 5 can explain the high-energy neutrino events at IceCube. We take only one nonzero dimensionless trilinear R-parity violating couplings, namely, λ 121 coefficient of L e L μ e c . λ 121 helps in producing the neutrino flux through the decay of the neutralino (see Figure 5). We find the decay width for the dark matter decaying into e + μ − ν e and e − μ + ν e [134] as where coupling κ χ 1 e +ẽ− = κ χ 1 μ +μ−~ffi ffi ffi 2 p g 2 [4,5], M χ 1 ≃ 6:3 PeV, and Mẽ− ,μ − ≃ 14:36 PeV (see Table 1). For the lepton number violating coupling λ 121 ≈ 2:82 × 10 −28 , we get the decay time for this channel τ ν,DM ≈ 8:9 × 10 28 sec (see Table 2). It is to be noted that we need very tiny λ's to explain the IceCube HESE data. It indeed has the fine-tuning issue, and the dynamical explanation lies somewhere else. To explain the IceCube HESE data in terms of decaying dark matter, fine-tuning actually seems to be the most "natural" option [56,[95][96][97].

4.2.
Fitting the IceCube Data. In this subsection, we fit the flux of neutrinos observed at IceCube from the decay of the neutralino LSP. The total contribution to the neutrino flux from the atmospheric background and the astrophysical sources along with the galactic (G) DM halo and extragalactic (EG) DM is given by Following the analysis as in Ref. [39] for our mSUGRA model parameters, we compute the number of neutrino events as a function of deposited energy where T E = 2635 is the total exposure time, E dep is the deposited energy in the laboratory frame, and AðE ν Þ is the neutrino effective area for particular lepton flavor [135]. We sum over all the neutrino flavors. Due to low statistical data points at IceCube, it is acceptable to assume that the two energies coincide, i.e., E dep ≃ E ν [41].   We have extracted the atmospheric background data from Ref. [136] and added it to the data from astrophysical sources which come mainly due to the decay of highly energetic pions. The source of these pions could be known sources like active galactic nuclei or the Supernova remnants. We use the power law flux E 2 ν ðdΦ astro /dE ν Þ = Φ 0 ðE ν Þ −γ with Φ 0 = 2:2 × 10 −8 cm −2 sec −1 sr −1 and γ = 0:8 [41] to fit the data from the astrophysical sources. Both the galactic and extragalactic neutrino flux contributions are important to explain the excess neutrino flux around 1-2 PeV [39-43, 53, 135]. We take NFW (Navarro, Frenk, and White) DM density profile to account for the galactic dark matter contribution, where the neutrino energy spectrum dN/dE ν evaluated at our model parameter values has been used [137]. We present the neutrino event distribution in Figure 6. The contribution to the neutrino flux from the DM decay can explain the PeV excess at IceCube.

Conclusions
In this paper, we have constructed a Starobinsky-like Higgssneutrino model of plateau inflation from supergravity D -term in MSSM fields, and 6 PeV bino-type dark matter gives the observed flux of PeV neutrino events at IceCube HESE. A subdominant fraction (~11%) of the DM relic density and its decay to neutrinos is obtained by choosing the couplings of the R-parity violating operators. The SUSY breaking is obtained by the Polonyi field which sets the scale of soft SUSY parameters m 0 , m 1/2 , A 0 , and m 3/2 as a function of the parameters of the model. By running the RGEs, we show the low energy (PeV scale) spectrum of SUSY particles and show that the model can accommodate the~125 GeV Higgs.
The SUSY spectrum so obtained modifies the RGEs above the PeV scale and gives the coupling constant unification at the GUT scale; however, such a gauge coupling unification can be achieved for a large range of SUSY breaking scales. We find that there is degeneracy in the values of inflation model parameters ðγ, β, ζÞ in predicting the correct CMB amplitude. However, tan ðβÞ = 1:8, fixed from SUSY breaking, removes this degeneracy and provides a unique solution for inflation and brings the explanation for dark matter, PeV neutrinos, and inflation within the same model setup.

Data Availability
The data used to support the findings of this study are available from the corresponding author upon request.

Conflicts of Interest
The authors declare that there are no conflicts of interest regarding the publication of this paper. I I  I   I I  I  I I  I   I I  I  I I  I  I I  I  I I  I  I I  I  I I  I   I I  I   I I  I   I I  I   I I  I   I I  I   DM with mass  10 Advances in High Energy Physics