Leptogenesis after superconformal subcritical hybrid inflation

We consider an extended version of superconformal subcritical hybrid inflation model by introducing three right-handed neutrinos that have Majorana mass terms. In the model one of the right-handed sneutrinos plays a role of the inflaton field, and it decays to reheat the universe after inflation. Vacuum expectation value for the waterfall field gives an unconventional pattern of the light neutrino mass matrix, and the neutrino Yukawa couplings that determine the reheating temperature are not constrained by the neutrino oscillation data. Consequently thermal leptogenesis or sneutrino leptogenesis is realized.


Introduction
Inflation paradigm is strongly supported by the observations of the cosmic microwave background radiation (CMB). Slow-roll scalar field in the early universe is a promising candidate for inflation, and many types of inflation models have been proposed so far. In a theoretical point of view, it would be tempting to ask what the underlying physics or symmetry of the inflaton field is. Supersymmetry (SUSY) might be one of the answers. It protects the flatness of the inflaton direction, which is suitable for inflation.
Recently supersymmetric D-term hybrid inflation has been revisited in various point of view. Under shift symmetric Kähler potential [1], subcritical hybrid inflation was found, where inflation continues for subcritical point value of the inflaton field [2,3]. On the other hand, it was shown in Refs. [4,5] that Starobinsky model [6] emerges in the framework of superconformal supergravity [7][8][9][10]. It turned out in the following study that this framework has another new regime of inflation. It was shown that a general class of superconformal α-attractor model [11,12] appears in the subcritical regime of inflation, which we call superconformal subcritical hybrid inflation [13]. In addition, the energy scale of inflation should coincide with the grand unification scale to be consistent with the Planck observation data, which is the feature found in the subcritical hybrid inflation [2,3]. Namely, the superconformal subcritical hybrid inflation has both features of the superconformal α-attractor models and the subcritical hybrid inflation. The shift symmetry and superconformality are crucial for them.
In this paper we will study the thermal history after the end of superconformal subcritical hybrid inflation. (See Refs. [14,15] that study the phenomenology of Pati-Salam version of subcritical hybrid inflation. Recently Ref. [16] comprehensively studies the D-term hybrid inflation, including reheating, leptogenesis, and the SUSY breaking mechanism.) For the purpose, we introduce three right-handed neutrinos that interact with the minimal supersymmetric standard model (MSSM) sector. In fermionic sector, the mass matrix for the light neutrinos is given by the seesaw mechanism [17], but it has an unconventional structure. In bosonic sector, on the other hand, it will be shown that one of sneutrinos can play a role of the inflaton field. In addition, baryon asymmetry that is sufficient amount to explain the observed value is generated via leptogenesis [18]. This paper is organized as follows. In the next section the model that we con-sider is described. Then Sec. 3 shows the conditions required for the superconformal subcritical hybrid inflation in this model. Mass matrices of the heavy and light (s)neutrinos, including parametrization of the neutrino Yukawa couplings, are given in Sec. 4, then we discuss the reheating and leptogenesis after inflation in Sec. 5.
Sec. 6 is dedicated to conclusions.

The model
We consider a model described by the superpotential where W MSSM is the superpotential of the MSSM sector and Here N c i , L i = (ν Li , l Li ) T , and H u = (H + u , H 0 u ) T are the chiral superfields of the right-handed neutrinos, left-handed leptons, and up-type Higgs, respectively, and L j H u = ν Lj H 0 u − l Lj H + u . S ± are the local U(1) fields with charge ±q (q > 0), one of which plays a role of the waterfall field. #1 Indices are summed over i, j = 1 -3. (We will use the same contraction in the following discussion unless otherwise mentioned.) M ij terms are explicit superconformal breaking terms that are added by phenomenological purpose. While we do not argue their origin, M ij 1 are expected. The Kähler potential, on the other hand, is given by where Here I MSSM are chiral superfields in the MSSM sector. The last term is superconformal breaking term that is considered in Refs. [4,10]. With the superpotential and #1 We write the superpartners with tilde for the MSSM fields and right-handed neutrinos. For S ± , the same symbols are used for scalar fields while fermionic parts are expressed with tilde. In the current and the next sections, we adopt the unit in which the reduced Planck mass M pl 2.4 × 10 18 GeV is taken to be unity unless otherwise mentioned.
Kähler potential, the scalar potential is given by where V F and V D are F-and D-terms, respectively, and given by [4] Here Φ ≡ −3Ω −2 and ∆ ≡ Φ − δ αᾱ Φ α Φᾱ have been additionally introduced. Subscript in W and Φ stands for the field derivative, e.g., W α ≡ ∂W/∂z α where z α is a chiral superfield. In the D-term, we have introduced the Fayet-Iliopoulos (FI) term ξ (> 0) associated with the U(1). #2 Due to the FI term, S + has a vacuum expectation value (VEV) at the global minimum, which is obtained as S + = ξ/q(1 +ξ) withξ ≡ ξ/3q.
As in Ref. [13], we take χ i ≤ 0 without loss of generality. In the present model, we impose the following condition: 2ReÑ c 3 has an approximate shift symmetry that is explicitly broken by λ 3 ( 1). Then, φ is expected to be the inflaton as studied in Ref. [13]. In the inflation model, s ≡ √ 2|S + | plays a role of the waterfall field. N c 1 and N c 2 , on the other hand, have no such symmetry. Instead there is a freedom to choose any basis for N c 1 and N c 2 with a redefinition of M ij and λ i due to χ 1,2 0.
Then inflation that is consistent with the observations of the CMB is realized in the parameter space [13], The origin of the FI term in canonical superconformal supergravity model [10] is discussed in Ref. [4]. See also Ref. [16] for recent development.
for q = g = 1, δχ = 0.9 and the number of e-folds N e = 55 -60, which we take in the later numerical study. #3 The mass terms in the superpotential, however, have a possibility to alter the inflationary path. In the next section, we will derive the conditions in order not to affect the inflationary dynamics.

Inflation
We define several variables that are used in the following analysis. During inflation, the other fields except for the inflaton and waterfall field are irrelevant. Thus it is convenient to define following potentials, Then the critical point value φ c is defined as a field value below which the waterfall field becomes tachyonic. It receives O(M 2 ij ) corrections as This perturbative expansion is valid when #4 It will be checked in this section that the above conditions are satisfied in this inflation model.
when potential is expressed in terms of canonically-normalized inflaton field. #3 We will estimate the number of e-folds in Sec. 5.1 to confirm this. #4 We have checked that O(M 4 i3 ) term is irrelevant when Eq. (3.7) is satisfied, thus we ignore it in the following discussion.

Pre-critical regime
Let us begin with the regime where the inflaton is approaching down to the critical point value. Since the waterfall field is stabilized at the origin in this regime, the relevant Lagrangian is given as It is seen that ∆M 2 term gives a gradient to the inflaton field, which should not invade the slow-roll conditions. To see the impact of ∆M 2 term, it is instructive to can be solved easily to obtain, Ψ δχ −1/2 tanh β 1/2φ , (3.13) where β = −(1 + χ)/6 = λ 2 δχ/2qg 2 ξ. Then the potential in terms ofφ is given as On the other hand, it was shown in Ref. [4] that there is one-loop corrections to the tree-level potential. In terms of the canonically-normalized field, it is given by Therefore, in order not to affect the inflationary trajectory, it is sufficient that the terms proportional to |M i3 | 2 are subdominant compared to the one-loop potential.
#5 It is noted that the term proportional to ∆M 2 in Eq. (3.11) is equivalent to In the parameter space given in Eq. (2.11), √ βφ c arcsinh √ βφ c ∼ O(1). Then, the conditions are given as It is easy to check that the slow-roll conditions are satisfied under the constraints.
Since the constraints are more stringent than Eqs. (3.6) and (3.7), it has been confirmed that the perturbative expansion to obtain Eq. (3.3) is valid.

Subcritical regime
In the previous subsection, we have seen that the slow-roll conditions are satisfied before reaching to the critical point value. After the inflaton field becomes subcritical point value, the tachyonic growth of the waterfall field occurs. It is expected that the inflation continues in the subcritical regime when M i3 → 0. In this subsection, we will derive the conditions under which the inflaton and waterfall field dynamics are not affected with non-zero M i3 .
As seen in the previous section, the perturbative expression for φ c is valid under the conditions given in Eqs. (3.17) and (3.18). Then, the tachyonic growth of the waterfall field is not affected by the additional gradient in the inflaton direction due to |M i3 | 2 terms since φ c φ c,0 . Consequently, the dynamics of the waterfall field around the critical point is the same as one discussed in Ref. [13]. Then after the tachyonic growth, the waterfall field relaxes to the local minimum value s min , which is found to be Then the potential in the subcritical regime of the inflaton field is effectively given by V (φ, s min ) and the dynamics reduces to single field inflation that is described by the Lagrangian, where Recall thatξ , ξ 1 in the parameters in Eq. (2.11). Then it is clear that the additional term proportional to ∆M 2 is the same as in Eq. (3.11). Note that s min is negligible in Ω(φ, s min ). Then, the canonically-normalized inflaton field is given by Eqs. (3.12)-(3.14). Consequently, V inf is given by Therefore, if Eqs. (3.17) and (3.18) are satisfied, then the dynamics in the subcritical regime reduces to one in Ref. [13] To summarize the present and previous subsections, the inflaton-waterfall field dynamics is unchanged when for i = 1-3 are satisfied.

Stability of inflationary trajectory
It was pointed out in Ref. [19] thatL i H u may become tachyonic in sneutrino inflation. In order to find out the stability condition, let us derive the mass matrix inL i and H u basis. From V tot , it is obtained by On the other hand, the kinetic terms ofL i and H u are given by Therefore, using canonically-normalized fields, the mass terms are rewritten as where we have defined (y ν y † ν ) 1/2 33L 3 ≡ y ν3iLi in the second line following Ref. [19]. Then, the stability condition is given by Using Eqs. (3.12) and (3.14), it turns out that This upper bound is weaker than (3.23) in most of the parameter space, which will be seen later.

Neutrino mass
In this section, we derive the mass matrices for the heavy and light neutrinos. Around the global minimum, Ω 1 since ξ 1. Consequently, all the fields are canonical.
Thus, the mass terms are derived similarly in global SUSY model.

Mass matrix
The superpotential (2.2) gives Majorana masses for the light neutrinos. To see how the masses are generated, we write down the mass terms for fermionic part of N c i , ν Li andS − , M andm ν are 4 × 4 and 4 × 3 matrices, respectively, and given bỹ Here m ν ij = y ν ij H 0 u with H 0 u being the VEV of the up-type neutral Higgs. Then mass matrix M ν for the light neutrinos are obtained by the seesaw mechanism [17], An important consequence of the mass matrix is that the one of three light neutrinos is massless. This is because the rank of M ν is two. Using this mass matrix, it is possible to constrain the parameters by the observed neutrino masses.
In the later discussion we assume Here, recall that there is a freedom to choose a basis for N c 1 and N c 2 . Then, M 12 can be rotated away. As a result, M ν is given in the following simple expression, This is independent of λ 1,2 , M i3 , m φ and y ν3i (i = 1-3). Therefore, they are not constrained by the neutrino oscillation data. This fact is important in the estimation of the reheating temperature, which we will see later.
Before further discussing the light neutrino mass matrix, let us note that the mass matrixM corresponds to the mass matrix in the superpotential around the global minimum,  Table 1: Neutrino mass data taken from Ref. [20], adopting data with the atmospheric neutrino by Super-Kamiokande. ∆m 2 ij ≡ m 2 i − m 2 j , and ∆m 2 3l = ∆m 2 31 > 0 for the normal hierarchy (NH) case and ∆m 2 3l = ∆m 2 32 < 0 for the inverted hierarchy (IH) case.
Recall that we have the requirement (3.23) for successful inflation. Therefore,M should be almost block-diagonal as where M i > 0. Here we have left M 3 for later discussion. In the following analysis we use Eq.(4.10) forM .M is further diagonalized by a unitary matrix UM as, Here we have omitted O(M 3 /m φ ) corrections since they are irrelevant in the later analysis.

Parametrization of neutrino Yukawa couplings
Now let us discuss M ν . It can be diagonalized by a unitary matrix U ν as Ref. [20], which are listed in Table 1.
Before discussing the parametrization of the neutrino Yukawa couplings, it is instructive to count the number of parameters. The situation is the same as one discussed Refs. [19,21] since the mass matrix of the light neutrinos (4.8) is similar.
Since one neutrino is massless, there are 7 parameters in low energy, i.e., 2 neutrino masses + 3 real mixing angles + 2 phases. On the other hand, M ν includes y νki and M k where k = 1, 2 and i = 1, 2, 3, which means 12 real parameters (neutrino Yukawa couplings) + 2 real parameters (right-handed neutrino masses). However, 3 phases can be absorbed by lepton doublets and 2 real parameters are unphysical since M ν is unchanged by the rescalings y νki → γ k y νki and M k → γ 2 k M k with γ k being real constants. Therefore, we have 9 independent parameters in M ν to determine 7 parameters in the light neutrino sector. As it will be seen below, however, the parametrization of the Yukawa couplings is different, especially for y ν3i that are important parameters for the estimation of the reheating temperature.
, respectively. It is found that R is more restrictive than Eq. (4.15). Namely, Using the relations, the neutrino Yukawa couplings can be expressed in terms of R.
For later discussion, it is useful to give following quantities: It is seen that (y ν y † ν ) 11 and (y ν y † ν ) 22 are constrained by the neutrino oscillation data, meanwhile (y ν y † ν ) 33 is basically a free parameter since R 3j is not constrained. This is consistent with the fact that M ν is independent of y ν3i .
The discussion is quite similar in the IH case. The definition of R is the same form as in Eq. (4.14), but satisfies we get r T r = rr T = 1 , (4.25) 27) and the neutrino Yukawa couplings are given by, (4.31)

Post inflationary regime
After the end of inflation, the inflaton oscillates around the global minimum and decays eventually. Due to the decay the universe is reheated and thermal plasma is created. In this section, we estimate the reheating temperature and discuss how the lepton number asymmetry is generated. As in the previous section, we take Ω 1.
After the universe is reheated, gravitinos are produced in various ways. We discuss the gravitino problem at the end of this section.

Reheating
The reheating temperature T R due to the inflaton decay is estimated by, where g * (T ) is the effective degree of freedom of radiation fields at temperature T and Γ φ is the decay rate of the inflaton. This expression is valid when the neutrino Yukawa couplings that are responsible for the decay is sufficiently small to satisfy T R m φ [24,25], which is the situation we focus on. #6 The inflaton decays as φ → LH u ,LH u ,LH u ,L * H * u . #7 Here flavor indices and SU(2) doublet components are summed implicitly. Then the decay rates for the modes are given by , the total decay rate is given by Then the reheating temperature is estimated as #6 Of course, it is possible to consider a higher reheating temperature than the inflaton mass. Such a case is discussed in Ref. [19]. We will comment on the impact of such high reheating temperature on leptogenesis in the next subsection. #7 In general, the inflaton decays to gravitino pair or gravitino and right-handed neutrino. We will discuss those processes in Sec. 5.3.
Recall that (y ν y † ν ) 33 is not constrained by the neutrino observations. As a consequence, it is possible to consider a wide range of values for the reheating temperature, which is suitable for leptogenesis.
To end this subsection, we derive the number of e-folds before the end of inflation.
In this model, the inflaton oscillates after the end of inflation and eventually decays to reheat the universe. Therefore, it is given by

Leptogenesis
Now we discuss the lepton number asymmetry. The lepton number is generated via leptogenesis [18] (see, for example, Refs. [26,27] for review). In the following numerical study, we discuss following representative cases: However, the effect of coherent oscillation ofÑ i is negligible since the energy density ratio ofÑ i to radiation at the decay is estimated as less than ξ 2 /18M 4 pl ∼ 10 −9 . effective neutrino mass [30] and equilibrium neutrino mass [31], where v 246.7 GeV. Ifm 1 /m * is larger than unity, then it is the strong washout regime and the lepton number generated at the reheating is washed out.m 1 is estimated by using Eqs. (4.20) and (4.28), .  [28,29], which is always possible as confirmed in the previous subsection. Then the resultant baryon number becomes independent of T R . In our study, we adopt the analytic expressions in Ref. [29] for the calculation of the baryon number. Note that although the results there are given in non-supersymmetric model, the results in supersymmetric model do not change much both quantitatively and qualitatively [27,32,33]. In our study we adopt the discussion given in Ref. [27].
Then the baryon number is determined by where n B and n γ are number densities of baryon and photon at present, respectively, a sph = 28/79, f = 2387/86, and a factor of √ 2 counts the supersymmetric effect.
The efficiency factor κ f is given by [29] κ f = (2 ± 1) × 10 −2 0.01 eṼ m 1 Finally, referring Ref. [34], the asymmetric parameter 1 in our model is given by . Therefore, parametrizing m eff as m eff = m max eff sin δ, the asymmetric parameter is given by ≥ η obs B where sin δ = 1 and η obs B is given by [35] η obs B = (6.12 ± 0.03) × 10 −10 . (5.19) In Fig. 1, allowed regions are depicted for the NH and IH cases. Here we consider so-called high-scale SUSY and take H 0 u = v/2 to get 125 GeV Higgs mass [36,37]. In the plot upper bound on M 1 is given by (5.7), i.e., M 1 < m φ = 10 13 GeV, and the lower bound onm 1 is from Eq. (5.12). #10 The theoretical uncertainties in Eq. (5.14) are taken into account. It is found that the present baryon number can be explained in a wide range of parameter space for the NH case. For the IH case, on the other hand, it seems that the parameter space for a successful leptogenesis is relatively limited. The lowest value required for M 1 turns out to be The lower limit is near the upper bound in the IH case. Here recall that the upper bound on M 1 is just a theoretical one. When M 1 ∼ m φ , T R should be comparable to m φ , which is possible as discussed in Refs. [19,24,25]. In such a case, sneutrino inflation and leptogenesis can be another source for lepton asymmetry, which will be discussed below in detail. Therefore, the upper bound merely indicates the parameter space for simple thermal leptogenesis to work.
Let us move on to case (II). Since they are much heavier than the inflaton, N 1,2 andÑ 1,2 are never thermalized after the reheating. For N 3 andÑ 3 , on the other hand, it depends on the effective neutrino mass that is defined bỹ Then, from Eq. (5.5), one obtains Here m * is defined similarly to Eq. (5.10) but replacing g * (M 1 ) by g * (m φ ), and we have taken g * (T R ) g * (m φ ). As explained in Sec. 5.1, the expression Eq. (5.5) is valid for T R /m φ 1 that is satisfied form 3 < m * . Such a case corresponds to #10 Strictly speaking, the equality should be excluded since baryon number is zero.

NH, IH
Let us supposem 3 m * , i.e., the weak washout regime and T R /m φ 1. Then baryon number is given by where a MSSM sph = 8/23 and d = (s/n γ ) 0 = 43π 4 /495ζ(3) is the present value of entropy density to and photon density ratio. φ is obtained by an explicit calculation as where . (5.25) In the second step, we have used Eqs. (4.21), (4.23), (4.29), and (4.31). It should be noted that φ is independent of the inflaton mass, but it depends on M 3 . Even though R 3j are not constrained, it has been found that m eff is bounded from above.
The maximum value turns out to be (5.28) Since η B is independent of m φ , the requirement η max B ≥ η obs B gives a lower bound on M 3 , which is plotted in Fig. 2. Here H 0 u = v/2 is taken as in Fig. 1. Upper bound M 3 < 2×10 11 GeV is from Eq.(3.23). Another upper bound on M 3 from the stability of the inflationary trajectory, Eq. (3.28), is also shown. We quit plotting for regioñ m 3 > 10 −5 eV becausem 3 m * is no longer valid. In the plot, contours of T R are depicted. It is found that the leptogenesis is successful in a wide parameter space for both the NH and IH cases. Lower bound on M 3 behaves similarly to region C in In the case wherem 3 gets much larger than m * , the situation reduces to case (I). Namely, the reheating temperature is so high that bothÑ 3 and N 3 are thermalized and thermal leptogenesis takes place. Resultant allowed region is the same as the NH case of Fig. 1, by replacing M 1 andm 1 by M 3 andm 3 , respectively, but there is no lower bound onm 3 meanwhile there is the upper bound on M 3 . In the intermediate case,m 3 ∼ m * , on the other hand, the Boltzmann equations should be solved numerically to get the lepton number, which is already done in Ref. [42].
The result corresponds to region B in Fig. 1 of the reference. Strictly speaking, the effective dissipation rate should be used instead of the decay rate of the inflaton [25] in the Boltzmann equations. As shown in the reference, the reheating process is so efficient when the dissipation rate is taken into account that the reheating temperature can exceed the mass of the inflaton mass and consequently N 3 andÑ 3 are easily thermalized. Once they are thermalized, the thermal leptogenesis takes place, where the resultant baryon number becomes independent of the reheating temperature.
Eventually the situation reduces to the case (I). Such qualitative behavior can be confirmed by numerical study, which is left for the future work.
Crucial difference from sneutrino leptogenesis [38][39][40][41][42] is that although M 3 and m 3 , i.e., (y ν y † ν ) 33 , are important parameters to determine baryon number, they are sequestered from other physical quantities, such as the heavy right-handed (s)neutrino masses or the light neutrino mass matrix. Therefore, there is no consequence in other low energy experiments. This is a feature of case (II).

Gravitino problem
In the framework of supergravity, a fair amount of gravitino ψ µ can be produced in various ways in the thermal history of the universe. Since the interactions of gravitino with the MSSM particles are Planck-suppressed, gravitino is long-lived and its decay can spoil the successful big-bang nucleosynthesis if it is unstable. Although this problem can be avoided when gravitino is enough heavy to have the lifetime much shorter than 1 sec, gravitino decay produces the lightest superparticle (LSP).
Then the LSP produced by the decay may overclose the universe if the R-parity is conserved.
In general, process (i) includes gravitino pair production. The decay width of the mode, however, depends on the inflaton VEV [57][58][59][60][61][62]. In our case, therefore, this process can be ignored since the inflaton does not have a VEV. On the other hand, the inflaton can decay to gravitino and right-handed neutrino. The decay width is given by where Here m f and m 3/2 are masses of N 3 and ψ µ , respectively. The mass difference between φ and N 3 is expected to be given by the soft SUSY breaking mass scale for scalar superpartners, |m φ −m f | ∼m.
Gravitino abundance via process (ii) is most effective at high temperature, thus it is proportional to T R , meanwhile in process (iii) gravitino is dominantly produced when the temperature is around the mass of decaying particle. Adopting the expression given in Ref. [63], the abundances via processes (ii) and (iii) are given by (5.34) Here the contribution of the longitudinal mode of gravitino is suppressed in Ω TH 3/2 by considering gluino is lighter than gravitino. In Ω FI 3/2 , we have assumed that all scalar leptons and quarks in the MSSM (whose mass scale ism) are heavier than gravitino and that they are thermalized. And as in the discussion of the inflaton decay,m = km 3/2 has been taken. #11 Then the relic abundance of the LSP due to gravitino decay is estimated as where m LSP is the LSP mass and Ω 3/2 = Ω inf 3/2 + Ω TH 3/2 + Ω FI 3/2 is the total gravitino abundance. Ω non-th LSP h 2 should not exceed the observed dark matter abundance Ω DM h 2 0.12 [35], which gives a constraint on gravitino mass. TeV [64]. m φ = 10 13 GeV, (y ν y † ν ) 33 = 10 −11 , and k = 2 (left), 10 (right) are taken to determine the contributions from processes (i) and (iii). It is seen that in lower gravitino mass region, the dominant contribution to Ω non-th LSP is from process (ii). In order for the contribution not to exceed the dark matter abundance, T R 10 9 GeV #11 We have checked that the contribution fromÑ 1 is negligible even ifÑ 1 is thermalized, i.e., in case (I).
is required, which is well-known result. This gives a stringent constraint on the parameter space for successful leptogenesis shown in Figs. 1 and 2 if gravitino is not heavy enough. Namely,m 1 ∼ 10 −2 eV is the allowed region in case (I) meanwhile 10 −13 eV m 3 10 −11 eV is allowed in case (II). On the other hand, the contributions from processes (i) and (iii) depend on the parameters, especially k =m/m 3/2 (and m 3/2 ). In order for Ω non-th LSP not to exceed the dark matter abundance, the upper bound on gravitino mass is obtained depending on the mass spectrum of squarks and sleptons, e.g., m 3/2 10 8 (10 6 ) GeV form ∼ m 3/2 (10m 3/2 ). Such gravitino mass is preferred in minimal or mini split supersymmetry [65,66], pure gravity mediation [67,68], and spread supersymmetry [63,69].
On the other hand, there is also an allowed region in higher gravitino mass region.
This is because gravitino decays before thermal freeze-out of the LSP in that region.
Another option is the R-parity violation. Under the R-parity violation, the LSP decays to the standard-model particles. Then, the LSP does not contribute to the matter abundance of the universe so that there is no constraint on m 3/2 .

Conclusions
Superconformal subcritical hybrid inflation is one of attractive inflation models that are consistent with the observed cosmological parameters by the Planck satellite. In this paper we have studied the cosmology of an extended version of the model. In the model three right-handed neutrinos are introduced. The superpotential consists of one in the supersymmetric seesaw model and the interaction terms of the righthanded neutrinos with the additional matter fields, one of which plays the role of the waterfall field. In the Kähler potential, on the other hand, it is possible for the sneutrinos to have shift symmetry by introducing explicit superconformal breaking terms of O(1). Due to the shift symmetry, one of the sneutrinos becomes the inflaton field similarly in superconformal subcritical hybrid inflation. Although the mass terms of the sneutrinos can affect the trajectory of the inflaton, it has turned out that the effect is restrictive and viable inflation is realized. After inflation, the inflaton field decays to Higgses and sleptons or Higgsinos and leptons to reheat the universe.
Light neutrino masses are given by the seesaw mechanism. However, the mass matrix is different from the conventional one. It turns out that one of the neutrinos is massless. Assuming that suppressed couplings of the other right-handed neutrinos to the waterfall field, it has been found that the neutrino Yukawa couplings that couples the inflaton to the MSSM sector are not constrained by the neutrino oscillation data.
Consequently, the reheating temperature is a free parameter, which is suitable for leptogenesis.
We have considered two representative cases; (I) the other right-handed (s)neutrinos are lighter than the inflaton; (II) the other right-handed (s)neutrinos are heavier than the inflaton. In case (I), thermal leptogenesis is possible if the reheating temperature is larger than ∼ 10 9 GeV. It has been found leptogenesis is successful in a wide range of parameter space in the normal hierarchy case while the parameter space for leptogenesis is relatively limited in the inverted hierarchy case. In case (II), on the other hand, sneutrino leptogenesis takes place if the reheating temperature is larger than ∼ 10 8 GeV. It has turned out that in both the normal and inverted hierarchy cases successful leptogenesis is realized in wide range of parameter space.