A to Z of Flavour with Pati-Salam

We propose an elegant theory of flavour based on A4 × Z5 family symmetry with Pati-Salam unification which provides an excellent description of quark and lepton masses, mixing and CP violation. The A4 symmetry unifies the left-handed families and its vacuum alignment determines the columns of Yukawa matrices. The Z5 symmetry distinguishes the right-handed families and its breaking controls CP violation in both the quark and lepton sectors. The Pati-Salam symmetry relates the quark and lepton Yukawa matrices, with Yu = Yν and Yd ~ Ye. Using the see-saw mechanism with very hierarchical right-handed neutrinos and CSD4 vacuum alignment, the model predicts the entire PMNS mixing matrix and gives a Cabibbo angle θC ≈ 1/4. In particular, for a discrete choice of Z5 phases, it predicts maximal atmospheric mixing, θ23l = 45° ± 0.5° and leptonic CP violating phase δl = 260° ± 5°. The reactor angle prediction is θ13l = 9° ± 0.5°, while the solar angle is 34° ≳ θ12l ≳ 31°, for a lightest neutrino mass in the range 0 ≲ m1 ≲ 0.5 meV, corresponding to a normal neutrino mass hierarchy and a very small rate for neutrinoless double beta decay.

The problem of understanding the quark and lepton masses, mixing angles and CP violating phases remains one of the most fascinating puzzles in particle physics. Following the discovery of a Standard Model (SM)-like Higgs boson at the LHC [1,2], it seems highly plausible that quark masses, mixing angles and CP phase originate from Yukawa couplings to a Higgs field. However the SM offers absolutely no insight into the origin or nature of these Yukawa couplings, motivating approaches beyond the SM [3,4].
In the quark sector, the Yukawa couplings are organised into 3 × 3 quark Yukawa matrices Y u and Y d , which must be responsible for the quark mass hierarchies and small quark mixing angles, together with the CP phase. Similarly, the charged lepton Yukawa matrix Y e must lead to a mass hierarchy similar to that of the down-type quarks. The origin of small quark mixing and CP violation and the strong mass hierarchies of the quarks and charged leptons, with an especially strong hierarchy in the up-type quark sector, is simply unexplained within the SM. The nine charged fermion masses, three quark mixing angles, including the largest Cabibbo angle θ C ≈ 13 • , and the CP phase are all determined from experiment. From a more fundamental point of view, the three Yukawa matrices Y u , Y d and Y e contain 54 undetermined Yukawa couplings leading to 13 physical observables with a calculable scale dependence [5,6].
Following the discovery of atmospheric neutrino oscillations by Super-Kamiokande in 1998 and solar neutrino oscillations by SNO in 2002 [7,8], Daya Bay has recently accurately measured a non-zero reactor angle [9] which rules out tri-bimaximal (TB) [10] mixing. However, recent global fits [11][12][13] 1 are consistent with tri-bimaximal-Cabibbo (TBC) [14] mixing, based on the TB atmospheric angle θ l 23 ≈ 45 • , the TB solar angle θ l 12 ≈ 35 • and a reactor angle θ l 13 ≈ θ C / √ 2 ≈ 9 • . The extra parameters of the lepton sector include three neutrino masses, three lepton mixing angles and up to three CP phases, although no leptonic CP violation has yet been observed and the lightest neutrino mass has not been measured. The 9 additional neutrino observables, together with the 13 physical observables in the charged fermion sector, requires 22 unexplained parameters in the flavour sector of the SM. This provides a powerful motivation to search for theories of flavour (TOF) based on discrete family symmetry which contain fewer parameters [15,16].
The origin of neutrino mass is presently unknown and certainly requires some extension of the SM, even if only by the addition of right-handed (RH) neutrinos which are singlets under the SM gauge group. Since such RH neutrinos may have large Majorana masses, in excess of the electroweak breaking scale, such a minimal extension naturally leads to the idea of a see-saw mechanism [17][18][19][20], resulting from a neutrino Yukawa matrix Y ν , together with a complex symmetric Majorana matrix M R of heavy right-handed neutrinos, leading to a light effective Majorana neutrino mass matrix where v is the Higgs vacuum expectation value (VEV). However the see-saw mechanism does not explain large lepton mixing angles, with the smallest being the reactor angle θ l 13 ≈ 9 • , nor does it address any of the flavour puzzles in the charged fermion sector.

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The origin of large lepton mixing may be accounted for within the see-saw mechanism with the aid of sequential dominance (SD) [21][22][23]. For example, with an approximately diagonal M R , the lightest right-handed neutrino ν atm R may give the dominant contribution to the atmospheric neutrino mass m 3 , the second lightest right-handed neutrino ν sol R to the solar neutrino mass m 2 and the heaviest, almost decoupled, right-handed neutrino ν dec R may be responsible for the lightest neutrino mass m 1 . The immediate prediction of SD is a normal neutrino mass hierarchy, m 3 > m 2 m 1 , which will be tested in the near future. However SD also provides a simple way to account for maximal atmospheric mixing and tri-maximal solar mixing by adding constraints to the first two columns of the neutrino Yukawa matrix Y ν , with the third column assumed to be approximately decoupled from the see-saw mechanism. In the diagonal Y e basis, if the dominant first column of Y ν is proportional to (0, 1, 1) T then this implies a maximal atmospheric angle tan θ l 23 ≈ 1 [24]. This could be achieved with a non-Abelian family symmetry such as A 4 [25], if the first column is generated by a triplet flavon field with a vacuum alignment proportional to (0, 1, 1) T . In such models, it has been shown that the vacuum alignment completely breaks the A 4 symmetry, and such models are therefore referred to as "indirect" models [26]. Such "indirect" models are highly predictive and do not require such large discrete groups as the "direct" models where the Klein symmetry of the neutrino mass matrix is identified as a subgroup of the family symmetry [27][28][29].
"Indirect" models of leptons have been constructed based on A 4 using both CSD3 [33] and CSD4 [34] since these are the most promising from the point of view of the reactor angle. From the point of view of extending to the quark sector, CSD4 seems to be the most promising since in unified models with Y u = Y ν , the second column is proportional to (1,4,2) T . This simultaneously provides a prediction for both lepton mixing and the Cabibbo angle [35]. The model in [35] was based on A 4 family symmetry with Z 4 3 × Z 5 5 and quark-lepton unification via the Pati-Salam (PS) [36] gauge subgroup SU(4) P S × SU(2) L × U(1) R and the CSD4 alignment (1,4,2). The small quark mixing angles arose from higher order (HO) corrections appearing in Y u and Y ν , providing a theoretical error or noise which blurred the PMNS predictions. Here we discuss an alternative A 4 model which has three advantages over the previous model. Firstly it is more unified, being based on the full PS gauge group SU(4) P S × SU(2) L × SU(2) R [36]. Secondly it introduces only a single Z 5 symmetry,

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replacing the rather cumbersome Z 4 3 × Z 5 5 symmetry. Thirdly, it accounts for small quark mixing angles already at the leading order (LO), with all Higher Order (HO) corrections being rather small, leading to more precise predictions for the PMNS parameters, such as maximal atmospheric mixing. Unlike other A 4 ×PS models (see e.g. [37]), the present model does not involve any Abelian U(1) family symmetry. Instead the left-handed PS fermions are unified into a triplet of A 4 while the right-handed PS fermions are distinguished by Z 5 , as in figure 1.
In the present paper, then, we propose a rather elegant TOF based on the PS gauge group combined with a discrete A 4 × Z 5 family symmetry. PS unification relates quark and lepton Yukawa matrices and in particular predicts equal up-type quark and neutrino Yukawa matrices Y u = Y ν , leading to Dirac neutrino masses being equal to up, charm and top masses. The see-saw mechanism then implies very hierarchical right-handed neutrinos. The A 4 family symmetry determines the structure of Yukawa matrices via the CSD4 vacuum alignment [33,34], with the three columns of Y u = Y ν being proportional to (0, 1, 1) T , (1, 4, 2) T and (0, 0, 1) T , respectively, where each column has an overall phase determined by Z 5 breaking, which controls CP violation in both the quark and lepton sectors. The down-type quark and charged lepton Yukawa matrices are both approximately equal and diagonal Y d ∼ Y e , but contain small off-diagonal elements responsible for the small quark mixing angles θ q 13 and θ q 23 . The model predicts the Cabibbo angle θ C ≈ 1/4, up to such small angle corrections. The main limitation of the model is that it describes the fermion masses and small quark mixing angles by 16 free parameters. The main success of the model is that, since there are 6 fewer parameters than the 22 flavour observables, it predicts the entire PMNS lepton mixing matrix including the three lepton mixing angles and the three leptonic CP phases. The model may be tested quite soon via its prediction of maximal atmospheric mixing with a normal neutrino mass hierarchy.
The layout of the remainder of the paper is as follows. In section 2, we give a brief overview of the essential features of the model. In section 3, we present the full model and show how the messenger sector can lead to effective operators, then discuss how these operators lead to Yukawa and Majorana mass matrices. In section 4, we derive the quark masses and mixing, including CP violation, arising from the quark Yukawa matrices, first analytically, then numerically. In section 5, we implement the see-saw mechanism, then consider the resulting neutrino masses and lepton mixing, with modified Georgi-Jarlskog relations, before performing a full numerical analysis of neutrino masses and lepton mixing, including CP violation. In section 6, we consider higher order corrections to the results and show that they are small due to the particular messenger sector. Finally section 7 concludes the paper. A 4 group theory is discussed in appendix A and the origin of the light Higgs doublets H u and H d in appendix B.
2 Overview of the model

Symmetries of the model
The model is based on the Pati-Salam gauge group [36], with A 4 × Z 5 family symmetry, The quarks and leptons are unified in the PS representations as follows,

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so as to maintain supersymmetric gauge coupling unification. Since the PS Higgs fields do not carry any A 4 × Z 5 charges, the potential responsible for supersymmetric PS breaking considered in [41] is assumed to be responsible for PS breaking here.

CP violation
Our starting point is to assume that the high energy theory, above the PS breaking scale, conserves CP [42,43]. We shall further assume that CP is spontaneously broken by the complex VEVs of scalar fields which spontaneously break A 4 and Z 5 . The scalars include A 4 triplets φ ∼ 3, A 4 singlets ξ ∼ 1, and other one dimensional A 4 representations such as Σ u ∼ 1 and Σ d ∼ 1 . In addition all of the above fields carry Z 5 charges denoted as the powers α n , where α = e 2πi/5 and n is an integer. For example ξ ∼ α 4 under Z 5 . The group theory of A 4 is reviewed in appendix A, while Z 5 corresponds to α 5 = 1. Under a CP transformation, the A 4 singlet fields transform into their complex conjugates [44,45], where the complex conjugate fields transform in the complex conjugate representations under On the other hand, in the Ma-Rajarsakaran [25] basis of appendix A, for A 4 triplets φ ∼ (φ 1 , φ 2 , φ 3 ), a consistent definition of CP symmetry requires the second and third triplet components to swap under CP [44,45], CP violation has also been considered in a variety of other discrete groups [46][47][48][49][50][51]. With the above definition of CP, all coupling constants g and explicit masses m are real due to CP conservation and the only source of phases can be the VEVs of fields which break A 4 × Z 5 . In the model of interest, all the physically interesting CP phases will arise from Z 5 breaking as in [42,43]. For example, consider the A 4 singlet field ξ which carries a Z 5 charge α 4 . The VEV of this field arises from Z 5 invariant quintic terms in the superpotential [42,43], where, as in [42,43], P denotes a singlet and the coupling g and mass m are real due to CP conservation. The F-term condition from eq. (2.8) is, This is satisfied, for example, by ξ = |(Λ 3 m 2 ) 1/5 |e −4iπ/5 , where we arbitrarily select the phase to be −4π/5 from amongst a discrete set of five possible choices, which are not distinguished by the F-term condition, as in [34]. We emphasise that CP breaking is controlled by the Abelian Z 5 symmetry rather than the non-Abelian A 4 symmetry.

Vacuum alignment
Let us now consider the A 4 triplet fields φ which also carry Z 5 charges. In the full model there are four such triplet fields, or "flavons", denoted as φ u The idea is that φ u i are responsible for up-type quark flavour, while φ d i are responsible for down-type quark flavour. These VEVs are driven by the superpotential terms, where P ij are linear combinations of singlets as in [34]. The coupling constants g ij , mass parameters M ij and cut-off scale Λ are enforced to be real by CP while the fields φ u i and φ d i will develop VEVs with quantised phases. If we assume that φ u i both have the same phase, e imπ/5 , then eq. (2.10) implies that φ d i should have phases e inπ/5 such that where n, m are positive or negative integers. The structure of the Yukawa matrices depends on the so-called CSD4 vacuum alignments of these flavons which were first derived in [34], and we assume a similar set of alignments here, although here the overall phases are quantised due to Z 5 , and We note here that the vacuum alignments in eq. (2.13) and the first alignment in eq. (2.12) are fairly "standard" alignments that are encountered in tri-bimaximal mixing models, while the second alignment in eq. (2.12) is obtained using orthogonality arguments, as discussed in [34], to which we refer the interested reader for more details.

Two light Higgs doublets
The model will involve Higgs bi-doublets of two kinds, h u which lead to up-type quark and neutrino Yukawa couplings and h d which lead to down-type quark and charged lepton Yukawa couplings. In addition a Higgs bidoublet h 3 , which is also an A 4 triplet, is used to give the third family Yukawa couplings. After the PS and A 4 breaking, most of these Higgs bi-doublets will get high scale masses and will not appear in the low energy spectrum. In fact only two light Higgs doublets will survive down to the TeV scale, namely H u and H d . The precise mechanism responsible for this is quite intricate and is discussed in appendix B. Analogous Higgs mixing mechanisms are implicitly assumed in many models, but are rarely discussed explicitly (however for an example within SO(10) see [52]).

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The basic idea is that the light Higgs doublet H u with hypercharge Y = +1/2, which couples to up-type quarks and neutrinos, is a linear combination of components of the Higgs bi-doublets of the kind h u and h 3 , while the light Higgs doublet H d with hypercharge Y = −1/2, which couples to down-type quarks and charged leptons, is a linear combination of components of Higgs bi-doublets of the kind h d and h 3 , (2.14)

Yukawa operators
The renormalisable Yukawa operators, which respect PS and A 4 symmetries, have the following form, leading to the third family Yukawa couplings shown, using eqs. (2.2), (2.14), where we have used eqs. (2.2), (2.14). The non-renormalisable operators, which respect PS and A 4 symmetries, have the following form, where i = 1 gives the first column of each Yukawa matrix, while i = 2 gives the second column and we have used eqs. (2.2), (2.14). Thus the third family masses are naturally larger since they correspond to renormalisable operators, while the hierarchy between first and second families arises from a hierarchy of flavon VEVs.

Yukawa matrices
Inserting the vacuum alignments in eqs. (2.18) The PS unification predicts the equality of Yukawa matrices Y u = Y ν and Y d ∼ Y e , while the A 4 vacuum alignment predicts the structure of each Yukawa matrix, essentially identifying the first two columns with the vacuum alignments in eqs. (2.12) and (2.13). With a diagonal right-handed Majorana mass matrix, Y ν leads to a successful prediction of the PMNS mixing parameters [34]. Also the Cabibbo angle is given by θ C ≈ 1/4 [35]. Thus eq. (2.18) is a good starting point for a theory of quark and lepton masses and mixing, although the other quark mixing angles and the quark CP phase are approximately zero. However above discussion ignores the effect of Clebsch factors which will alter the relationship between elements of Y d and Y e , which also include off-diagonal elements responsible for small quark mixing angles in the full model. Table 1. The basic Higgs, matter, flavon and messenger content of the model, where α = e 2πi/5 under Z 5 . R is a supersymmetric R-symmetry.

The model
The most important fields appearing in the model are defined in table 1. In addition to the fields introduced in the previous overview, the full model involves Higgs bi-doublets h 15 in the adjoint of SU(4) C , as well as messenger fields X with masses given by the VEV of dynamical fields Σ. The effective non-renormalisable Yukawa operators therefore arise from a renormalisable high energy theory, where heavy messengers X with dynamical masses Σ are integrated out, below the energy scale Σ .

Operators from messengers
Although the Yukawa operators in the up sector of the full model turn out to be the same as in eq. (2.16), the Yukawa operators in the down sector of the full model will involve Clebsch factors which will imply that Y d and Y e are not equal. In addition Y d and Y e will involve off-diagonal elements which however are "very small" in the sense that they will give rise to the small quark mixing angles of order V ub and V cb . The Cabibbo angle arises predominantly from the second column of Y u , with the prediction V us ∼ 1/4 being corrected by the very small off-diagonal elements of Y d . The allowed Yukawa operators arise from integrating out heavy fermion fields called "messengers" and will depend on the precise choice of fermion messengers. In table 1 we have allowed messengers of the form X F i for charges α i (i = 1, . . . , 4), with a very restricted set of messengers X F 1 (X F 1 ) and X F 3 (X F 3 ) with charges α and α 3 , in the 1 The assumed messengers X F i have allowed couplings to φF as follows, The messengers X F and X F have allowed couplings to hF c i as follows, The messengers couple to each other and become heavy via the dynamical mass fields Σ which appear in table 1, The leading order operators responsible for the Yukawa couplings involving the first and second families to Higgs fields are obtained by integrating out the heavy messengers, leading to effective operators.
The diagrams in figure 2 yield the following operators which will be responsible for the up-type quark and neutrino Yukawa couplings, The above operators are similar to those in eq. (2.16) and will yield a Yukawa matrix Y u = Y ν as in eq. (2.18). The diagrams in figure 3 yield the operators which will be responsible for the diagonal down-type quark and charged lepton Yukawa couplings, These operators are similar to those in eq. (2.17) and will yield Yukawa matrices similar to those in eq. (2.18) but with Y d = Y e due to the Clebsch-Gordan coefficients from the Higgs in the 15 dimensional representation of SU(4) C . In addition, the above messenger sector generates further effective operators which give rise to off-diagonal down-type quark and charged lepton Yukawa couplings,  The operators responsible for the heavy Majorana neutrino masses are given by, corresponding to the diagrams in figure 4. These operators are mediated by the singlet messengers X ξ i and involve the explicit messenger mass scale Λ which may take values higher than the A 4 × Z 5 and Pati-Salam breaking scales. The first three of these operators are controlled by the Majoron fields ξ i in table 1, which carries a non-trivial phase due to the Z 5 symmetry, as discussed later. Note that the dynamical mass Σ fields do not enter the Majorana sector since they transform under A 4 as 1 , 1 and hence do not couple to pairs of X ξ i . Also note that the Majoron ξ fields which transform under A 4 × Z 5 as ξ ∼ (1, α 4 ) do not enter the charged fermion sector since they do not couple X F i to the messengers X F and X F which transform under A 4 as 1 and 1 .

Yukawa and Majorana mass matrices
According to the mechanism discussed in appendix B, the four Higgs multiplets in the fourth block of table 1,

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With the vacuum alignments in eq. (2.12), the operators in eq. (3.4) then result in non-diagonal and equal up-type quark and neutrino Yukawa matrices, where, Note that since Y u = Y ν , the up-type quark masses are equal to the Dirac neutrino masses, From eq. (3.9) the up-type quark masses are given to excellent approximation by, The Yukawa coupling eigenvalues for up-type quarks are given by, where we have inserted some typical up-type quark Yukawa couplings, hence, where the ratio of up to charm masses is accounted for by the 2% ratio of flavon VEVs. Similarly, with the vacuum alignments in eqs. (2.12), (2.13), the operators in eqs. (3.5), (3.6) then result in down-type quark and charged lepton Yukawa matrices related by Clebsch factors, where the diagonal Yukawa couplings for down-type quarks are given by, where u,d were defined in eq. (3.8) and for low tan β we have inserted some typical downtype quark Yukawa couplings, assuming that the mixing angles are small. The off-diagonal entries to the down-type quark and charged lepton Yukawa matrices are given by, where, From eq. (3.15) the diagonal down-type quark and charged lepton Yukawa couplings are related by, These are the well-known Georgi-Jarlskog (GJ) relations [53], although the factor of 1/3 which appears in the first relation above arises from a new mechanism, namely due to non-singlet fields which appear in the denominator of effective operators as discussed in detail in [54]. The viablity of the GJ relations for mass eigenstates is discussed in [5,6]. However here there are small off-diagonal entries in the Yukawa matrices which will provide corrections to the mass eigenstates, as well as other corrections to the GJ relations, as discussed later. Finally, from eq. (3.7), we find the heavy Majorana mass matrix, The heavy Majorana neutrino masses from eq. (3.7) are in the ratios, There is a competing correction to M 1 coming from the off-diagonal element, namely M 2 13 /M 3 ∼ξ 2 with the same phase, which may be absorbed into the definition of the lightest right-handed neutrino mass. Since we need to have a strong hierarchy of righthanded neutrino masses we shall require (see later), which may be achieved for example by,ξ Typically the heaviest right-handed neutrino mass is given by, For example, the effect of Majorons on right-handed neutrino annihilations, leading to possibly significantly enhanced efficiency factors, was recently discussed in [55].

Convention
We shall use the convention for the quark Yukawa matrices, which are diagonalised by, The CKM matrix is then given by, In the PDG parameterization [56], in the standard notation, U CKM = R q 23 U q 13 R q 12 in terms of s q ij = sin(θ q ij ) and c q ij = cos(θ q ij ) and the CP violating phase δ q .

Analytic estimates for quark mixing
In the above convention, the quark Yukawa matrices differ from those given in eqs. (3.9), (3.15) by a complex conjugation, 2 where the parameters defined in eqs. (3.13), (3.16), 3.17 are given below, where we have displayed the phases from eqs. (2.12), (2.13) explicitly in the new convention. Cabibbo mixing clearly arises predominantly from the up-type quark Yukawa matrix Y u , which leads to a Cabibbo angle θ C ≈ 1/4 or θ C ≈ 14 • . The other quark mixing angles and CP violating phase arise from the off-diagonal elements of Y d , which also serve to correct the Cabibbo angle to yield eventually θ C ≈ 13 • . 2 The complex conjugation of the Yukawa matrices arises from the fact that the Yukawa matrices given in eqs. (3.9), (3.15) involving the unbarred left-handed and CP conjugated right-handed fields. Note that our LR convention for the quark Yukawa matrices in eq. (4.1) differs by an Hermitian conjugation compared to that used in the Mixing Parameter Tools package [57] due to the RL convention used there.

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Recall that any 3×3 unitary matrix U † can be written in terms of three angles θ ij , three phases δ ij (in all cases i < j) and three phases ρ i in the form [24], and similarly for U 13 , U 23 , where s ij = sin θ ij and c ij = cos θ ij and the angles can be made positive by a suitable choice of the δ ij phases. We use this parameterisation for both U † u L and U † d L , where the phases ρ i can be absorbed into the quark mass eigenstates, leaving where U † u L contains θ u ij and δ u ij , while U † d L contains θ d ij and δ d ij . The CKM matrix before phase removal may be written as On the other hand, U CKM can be also parametrised as in eq. (4.8), The angles θ ij are the standard PDG ones in U CKM , and five of the six phases of U CKM in eq. (4.12) may be removed leaving the standard PDG phase in U CKM identified as [24]: In the present case, given Y u , it is clear that θ u 13 ≈ θ u 23 ≈ 0. Similary, given Y d , we see that θ d 12 ≈ 0. This implies that eq. (4.11) simplifies to: (4.14) Then, by equating the right-hand sides of eqs. (4.12) and (4.14) and expanding to leading order in the small mixing angles, we obtain the following relations: from which we deduce, where, Since |y 0 d /y 0 b | ∼ 0.001, eq. (4.20) implies that, where the last relation uses eq. (3.18).
Concerning the phases, from eq. (4.7) we find, in the convention of eq. (4.9), where, from eq. (2.11), n + m is a multiple of 5. Hence, from eqs. (4.15), (4.16), 4.17, so the physical CP phase is given by the very approximate expression, Clearly CP violation requires n = m, indeed δ q only depends on the difference n − m with a positive value of δ q ∼ 7π 18 in the first quadrant requiring n < m. Since n + m must be a multiple of 5, then the only possibility is n = 2, m = 3 which corresponds to one of the discrete choices of phases in eq. (2.11).

Numerical results for quark mixing
With the phases fixed by the choice of discrete choice of phases n = 2, m = 3, as discussed in the previous subsection, the only free parameters are a, b, c in the up sector, and A, B, C and y 0 d , y 0 s , y 0 b in the down sector matrices, where we have explicitly removed the phases from these parameters, in order to make them real, Note that we have introduced a small correction term in the (1, 3) entry of Y u which will mainly affect θ q 13 . Physically this corresponds to a small admixture of the first component of the Higgs triplet h 3 contributing to the physical light Higgs state H u , as discussed in appendix B. The previous analytic results were for = 0, but we find numerically that the best fit to CKM parameters requires a non-zero value of .
For the following results, we shall fix the parameters which approximately determine the six quark masses at the high scale to be, Although the quark results are insensitive to the sign of y 0 b , the lepton sector results lead to a better fit with the negative sign of y 0 b as discussed later. Using the Mixing Parameter Tools (MPT) package [57], in figure 5 we show the CKM parameters for different choices of A, B as a function of C. θ q 23 is really only sensitive to C only, while θ q 12 is mainly sensitive to B. θ q 13 and δ q are both sensitive A. The effect of the correction is to shift the blue dashed curve to the red solid curve, lowering θ q 13 while leaving θ q 23 almost unchanged, allowing the best fit of the CKM parameters for C = 36.
To take a concrete example, for the red solid at the value C = 36, with the above input parameters A = 9, B = 7 (cf. eq. (4.21)) and = −2.4 × 10 −3 , we find the quark Yukawa eigenvalues at the high scale, These parameters are consistent with those given, for example, in [5,6], after including RG corrections, in particular due to the large top Yukawa coupling. Notice that there are as many input parameters as there are physical observables in the quark sector, so no prediction is claimed. However we emphasise two interesting features, firstly that the Cabibbo angle is understood to arise from Y u leading to θ C ≈ 1/4 or θ C ≈ 14 0 , with a small (one degree) correction mainly controlled by B. Secondly the phases which appear are quantised according to Z 5 , which also controls the leptonic phases as discussed in the following subsection. Indeed, with Y ν = Y u fixed by the quark sector, the entire neutrino sector only depends on three additional right-handed neutrino masses, which determine the three physical neutrino masses, with the entire neutrino mixing matrix then being fully determined, with only very small charged lepton mixing corrections appearing in the PMNS mixing matrix.

Lepton masses and mixing
In this section we discuss the leading order predictions for PMNS mixing which arise from the neutrino Yukawa and Majorana matrices in eq. (3.9) which result in a very simple form of effective neutrino mass matrix, after the see-saw mechanism has been applied.

Convention
The neutrino Yukawa matrix Y ν is defined in a LR convention by 3 where α = e, µ, τ labels the three left-handed neutrinos and i = 1, 2, 3 labels the three right-handed neutrinos. The physical effective neutrino Majorana mass matrix m ν is determined from the columns of Y ν via the see-saw mechanism, where the light Majorana neutrino mass matrix m ν is defined by 4 L ν = − 1 2 m ν ν L ν c L + h.c., while the heavy right-handed Majorana neutrino mass matrix M R is defined by 3 This LR convention for the Yukawa matrix differs by an Hermitian conjugation compared to that used in the Mixing Parameter Tools package [57] due to the RL convention used there. 4 Note that this convention for the light effective Majorana neutrino mass matrix m ν differs by an overall complex conjugation compared to that used in the Mixing Parameter Tools package [57].

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The PMNS matrix is then given by We use a standard parameterization U PMNS = R l 23 U l 13 R l 12 P l in terms of s l ij = sin(θ l ij ), c l ij = cos(θ l ij ), the Dirac CP violating phase δ l and further Majorana phases contained in P l = diag(e i β l 1 2 , e i β l 2 2 , 1). The standard PDG parameterization [56] differs slightly due to the definition of Majorana phases which are by given by P l PDG = diag(1, e i α 21 2 , e i α 31 2 ). Evidently the PDG Majorana phases are related to those in our convention by α 21 = β l 2 −β l 1 and α 31 = −β l 1 , after an overall unphysical phase is absorbed by U e L .

See-saw mechanism
The neutrino Yukawa and Majorana matrices are as in eq. (3.9), with Y ν = Y u in eq. (4.25), where we have ignored the small off-diagonal Majorana mass M 13 which gives a tiny mixing correction of order 10 −5 from eq. (3.24), and dropped the correction which is completely negligible in the lepton sector due to sequential dominance (see below). We have also assumed a phase in the Majoron VEV ξ ∼ e 4iπ/5 in the operators in eq. (3.7) responsible for the right-handed neutrino masses, as discussed below. Using eq. where, are three real parameter combinations which determine the three physical neutrino masses m 1 , m 2 , m 3 , respectively. According to sequential dominance m c will determine the lightest neutrino mass m 1 where we will have m 1 m 2 < m 3 , so that the third term arising from the heaviest right-handed neutrino of mass M 3 is approximately decoupled from the see-saw mechanism. (This is why the correction is completely negligible in the lepton sector.) In order to understand the origin of the relative phases η = 2π/5 which enter the neutrino mass matrix m ν , it is worth recalling that the see-saw operators responsible for the dominant first two terms of the neutrino mass matrix in eq. (5.5) have the form where we have written φ atm = φ u 1 , φ sol = φ u 2 to highlight the fact that the first term gives the dominant contribution to the atmospheric neutrino mass m 3 , while the second JHEP08(2014)130 term controls the solar neutrino mass m 2 . The mild neutrino hierarchy between m 3 and m 2 emerges due to the choice of Majoron VEV ξ in eq. (3.24) which partly cancels the hierarchy in the square of the flavon VEVs in eq. (3.14). The lightest neutrino mass m 1 arises from smaller terms (not shown), leading to a normal neutrino mass hierarchy, where the heaviest atmospheric neutrino mass m 3 is associated with the lightest right-handed neutrino mass M 1 as in light sequential dominance [21][22][23].
Since φ atm and φ sol have the same phase, e −i3π/5 , and ξ has a phase 5 e 4iπ/5 , eq. (5.7) shows that the atmospheric term has a phase (e −i3π/5 ) 2 /(e 4iπ/5 ) 2 = e −14iπ/5 , while the solar term is real. After multiplying m ν by an overall phase e 4iπ/5 , which we are allowed to do since overall phases are irrelevant, the atmospheric term becomes real, while the other two terms pick up phases of e 4iπ/5 . This is equivalent to having a phase η = 2π/5 in eq. (5.5). Different choices of phase for η are theoretically possible, but the phenomenologically successful choice for the relative phase of the atmospheric and solar terms (the first and second terms in eq. (5.5)) is η = 2π/5, whereas for example η = −2π/5 leaves the mixing angles unchanged but reverses the sign of the CP phases [33][34][35]. The dependence on see-saw phases was fully discussed in [33]. Here we only note that in this model the see-saw phases are restricted to a discrete choice corresponding to the fifth roots of unity due to the Z 5 symmetry. The fact that the decoupled third term proportional to m c (responsible for the lightest neutrino mass m 1 ) has the same phase as the second term proportional to m b (responsible for the solar neutrino mass) is a new prediction of the current model and will affect the m 1 dependence of the results. The neutrino mass matrix in eq. (5.5) may be diagonalised numerically to determine the physical neutrino masses and the PMNS mixing matrix as in eq. (5.2). We emphasise that, at leading order, with the phase η = 2π/5 fixed by the previous argument, the neutrino mass matrix involves just 3 real input parameters m a , m b , m c from which 12 physical parameters in the lepton sector are predicted, comprising 9 lepton parameters from diagonalising the neutrino mass matrix m ν in eq. (5.5) (the 3 angles θ l ij , 3 phases δ l , β l 1 , β l 2 and the 3 light neutrino masses m i ) together with the 3 heavy right-handed neutrino masses M i from eq. (5.8). The model is clearly highly predictive, involving 12 predictions in the lepton sector from only 3 input parameters.

A first numerical example
To take a numerical example, diagonalising the neutrino mass matrix in eq. (5.5), with the three input parameters m a = 0.035 eV, m b = 0.002 eV, m c = 0.002 eV, (5.9) the Mixing Parameter Tools package [57] gives the physical neutrino masses, eq. (5.9) shows the 3 input parameters, while eqs. (5.10), (5.12), 5.14 shows the 12 output predictions. One may regard the 3 input parameters in eq. (5.9) as fixing the 3 light physical neutrino masses in eq. (5.10), with all the 6 PMNS matrix parameters in eq. (5.12) as being independent predictions, along with the 3 right-handed neutrino masses in eq. (5.14). So far we have ignored charged lepton corrections which are expected in the model to be small. However the corrections are not entirely negligible as the following example shows. The charged lepton Yukawa matrix is given from eq. (3.15), which should be compared to the down quark Yukawa matrix in eq. (4.26). The off-diagonal elements of Y e are small, similar to those of Y d which are responsible for the small quark mixing angles and a correction to the Cabibbo angle of one degree. The quark mixing angles fix the three real parameters to be for example A = 9, B = 7, C = 36 and the down quark couplings in eq. (4.28). Including the charged lepton Yukawa matrix with these parameters and the same neutrino mass parameters as in eq. (5.9), the MPT package gives the lepton mixing parameters,

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Comparing the results in eq. (5.16) to those in eq. (5.12), we see that the atmospheric angle has increased by about 3 • to become maximal due to the (2, 3) element in the charged lepton Yukawa matrix, which is enhanced by a Clebsch factor of 3 relative to the same element in the down Yukawa matrix. The reactor angle has decreased slightly, and the CP oscillation phase has increased. With y 0 b taken to be positive instead of negative, and all the other parameters unchanged, we find the results below, The main effect of the sign of y 0 b is on the atmospheric and reactor angles.

Modified Georgi-Jarlskog relations
Since the charged lepton masses are known with much higher precision than the down type quark masses, the down Yukawa couplings in practice will be predicted from inputting the charged lepton masses in order to accurately fix y 0 d , y 0 s , y 0 b . Comparing Y e in eq. (5.15) to Y d in eq. (4.26), we find that we do not get exactly the GJ relations in eq. (3.19) due to the off-diagonal elements which also involve Clebsch factors. Numerically we find that, for y 0 b negative and the other parameters as above, the Yukawa eigenvalues at the GUT scale are approximately related as, For example for y 0 b negative we find the r.h.s. to be 7.3 which differs by more than 4 sigma. In order to bring this relation into better agreement with experiment we would need to increase this ratio, for example by increasing the muon Yukawa eignenvalue compared to the strange quark Yukawa eigenvalue. One way to do this is to introduce a flavon φ d15

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For example by suitable choice of the mixing angle γ we can arrange y 0 µ = 4.5y 0 s , By comparing Y e in eq. (5.23) to Y d in eq. (4.26), we find the modified GJ relations, which reproduces the central value in eq. (5.20). In the above estimate we have assumed A = 9, B = 7, C = 36 and the other couplings in eq. (4.28). Using the same neutrino mass parameters as in eq. (5.9), the MPT package gives the same lepton mixing parameters as for the GJ form in eq. (5.16), to very good accuracy.

Numerical results for neutrino masses and lepton mixing
In our numerical results we shall use the charged lepton Yukawa matrix in eq. As discussed previously, the lepton mixing depends on predominantly on m ν which involves the three real mass parameters m a , m b , m c , which are effectively fixed by the neutrino masses. However there are small corrections coming from Y e , which involves the real parameters A, B, C which determine the quark mixing angles and the real Yukawa couplings y 0 d , y 0 s , y 0 b which were previously determined from the down-type quark masses. As discussed previously (cf. eqs. (5.12), (5.16), 5.17) the effect on lepton mixing depends on the sign of y 0 b where the negative sign pushes up the atmospheric angle towards maximal, while also decreasing the reactor angle, while the positive sign has the opposite effect. Here we shall show results for the negative sign of y 0 b , as in eq. (4.28). We shall also use the same real parameters A = 9, B = 7, C = 36 which gave a good fit to the quark mixing angles and CP phase in eq. (4.31). Since lepton mixing depends mainly on the three real mass parameters m a , m b and m c which also determine the neutrino masses, we shall show results as a function of the neutrino mass parameters. Here we shall restrict ourselves to showing results where we keep the parameters appearing in Y e fixed at the above "benchmark" values, and vary only m a , m b and m c . The parameter m a is mainly responsible for the atmospheric neutrino mass and hence ∆m 2 31 , while m b is mainly responsible for the solar neutrino mass and hence ∆m 2 21 , with m c being mainly responsible for the lightest neutrino mass m 1 , which is zero for m c = 0. Once the parameters m a and m b are chosen to fix ∆m 2 31 and ∆m 2 21 for m c = 0 , then all neutrino parameters are predicted as a function of m c and hence m 1 , as described below.
Using the Mixing Parameter Tools package [57], in figure 6 we show the neutrino mass squared differences as a function of the lightest physical neutrino mass m 1 , corresponding to varying m c for various fixed values of m a , m b as given in the figure caption. Note that ∆m 2 21 actually increases with m 1 . This is because, with fixed m a and m b , switching on m c also increases m 2 . Since m 2 2 increases linearly with m c , after expanding, this has a more significant effect on ∆m 2 21 than the quadratic increase of m 2 1 , in the region of small m c . In figure 7 we show the resulting model predictions for the lepton mixing angles and CP oscillation phase. In all the plots (blue, red, green) coloured lines correspond to (high, central, low) values of ∆m 2 31 , while the (dashed, solid, dotted) styles correspond to (high, central, low) values of ∆m 2 21 . Note that the presently 3σ allowed range of mass squared parameters are [12,13]: ∆m 2 31 = (2.25 − 2.65).10 −3 eV 2 , ∆m 2 21 = (7.0 − 8.0).10 −5 eV 2 , and our choice of parameters covers most of these ranges. Thus the red solid curve corresponds to central values of both ∆m 2 31 and ∆m 2 21 for low values of m 1 , while the other curves reflect the uncertainty in the PMNS predictions due to the present precision in the neutrino mass squared differences.
Using the Mixing Parameter Tools package [57], in figure 7 we show the PMNS predictions of the model, resulting from eqs. (5.26), (5.27), plotted as a function of the lightest neutrino mass m 1 . From figure 7, the PMNS parameters are predicted to be in the following ranges:  The solar angle prediction is 34 • θ l 12 31 • , for the lightest neutrino mass in the range 0 m 1 0.5 meV, corresponding to a normal neutrino mass hierarchy. Since the solar angle is very insensitive to ∆m 2 31 and ∆m 2 21 values, and decreases as m 1 increases, an accurate determination of the solar angle will accurately determine m 1 in this model. The model also predicts a reactor angle θ l 13 = 9 • ± 0.5 • , close to its best fit value, with a significant dependence on ∆m 2 31 and ∆m 2 21 . A striking prediction of the model is the atmospheric angle which is predicted to be close to maximal to within about one degree for nearly all allowed ∆m 2 31 and ∆m 2 21 . The bulk of the parameter space for low m 1 predicts in fact θ l 23 = 45 • ± 0.5 • . It is worth noting that the most recent fit [11] is quite compatible with maximal atmospheric mixing to within 1σ for the case of a normal mass squared ordering, when the latest T2K disappearance data is included. The model also predicts accurately the CP phase with the bulk of the parameter space around δ l = 260 • ± 5 • , compatible with the best fit value, although the latter has a much larger error.
In general one can expect corrections coming from renormalisation group (RG) running [58,59] as well as canonical normalisation corrections [60][61][62]. For a SUSY GUT with light sequential dominance, as in the present model, the RG corrections for high tan β ∼ 50 have been shown to be [59]: sign means that the value increases in running from the GUT scale to low energy, while for low tan β 10 the RG corrections are negligible compared to the range of the predictions.
In particular the effect of right-handed neutrino thresholds [58] is expected to be negligible in this model since the heaviest right-handed neutrino mass is close to the GUT scale, while the lighter right-handed neutrinos have very small Yukawa couplings given by a ∼ 2.10 −5 and b ∼ 10 −3 from eq. (3.14). We emphasise that, since the parameters in Y e in eq. (5.27) are fixed from the quark sector, and the light neutrino masses are determined by three real parameters m a , m b , m c in eq. (5.26), the entire PMNS matrix containing 3 mixing angles and 3 CP phases emerges as a prediction of the model, although 2 of these CP phases will be difficult to measure for a normal neutrino mass hierarchy, so we have not plotted their predictions. The model may be tested most readily by its prediction of maximal atmospheric mixing and a normal neutrino mass hierarchy. It would be interesting to perform a χ 2 analysis of the quark and lepton masses and mixing angles predicted by the model, but that is beyond the scope of the present paper. The sum of neutrino masses is relevant for cosmology, since it contributes to hot dark matter, leading to a constraint on its value and eventually a measurement. This is defined by, Due to the rather strong normal hierarchy, this value is dominated by the value of m 3 , which is controlled by the parameter m a in the neutrino mass matrix in eq. (5.26).
In figure 9 we show the neutrinoless double beta decay parameter |m ee | (left panel) and the sum of neutrino masses Σm i (right panel) as predicted by the model, using the same parameter sets and colour coding as for the other plots. Note that for |m ee | (left panel) the three colours corresponding to different values of m a lie accurately on top of each other. The three dashed curves predict |m ee | ≈ 2.15 meV, the three solid curves predict |m ee | ≈ 2.10 meV and the three dotted curves predict |m ee | ≈ 2.05 meV, corresponding to the three different values of m b = 2.15, 2.10, 2.05. This can be understood from the neutrino mass matrix in eq. (5.26), since |m ee | = |m ν 11 | = m b , with the charged lepton matrix in eq. (5.23) providing only very small corrections to this result. The fact that eq. (5.31) was used to calculate the results and agrees very accurately with the expectation |m ee | = |m ν 11 | = m b provides a highly non-trivial check on our calculation of PMNS parameters and neutrino masses, and gives confidence to all our results. Note that |m ee |, being equal to m b , is approximately fixed by ∆m 2 21 in figure 6. Since |m ee | is predicted to be too small to measure in the foreseeable future, an observation of neutrinoless double beta decay could exclude the model. Similar comments apply to a cosmological observation of Σm i .

HO corrections to vacuum alignment
The triplet vacuum alignments are achieved by renormalisable superpotentials, as discussed in [34]. Since the messenger scale associated with any non-renormalisable corrections to vacuum alignment is unconstrained by the model, it is possible that any such terms may JHEP08(2014)130 be highly suppressed. In the present analysis we shall therefore ignore any HO corrections to the vacuum alignments in eqs. (2.12), (2.13).

HO corrections to Yukawa operators
Let us now consider HO corrections to the operators in eqs. (3.4), (3.5), 3.6, consisting of extra insertions of φ, leading to effective operators of the type, for n > 1. For example, Σu are both singlets of Z 5 , so either of these ratios may in principle be inserted into any of the LO operators in eqs. (3.4), (3.5) 3.6. However in practice, which HO insertions are allowed will depend on the details of the messenger sector. In order for an effective operator to be allowed, it is necessary that that the messenger diagram responsible for it can be drawn, and whether this is possible or not will depend on the choice of charges of the messenger fields X F and X F under all the symmetries.
In order to allow such HO operators as in eq. (6.1), for n > 1, at least one of the messenger fields X F and X F would have to be a triplet of A 4 in order to permit the coupling X F φX F where φ is a triplet, as is clear from figure 10 (left panel). Such triplet messenger fields X F and X F are not required in order to construct the LO operators and must be introduced for the sole purpose of allowing the HO operators of this kind.
Moreover, such triplet messenger fields would be dangerous since they may allow operators of the kind in eq. (6.1) for n = 1 involving the Higgs triplet h 3 which could contribute to up and charm quark masses for example.
For these reasons we have chosen not to introduce any messenger fields X F and X F which are triplets of A 4 , thereby forbidding HO operators of the type shown in eq. (6.1) for n ≥ 2 involving any Higgs fields or involving the A 4 triplet Higgs h 3 for n ≥ 1.
The couplings in eqs. (3.1), (3.2), 3.3 can also lead to HO operators of the generic kind, after integrating out the messengers, as shown in figure 10 (right panel).
where n ≥ 1. At the order n = 1, only a single operator of this kind is generated, which gives a correction in the (1,1) entry of Y u and hence a contribution to the up quark Yukawa coupling, where we have used y 0 d given in eq. (3.16). The correction is small if u Σ d d Σ u . Figure 10. Some possible higher order diagrams. The left panel shows a generic diagram involving triplet fermion messengers, which if present, would lead to effective higher order operators as in eq. (6.1). In our model we assume such triplet messengers to be absent which prevents diagrams with more than one φ field. The right panel shows a generic diagram responsible for the effective higher order operators as in eq. (6.2).

HO corrections to Majorana operators
The relevant bilinear charges in the Majorana sector are The messengers which transform under A 4 × Z 5 as X ξ i ∼ (1, α i ) can couple to the Majoron field ξ ∼ (1, α 4 ) leading to the LO operators in eq. (3.7) (dropping H c and Λ), Since each insertion of ξ carries a suppression factor of ξ /Λ ∼ 10 −5 , HO operators involving more powers of ξ, such as F c 1 F c 2 ξ 4 , are negligible.

Conclusions
In this paper we have proposed a rather elegant theory of flavour based on the Pati-Salam gauge group combined with A 4 × Z 5 family symmetry which provides an excellent description of quark and lepton masses, mixing and CP violation. Pati-Salam unification relates quark and lepton Yukawa matrices and in particular predicts Y u = Y ν , leading to Dirac neutrino masses being equal to up, charm and top masses. The see-saw mechanism involves very hierarchical right-handed Majorana neutrino masses with sequential dominance. The A 4 family symmetry determines the structure of Yukawa matrices via CSD4 vacuum alignment, with the three columns of Y u = Y ν being proportional to (0, 1, 1) T , (1, 4, 2) T and (0, 0, 1) T , respectively, where each column has a multiplicative phase determined by Z 5 breaking, which controls CP violation in both the quark and lepton sectors. The other Yukawa matrices Y d ∼ Y e are both approximately diagonal, with charged lepton masses related to down quark masses by modified GJ relations, and containing small off-diagonal elements responsible for the small quark mixing angles θ q 13 and θ q 23 . The model hence predicts the Cabibbo angle θ C ≈ 1/4, up to such small angle corrections.
The main limitation of the model is that it does not predict the charged fermion masses. However the third family masses are naturally larger since they arise at renormalisable JHEP08(2014)130 order, while the hierarchy between first and second family masses can be understood to originate from hierarchies between flavon VEVs. Although the model does not predict the small quark mixing angles, it does offer a qualitative understanding of both CP violation and the Cabibbo angle θ C ≈ 1/4, which, as discussed above, is closely related to the lepton mixing angles via the CSD4 vacuum alignment. Moreover, the model contains 6 fewer parameters in the flavour sector than the 22 parameters of the SM, and hence predicts the entire PMNS matrix, as is clear from eqs. (5.26), (5.27) where all the parameters which appear there are fixed by fermion (including neutrino) masses and small quark mixing angles. Hence the model predicts the entire PMNS lepton mixing matrix with no free parameters, including the three lepton mixing angles and the three leptonic CP phases with negligible theoretical error from HO corrections. The resulting PMNS matrix turns out to have an approximate TBC form as regards maximal atmospheric mixing and the reactor angle θ l 13 ≈ 9 • , although the solar angle deviates somewhat from its trimaximal value, corresponding to a negative deviation parameter s ∼ −0.03 to −0.1, where sin θ l 12 = (1 + s)/ √ 3 [63]. The predictions of a normal neutrino mass hierarchy and maximal atmospheric angle will both be either confirmed or excluded over the next few years by current or near future neutrino experiments such as SuperKamiokande, T2K, NOνA and PINGU [64][65][66][67][68]. The Daya Bay II reactor upgrade, including the short baseline experiment JUNO [69][70][71], will also test the normal neutrino mass hierarchy and measure the reactor and solar angles to higher accuracy, enabling precision tests of the predictions θ l 13 = 9 • ± 0.5 • and 34 • θ l 12 31 • , for the lightest neutrino mass in the range 0 m 1 0.5 meV. With such a mass range, neutrinoless double beta decay will not be observable in the foreseeable future. In the longer term, the superbeam proposals [72] would measure the atmospheric mixing angle to high accuracy, confronting the prediction θ l 23 = 45 • ± 0.5 • , and ultimately testing the prediction of the leptonic CP violating oscillation phase δ l = 260 • ± 5 • .

Acknowledgments
SFK would like to thank Pasquale Di Bari, Simon King and Christoph Luhn for discussions SFK also acknowledges partial support from the EU ITN grant INVISIBLES 289442 .
A A 4 A 4 has four irreducible representations, three singlets 1, 1 and 1 and one triplet 3. The products of singlets are: 1 ⊗ 1 = 1 1 ⊗ 1 = 1 1 ⊗ 1 = 1 1 ⊗ 1 = 1 . (A.1) The generators of the A 4 group, can be written as S and T with S 2 = T 3 = (ST ) 3 = I. We work in the Ma-Rajasakaran basis [25] where the triplet generators are, where S ab are Pati-Salam singlet fields which develop VEVs somewhat higher than the Pati-Salam breaking scale. When H c gets a VEV in its right-handed neutrino component, it will project out the T 3R = +1/2 component of h a , which we write as h + a . Similarly when H c gets a VEV in its right-handed neutrino component, it will project out the T 3R = −1/2 component of h b , which we write as h − b . The diagrams responsible for generating the operators of the form in eq. (B.2) are shown in figure 11. These diagrams should be considered as Higgsino doublet mixing diagrams. The Higgsino messenger fields which couple to (h a H c ) are denoted as X Ha and those which couple to (H c h b ) are denoted as X H b , where the messenger masses are generated by the couplings X Ha S ab X H b when S ab develops its VEV, leading to the effective operators in eq. (B.2).
The choice of singlets S 11 , S 33 , S 24 , S 34 with appropriate Z 5 and A 4 charges, lead to the following particular operators of the general form of eq. (B. Note that S ab has the same A 4 × Z 5 charges as S ba .

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