Radiative Corrections to Light Neutrino Masses in Low Scale Type I Seesaw Scenarios and Neutrinoless Double Beta Decay

We perform a detailed analysis of the one-loop corrections to the light neutrino mass matrix within low scale type I seesaw extensions of the Standard Model and their implications in experimental searches for neutrinoless double beta decay. We show that a sizable contribution to the effective Majorana neutrino mass from the exchange of heavy Majorana neutrinos is always possible, provided one requires a fine-tuned cancellation between the tree-level and one-loop contribution to the light neutrino masses. We quantify the level of fine-tuning as a function of the seesaw parameters and introduce a generalisation of the Casas-Ibarra parametrization of the neutrino Yukawa matrix, which easily allows to include the one-loop corrections to the light neutrino masses.


I. INTRODUCTION
The main goal of this work is to study in detail under which conditions the right-handed (RH) neutrinos present in a general type I seesaw scenario [1] can give a direct sizable contribution to the neutrinoless double beta (0νββ) decay rate, i.e., a contribution in the range of sensitivity of the current and upcoming 0νββ decay experiments, once all the relevant constraints are included in the analysis.
In [2,3], it was shown that a sizable sterile neutrino contribution to the 0νββ decay can be achieved if the heavy neutrino spectrum is hierarchical, with at least one RH neutrino with mass M below 100 MeV and the other state(s) above this scale. However, this spectrum is disfavoured by cosmological observations since the region M ∈ [1 eV, 100 MeV] is excluded by BBN and CMB data [4,5]. In [6][7][8] the possibility of having a relevant contribution from heavy RH neutrinos up to the TeV scale was explored. 1 It was found that indeed RH neutrinos as heavy as 100 GeV-10 TeV could, in principle, give a sizable and observable contribution to the 0νββ decay rate. In [8] the role of the fine-tuning and one-loop effects were discussed, concluding that for RH neutrino masses above 10 GeV a relatively high level of fine-tuning would be required. In [3] a more detailed study of the one-loop effects was performed and it was found that indeed they are significant and can play a very important role in the type I seesaw scenario. The lepton number violation introduced through the RH neutrino Majorana mass term, required to obtain a sizable effect in the 0νββ decay rate, naturally appears at one-loop level in the light neutrino sector. If fine-tuning is not invoked, the light neutrino mass constraints on the one-loop corrections make it very difficult to obtain a significant (RH) heavy Majorana neutrino contribution in the 0νββ decay effective Majorana mass, i.e., to have |m heavy ββ | 0.01 eV, m heavy ββ being the heavy Majorana neutrino contribution under discussion. We will show, in particular, that the scenario in which RH neutrinos with a mass M 1 GeV can give a sizable contribution to the 0νββ decay rate necessarily involves a fine-tuned cancellation between the tree-level and one-loop light neutrino contributions.
More specifically, in this work we re-analyse the conditions under which the heavy Majorana neutrinos with masses M > 100 MeV of the type I seesaw scenario can give a significant 1 The interplay between the light and heavy Majorana neutrino contributions in 0νββ decay was investigated phenomenologically first in [9]. direct contribution to the 0νββ decay effective Majorana mass, i.e., a contribution in the range of sensitivity of the current and upcoming 0νββ decay experiments. We show that for M a few GeV this requires a relatively large active-sterile neutrino mixing (charged current couplings of the heavy Majorana neutrinos). We clarify which seesaw realisations can provide the requisite mixing. We discuss the impact of the one-loop corrections in the different type I seesaw realisations considered. We analyse also numerically the problem of the sizable heavy Majorana neutrino contribution to the 0νββ decay effective Majorana mass, by studying the full parameter space, including the relevant one-loop corrections and the bounds on the active-sterile neutrino mixing from direct searches, charged lepton flavour violation and non-unitarity [10][11][12][13][14][15][16][17]. We quantify, in particular, the level of fine-tuning required in order to have a sizable heavy neutrino contribution to the 0νββ decay rate. In order to do the analysis and generate the right pattern for the light neutrino masses and mixing, we have constructed a modification of the Casas-Ibarra parametrization [18], which takes into account the impact of the one-loop corrections.
The paper is organized as follows: in section II we derive under which conditions it is possible to obtain a sizable active-sterile neutrino mixing, which can strongly affect the effective Majorana neutrino mass, m ββ . In section III we study the impact on m ββ of the one-loop corrections to the light neutrino masses and present our modified Casas-Ibarra parametrization which takes into account the one-loop effects. In section IV we perform the numerical analysis and quantify the level of fine-tuning necessary to have a dominant contribution in m ββ from the exchange of the heavy (sterile) neutrinos. Finally, we summarise our results in the concluding section.

II. LARGE ACTIVE-STERILE NEUTRINO MIXING AND 0νββ DECAY
We consider the most general type I seesaw scenario [1] with n ≥ 2 RH neutrino fields ν sR (s = 1, . . . , n). After the spontaneous breaking of the electroweak (EW) symmetry the full neutrino mass Lagrangian is where = e, µ, τ and ν c sL ≡ C ν sR T , C being the charge conjugation matrix. M R = (M R ) T is the Majorana mass matrix of the RH neutrinos and m D is the 3 × n neutrino Dirac mass matrix. The full mass matrix derived from Lagrangian (1) is therefore where m i (i = 1, 2, 3) and M k (k = 1, . . . , n) are the light and heavy Majorana neutrino masses, respectively. We define O as a 3 × 3 matrix with all elements equal to zero. The full neutrino mass M is diagonalised by a (3 + n) × (3 + n) unitary matrix U , through a well known rotation between the neutrino flavour and mass eigenstates. We give below the relation between the left-handed (LH) components of the corresponding fields (ν L , ν c sL and Taking into account that the active block of U is unitary to a very good approximation, the complete mixing matrix can be expanded as 2 where θ is a 3 × n matrix with "small" entries, which characterises the mixing between the active and the sterile neutrinos, U PMNS is the PMNS neutrino mixing matrix [19,20] and V is a n × n unitary matrix. The quantity (θ V ) k , = e, µ, τ , k = 1, . . . , n, is the coupling of the heavy Majorana neutrino N k to the charged lepton in the weak charged lepton current, and to the flavour neutrino ν in the weak neutral lepton current.
From the diagonalization of the complete neutrino mass matrix M, at leading order in θ we have [6] wherem It follows from Eqs. (5) and (7) that In terms of the seesaw parameters we have for the active-sterile neutrino mixing: Using Eqs. (5) and (10), we recover the usual type I seesaw relation for the (tree-level) light neutrino mass matrix, namely The effective Majorana neutrino mass, m ββ , which enters in the 0νββ decay amplitude, receives, in general, two different contributions, corresponding to the exchanges of the light and heavy virtual Majorana neutrinos: with m light where we have used Eq. (9), which holds at tree-level in the type I seesaw models. A good estimate for the contribution due to the heavy Majorana neutrino exchange for M k 100 MeV is [2] m heavy where M a ≈ 0.9 GeV and f (A) depends on the decaying isotope considered. For, e.g., 48 Ca, Using Eq. (14), it is easy to estimate the minimum mixing (θV ) min required in order to have a contribution at the aimed sensitivity of the next generation of 0νββ decay experiments, that is |m heavy ββ | 10 −2 eV. In Fig. 1 we compare this estimate for (θV ) min for the  The solid line corresponds to the naive seesaw scaling of (θV ) 2 (see the text for further details).
From Fig. 1  In order to understand under which conditions an enhancement with respect to the naive scaling of the active-sterile mixing (or equivalently, of the charged current couplings of the heavy Majorana neutrinos (θV ) k ) can be expected, we employ the Casas-Ibarra parametrization of θV [18]. In this parametrization the light neutrino masses and the angles and phases of the PMNS matrix are input parameters, in such a way that the correct light neutrino mixing pattern is always recovered. The Casas-Ibarra parametrization is obtained rewriting Eq. (5) as where R is a general 3 × n complex matrix which parametrizes the new physics degrees of freedom associated to the sterile neutrino sector. Using this parametrization, θV can be written as The matrix V can be set to the unit matrix if one works in the basis in which the Majorana Naively, from Eq. (11) one may conclude that θV ≈ O m M , i.e., that the mixing (or coupling) θV is expected to be suppressed by the heavy neutrino mass scale. However, having a larger mixing is perfectly possible due to an enhancement factor contained in the matrix R [6,7]. Obviously, such enhancement can only be in agreement with the light neutrino spectrum if there is a non-trivial suppression/cancellation in the l.h.s. of Eq. (9). This extra suppression is related to particular textures of the neutrino mass matrix, which can be motivated, for instance, introducing an extra U (1) global symmetry in the Lagrangian, as it is the case in the so called "inverse" and "direct" seesaw models [23,24]. In these models the indicated global symmetry can be identified with that corresponding to the conservation of a non-standard lepton charge (see further).
In the following we will focus on the minimal seesaw scenario with n = 2 RH sterile neutrinos 4 (see, e.g., [25]) giving rise to two heavy Majorana mass-eigenstate neutrinos, which predicts one massless and two massive light active neutrinos. For the light neutrino mass spectrum with normal hierarchy (NH) and inverted hierarchy (IH) we have The current best fit values obtained from the global fit analysis in [26] are ∆m 2 31 = 2.457 × 10 −3 eV 2 (NH) and ∆m 2 32 = −2.449 × 10 −3 eV 2 (IH) .
In this minimal seesaw scenario, the two (tree-level) non-zero light neutrino masses m tree 2 and m tree 3 (m tree 1 ) in the case of NH (IH) neutrino mass spectrum satisfy the relation: which is basis independent.
In the considered case the R-matrix, which enters into Eq. (16), can be parametrized as [7] where θ 45 and γ are real parameters. If R were real, i.e., γ = 0, there is no way to obtain any enhancement of the couplings/mixings θV of interest since R would essentially be a real orthogonal matrix. However, for γ = 0 and e ±γ 1 an enhancement of θV is possible: In fact, for e ±γ 1 the expression of R in the NH case reduces to Similarly, one can derive from (22) the same limit of R for the IH neutrino mass spectrum: Notice that the Casas-Ibarra parameter γ in (24) and (25) can be related to the maximum eigenvalue y [7] of the Dirac mass matrix m D in Eq. (2), that is where z denotes the relative mass splitting of the two heavy Majorana neutrino masses, z = (M 2 − M 1 )/M 1 , and v = 246 GeV is the EW symmetry breaking scale.
Introducing the expression (24) (or (25)) in Eq. (16) one obtains [6,7,27,28] Then, in terms of y the active-sterile neutrino mixing in Eq. (16) takes the form [7] |(θV ) 1 | 2 = 1 2 (2 + z) Eq. (28) holds and m heavy ββ is given by Eq. (32), was investigated in detail in [7] in the case when the two heavy Majorana neutrinos form a pseudo-Dirac pair, 0 < ∆M = M 2 − M 1 M 1 , M 2 , and have masses in the interval ∼ (50 − 1000) GeV. It was found that there exists a relatively large region of the allowed parameter space of the scheme in which the heavy Majorana neutrino contribution can change drastically the predictions based on the light Majorana neutrino exchange contribution. More specifically, it was found that [7]: i) |m ββ | in the case of NH spectrum can have values in the interval 0.01 eV |m ββ | 0.1 eV, i.e., in the range of sensitivity of the current GERDA [29], EXO [30], Kamland-Zen [31] and CUORE [32] experiments and of a few other experiments under preparation (Majorana [33], SNO+ [34], AMORE [35], etc.). We recall that in the case of 0νββ decay generated only by light Majorana neutrino exchange we have (see, e.g., [36,37]) |m ββ | = |m light ββ | 0.005 eV; ii) |m ββ | in the case of IH spectrum can be strongly suppressed due to partial, or even total, cancellation between m light ββ and m heavy ββ in m ββ (see also [38]). Since the magnitude of m heavy ββ , as it follows from Eq. (32), depends on the atomic number A of the decaying nucleus [9], the cancellation between m light ββ and m heavy ββ in m ββ can take place for a given nucleus (say, e.g., for 48 Ca) but will not hold for other nuclei ( 76 Ge, 82 Se, 130 Te, 136 Xe, etc.). If the 0νββ decay is due only to the light Majorana neutrino exchange we have in the case of IH spectrum, as is well known [39] (see also, e.g., [36]), 0.013 eV |m ββ | = |m light ββ | 0.050 eV. On the other hand, in [7] the role of the one-loop corrections was not studied. In [3] it was shown that the one-loop corrections to the light neutrino masses generated in the scheme under discussion turn out to be very relevant. Essentially, a sizable heavy contribution to the 0νββ decay for heavy masses in the range ∼ (50 − 1000) GeV generates at the same time a very large one-loop correction to the light neutrino masses. In this work we analyse in detail the role of the one-loop effects showing that similar conclusions to the ones drawn in [7] will be obtained. However, we will also show that the price one has to pay in order to have a significant impact of the heavy neutrinos in the 0νββ decay is the requirement of a highly fine-tuned cancellation between the tree-level and one-loop contributions to the light neutrino masses.

B. Comparison with Extended and Inverse Seesaw Scenarios
As an application of the previous results, we consider the effect of heavy RH neutrinos on the 0νββ decay amplitude in the case of two different realisations of the type I seesaw scenario, which predict a large active-sterile neutrino mixing θV , that is the well known extended seesaw (ESS) [40] and inverse/direct seesaw (ISS) [23,24] models. In particular, we will clarify how the large mixing realisations described in the previous section in terms of the Casas-Ibarra parametrization match with the ISS and ESS scenarios.
In order to understand the predictions in these classes of models it is useful to adopt the following parametrization of the generic mass terms in the seesaw Lagrangian (1), namely where Y i ≡ (y ie , y iµ , y iτ ) T , for i = 1, 2. This parametrization is completely general and, in principle, , µ, µ and Λ can take any value. 6 However, , µ and µ can be interpreted as lepton number violating couplings and, therefore, in principle they take arbitrarily small values, because in this case there is an approximate global symmetry of the seesaw Lagrangian corresponding to the conservation of the lepton charge L = L e + L µ + L τ + L 1 − L 2 , where L 1 and L 2 are the charges carried by the RH neutrino fields ν 1R and ν 2R , respectively. In the limit of = µ = µ = 0, the conservation of L is exact. In this case the neutrino sector consists of three massless neutrinos and one massive Dirac fermion, which can be inferred, in particular, directly from the expression of the charge L in terms of the charges L and L 1,2 [41,42]. The exact conservation of L corresponds to the case in which condition (28) is exactly fulfilled and the RH neutrino splitting satisfies: In terms of the new parameters, the exact (tree-level) expression of the light neutrino mass matrix given in (11) is proportional to µ and , that is and thus if µ = = 0 there is a complete cancellation at tree-level for the light neutrino masses. As we will see in the next section, if µ is different from zero, at least one neutrino 6 In the following we will assume for simplicity that all the parameters introduced in Eq. (33) are real.
mass can be generated at one-loop, even for µ = = 0 [3]. Furthermore, from the diagonalization of (34), we obtain for the product of the smallest (m tree l ) and the largest (m tree h ) light neutrino masses: From this relation it follows that in order to have two massive active neutrinos at tree-level, i.e., m tree l,h = 0, i) an explicit breaking of the lepton charge conservation via the neutrino Yukawa couplings is necessary, that is the parameter must always be different from zero; ii) the vectors of neutrino Yukawa couplings Y 1 and Y 2 cannot be proportional.
Accordingly, the two seesaw limits of Eq. (34) which give rise to large active-sterile neutrino mixing θV and generate sufficiently small active neutrino masses are: . This limit matches the so-called extended seesaw [40] models and corresponds to a hierarchical spectrum for the heavy neutrinos: where we also show the corresponding mixing with the active neutrinos. Then, the approximate tree-level contribution to the 0νββ decay effective Majorana mass due to the exchange of the light and the heavy neutrinos is • ii) Λ y 1α v µ , µ, y 2α v (ISS limit). This limit corresponds to a minimal realisation with only two RH neutrinos of the so-called inverse or direct seesaw models [28].
In this case the heavy neutrino spectrum is quasi-degenerate, forming a quasi-Dirac pair [43,44] In this limit the light and heavy contributions to the 0νββ decay rate are given by: m heavy Both of them are proportional to the small lepton number violating parameters, as it should be. Notice that the expression of m light ββ above is exactly the same as the one given in Eq. (40).
On one hand, it follows from Eqs. (40), (41), (44) and (45) that a relatively large contribution to the 0νββ decay rate due to the heavy Majorana neutrino exchange might be possible at tree-level without affecting the smallness of the light neutrino masses since in the limits considered here m heavy ββ ∝ µ , while m light ββ is independent of µ . On the other hand, Eqs. (36)(37) and (42)(43) confirm that the condition to obtain relatively large mixings, Eq. (28), is fulfilled at leading order, that is in the Casas-Ibarra parametrization the R-matrix corresponding to these two cases is similar to the textures reported in Eqs. (24) and (25).
Finally, we note that in the case of the ISS model, the smallness of the light neutrino masses comes from the existence of an approximate symmetry corresponding to the conservation of the lepton charge L . In contrast, in the ESS limit, the conservation of the lepton charge L is strongly violated through the µ coupling. This means that, in principle, the one-loop corrections to the neutrino masses can be expected to be more important in the ESS limit than in the ISS one since in the ESS case there is no symmetry protecting the light neutrino masses from getting relatively large corrections [3].

III. ONE-LOOP CORRECTIONS TO THE NEUTRINO MASS MATRIX
We turn now to the computation of the one-loop corrections to the light neutrino mass matrix and the effective Majorana neutrino mass associated to 0νββ decay amplitude.
At one-loop the neutrino self-energy Σ(p) provides the dominant finite correction to m ν [3,[45][46][47][48], which depends on the square of the neutrino Yukawa couplings, as in the tree-level contribution (11), and is further suppressed by the one-loop factor 1/(16 π 2 ). In a generic basis, with the Dirac and Majorana mass terms defined in Lagrangian (1), we obtain: where the new Majorana mass term generated at one-loop is in this case The loop function F (x) is defined as M H and M Z denoting the Higgs and the Z boson mass, respectively. Hence, the overall light neutrino mass matrix, m ν , is given by the sum of the tree-level (11) and one-loop (47) terms, which in the basis of charged lepton mass eigenstates satisfies the relation The finite radiative correction given in (47)  In the basis in which the RH neutrino mass is diagonal, the one-loop correction of interest has the following form: where we have used Eqs. (6) and (7). The contribution of the one-loop correction under discussion to the effective Majorana neutrino mass m light ββ , generated by the light Majorana neutrino exchange, as can be shown, is given by A. The Scheme with Two RH Neutrinos In the phenomenologically interesting scheme with two RH neutrinos, for each non-zero eigenvalue m k of Eq. (49), we have the exact relation where the second equality follows form the Sylvester's determinant theorem and we have introduced the function 7 Using (52) and (20), we get the identity where m l (m h ) is the smaller (larger) non-zero active neutrino mass, whose experimental value in the cases of NH and IH neutrino mass spectrum is given in Eqs. (17) and (18) here. As a consequence of Eq. (54), one has that in the case m tree l = 0, i.e. if two of the active neutrinos are massless at tree-level, it is not possible to generate at one-loop level two non-zero light (active) neutrino masses in the spectrum. In other words, in such a scenario both the solar and atmospheric neutrino oscillation mass differences cannot be radiatively generated.
As it is not difficult to show, in the minimal scenario with only two heavy Majorana neutrinos, in which condition (28) is exactly fulfilled, the one-loop contribution to the light neutrino mass matrix goes to zero in the limit ∆M = M 2 − M 1 → 0. Indeed, from Eqs. (28) and (51) we find: If, in addition, z 1, this expression further simplifies to: In the opposite limit, namely, takes also a rather simple form for z 1. In this case, to leading order in z 1, we obtain: Thus, in the scheme considered here, in which condition (28)   e.g., M 1 = 10 3 GeV and the maximal value of |(θV ) 2 e1 | = 10 −3 allowed by the current data. This requires, however, exceedingly small values of z, which lead to a subleading heavy neutrino contribution. Indeed, using the quoted values of M 1 and |(θV ) 2 e1 |, and taking into account that v = 246 GeV, it is not difficult to find from Eq. (58) that we can have |m 1−loop ββ | ≈ 0.01 (0.10) eV for z ≈ 6 × 10 −10 (6 × 10 −9 ). Such a small value of z suggests a severe fine-tuning, but it can also be understood in the context of the ISS scenario as a technically naturally small value of the lepton number violating parameters of this model.

B. One-loop Generalisation of the Casas-Ibarra Parametrization
In order to make sure that we generate the correct light neutrino mixing pattern, it is useful to generalise the Casas-Ibarra parametrization introduced in the previous section Hence, in analogy to the tree-level contribution, we have now Thus, we get the following expression for the heavy Majorana neutrino couplings in the weak charged current, or equivalently, for the active-sterile neutrino mixing, at one-loop order: In the numerical analysis reported in section IV we will make use of this parametrization of θV , with R given in (21) and (22) For the ESS scenario we have at leading order in Λ/µ Notice that for µ M H , M Z , this expression reduces to Therefore, when µ M H , M Z , since the lepton number violating scale µ is introduced at high energies, the one-loop contribution to the light neutrino masses appears to be suppressed as 1/µ , as expected.
In the ISS realisation, i.e. for v, µ, µ Λ, we obtain It is remarkable that in the ESS limit with µ M H , M Z and in the ISS limit the oneloop correction to the light neutrino masses has a contribution proportional to µ . This dependence on µ is very relevant since at one-loop the light neutrino contribution to the 0νββ decay amplitude does depend directly on µ , as for the heavy contribution in (41) and (45). This makes much more difficult to obtain a dominant contribution from the RH neutrinos in this limit, unless a fine-tuning of the seesaw parameters is introduced to guarantee the smallness of the neutrino masses as it was indeed already shown in Fig. 3.

IV. LARGE HEAVY NEUTRINO CONTRIBUTION TO 0νββ DECAY
In this section, we will address in more detail the question if the RH neutrinos can eventually give a sizable contribution to the 0νββ decay rate. As we have already mentioned, cosmological constraints close the mass window of M < 100 MeV [4,5] and thus only if the RH neutrino masses are larger than 100 MeV, a direct contribution to the process of interest can be expected.
Following the notation in Ref. [2], the 0νββ decay rate can be written as where G 01 is a well-known kinematic factor, U is the unitary matrix given in Eq. (4) which diagonalizes the complete neutrino mass matrix, m j are the corresponding eigenvalues, i.e., the neutrino masses (light and heavy), and M 0νββ are the Nuclear Matrix Elements (NMEs) associated with the process. Notice that the NMEs depend on the mass of the neutrino mediating the process since the dependence on the neutrino propagator is already included in the NMEs computation. The sum should be made over all the neutrino masses, including the heavy ones. In the following we will use the NMEs data provided in [2]. In particular, we will consider the NMEs computed for the 76 Ge. However, we have checked that the conclusions of our analysis do not significantly change considering a different nucleus.
We will use the modified Casas-Ibarra parametrization of the active-sterile neutrino mixing given in Eq. (61), to compute the full effective Majorana neutrino mass m ββ , which is given by the sum of the contributions from the exchange of the light and heavy Majorana neutrinos. In this way, we include in the computation the effect of the one-loop correction to the light neutrino masses, reproducing at the same time the correct neutrino oscillation parameters. We will also take into account the relevant bounds on the active-sterile mixing which come from direct searches, charged lepton flavour violation and non-unitarity constraints [10][11][12][13][14][15][16][17]. Notice that the inclusion of such bounds guarantees the perturbativity of the neutrino Yukawa couplings for any value of RH neutrino masses considered in this paper.
In the top panels (down panels) of Figs In the red shaded area of Figs. 4 and 5, the ratio between the leading and next to leading order contributions to the light neutrino masses in the seesaw expansion is smaller than 10.
The next to leading order contribution is given by [49]: From this expression, one can conclude that a cancellation between the one-loop and treelevel contributions to the light neutrino masses remains at next to leading order in the seesaw The measured neutrino oscillation parameters are fixed to the central values reported in [26].
expansion. This is in agreement with Figs. 4 and 5, which show that the next to leading order contribution is always negligible in the range of parameters of interest.
Ignoring for the time being the impact of the two-loop corrections, which will be com- In the NH case, the light neutrino contribution is smaller than 10 −2 eV and therefore any sizable effect to the process is due to the heavy neutrinos. This is why in the NH case we plot the total contribution m ββ , including light and heavy neutrinos. the NH and IH neutrino mass spectra: Taking into account that Fig. 4 is obtained by setting to zero the phase θ 45 and the Dirac and Majorana phases in the PMNS matrix and by using the best fit values of the neutrino oscillation parameters, Eqs. (68) and (69) imply the following relations between |(θV ) e1(e2) | 2 and the parameter γ:  A of the decaying nucleus [9].
The requirement of a sizable contribution of heavy neutrinos with masses 1 GeV to the 0νββ decay implies strong cancellations between the tree-level and one-loop expressions in the light neutrino mass matrix m ν originated from the seesaw mechanism. We show that such a cancellation can always be achieved while being consistent with neutrino oscillation data and low energy constraints from direct searches, charged lepton flavour violation and non-unitarity by using a generalisation of the Casas-Ibarra parametrization of the neutrino Yukawa matrix, which can be derived from Eqs. (60) and (61). We clarify the connection between this parametrization and the lepton number breaking terms in the seesaw Lagrangian, as usually defined in extended as well as inverse/direct seesaw UV completions of the Standard Model. Then, we numerically quantify the level of fine-tuning between the tree-level Finally, we can conclude on the basis of the results obtained in the present analysis that 0νββ sets the strongest constraints on lepton number violation in low scale type I seesaw extensions of the Standard Model. In particular, this implies a strong suppression of processes which involve the production at colliders (LHC included) of RH neutrinos and their decays with two like-sign charged leptons in the final state (see, e.g., [6,50]). Japan.
In this way, one can obtain a closed form for the logarithms which enter in Eq.
Therefore, by replacing Eqs. (A12) in (A3), we obtain an analytic expression for the one-loop contribution to the light Majorana neutrino mass matrix as a function of the parameters given in (33).