A New Sensitivity Goal for Neutrino-less Double Beta Decay Experiments

We study the implications of the Dark-LMA solution to the solar neutrino problem for neutrino-less double beta decay ($0\nu\beta\beta$ ). We show that while the predictions for the effective mass governing $0\nu\beta\beta$ remains unchanged for the inverted mass scheme, that for normal ordering becomes higher for the Dark-LMA parameter space and moves into the"desert region"between the two. This sets a new goal for sensitvity reach for the next generation experiments if no signal is found for the inverted ordering by the future search programmes.

Introduction : Fermions can be of two types -Dirac or Majorana. A Majorana particle is a self-conjugate fermion. All known fermions other than the neutrino are Dirac particles. Neutrinos, being neutral, are the only known particle that can possibly be a Majorana fermion. Hence, the question whether neutrinos are Dirac or Majorana particle is one of the most fundamental questions in physics. The most straightforward way to probe the Majorana nature of neutrinos is through neutrino-less double beta decay (0νββ). While beta decay involves the decay of a radioactive nucleus into a daughter nucleus along with an electron and an electron-type antineutrino, neutrino-less double beta decay is a rare process in which a nucleus of charge Z and mass number A decays into a daughter, producing two electrons and no neutrinos : (A, Z) → (A, Z + 2) + 2e − [1]. A positive signal of this will be a definite confirmation of the existence of lepton number violating Majorana mass term for the neutrinos [2]. Such a term requires transcending beyond the Standard Model of particle physics and could also be related to the observed preponderance of matter over antimatter which is essential for our existence. Thus it is not surprising that searches for 0νββ have been on-going for the past several decades [3]. While no undisputed positive signal has been seen in any of the experiments so-far, a lower limit (90% C.L.) on the 0νββ lifetime of T 1/2 ( 136 Xe) > 1.5 × 10 25 years has been obtained from KamLAND-Zen [4], T 1/2 ( 76 Ge) > 8 × 10 25 years from GERDA [5] and T 1/2 ( 130 T e) > 1.5 × 10 25 years from combined results of CURCINO and CUORE [6]. In this work we assume that 0νββ is driven solely via a Majorana mass term for the neutrinos. Therefore, non-observation of 0νββ puts an upper limit on the effective neutrino mass which depends on the neutrino mass and mixing parameters. The effective mass depends crucially on whether the neutrino mass spectrum conforms to normal ordering (NO) or inverted ordering (IO), which corresponds to whether the third mass eigenstate is the heaviest or lightest, respectively. In addition to the neutrino mass ordering, the effective neutrino mass also depends on some of the other neutrino mass and mixing parameters -the two mass squared differences ∆m 2 21 and ∆m 2 31 , two of the three mixing angles, viz., θ 12 and θ 13 and the Majo-rana phases α 1 and α 2 . By allowing these parameters to vary in their current 3σ allowed range, one obtains two bands of predicted values for the effective mass for IO and NO, separated by a "desert region". The effective mass corresponding to IO (∼ 0.015 -0.05 eV) is expected to be probed comfortably in the next-generation 0νββ experiments which include LEGEND, GERDA-II,MAJORANA D, CUPID, SNO+, KamLAND2-Zen, nEXO, NEXT 1.5K, PANDAX III 1k , Su-perNEMO etc. [7]. While lowering the sensitivity of these experiments to be able to probe the effective mass for the NO case is going to be challenging, it is possible to make some inroads into this region as well albeit with a lower probability [8]. Many of these planned experiments will be capable of probing the "desert region" i.e. territories < ∼ 0.01 eV even if they fall short of testing significant parts of the NO band [8][9][10][11].
In this letter we show, for the first time, the impact of the so-called Dark-LMA (DLMA) [12][13][14] solution to the solar neutrino problem on 0νββ. The standard LMA solution corresponds to standard neutrino oscillations with ∆m 2 21 7.5×10 −5 eV 2 and sin 2 θ 12 0.3, and satisfies the solar neutrino data at high significance. The DLMA solution appears as a nearly-degenerate solution to the solar neutrino problem for ∆m 2 21 7.5 × 10 −5 eV 2 and sin 2 θ 12 0.7, once we allow for the existence of non-standard neutrino interactions (NSIs) in addition to standard oscillations. The KamLAND experiment is unable to break this degeneracy since it observes neutrino oscillations in vacuum which depends on sin 2 2θ 12 and hence is same for both LMA and DLMA solutions 1 . The occurrence of the DLMA solution can also adversely affect the determination of mass ordering in beam based neutrino oscillation experiments in presence of NSI [15][16][17]. We will show that while the IO band for the effective mass in 0νββ experiments remains nearly same for LMA and DLMA solutions, the NO band gets shifted upwards for DLMA into the desert region mentioned above. As a result this may make it possible for the next-generation experiments to start probing 0νββ for NO as well. This entails two-fold aspects: Firstly, this opens up unheralded regions of the effective neutrino mass to be probed by future 0νββ experiments. Secondly, this provides a way of testing the long-standing DLMA solution to 1 Combining KamLAND and neutrino neutral current scattering experiments like CHARM to lift this degeneracy has been discussed in [13].

arXiv:1901.04313v2 [hep-ph] 16 Dec 2019
the solar neutrino problem, irrespective of the value of the NSI parameters. Scattering experiments can also resolve this degeneracy by measuring the NSI parameters. For instance, in [18], combined constraints from neutrino oscillation and CHARM and NuTeV measurements were used to demonstrate that the degeneracy between the two LMA solutions can be resolved if NSI is only with the down quarks. Subsequently, the study performed in [19] included the COHERENT neutrinonucleus scattering data and showed that the DLMA solution can be disfavored at the 3.1σ and 3.6σ C.L. for NSI with up and down quarks, respectively. However, it is worth stressing that these bounds depend on the mass of the light mediator and it has been shown in [20] that the COHERENT data excludes the DLMA solution at 95% C.L. for light mediator mass > 48 MeV only. The global analysis including oscillation and CO-HERENT data performed in [21] shows that the DLMA solution is still allowed at 3σ, albeit for a smaller range of values of NSI parameters and for light mediators of mass > ∼ 10 MeV.
Although the importance of precision determination of θ 12 on the effective mass determined by 0νββ experiments have been highlighted earlier [22,23], the ramifications of the DLMA solution for 0νββ is being investigated in this work for the first time.
Predictions for 0νββ: The half-life for 0νββ process in the standard three generation picture is given as, where G contains the phase space factors, m e is the electron mass and M ν is the nuclear matrix element (NME). m ββ is the effective neutrino mass given by, U is the unitary PMNS mixing matrix for the three active neutrinos and is given in the standard parametrization as, where R ij are the three rotation matrices defined in terms of the corresponding mixing angles θ ij , with the Dirac CP-phase δ attached toR 13 , and the phase matrix P = diag (1, e iα2 , e i(α3+δ) ) contains the Majorana phases. In this letter, we denote the DLMA solution for θ 12 in the presence of NSI as θ D12 and the standard LMA solution as θ 12 . The 3σ ranges of these two parameters are given in Table I [21,24]. In this parametrization, the effective neutrino mass is, where c ij = cosθ ij and s ij = sinθ ij . |m ββ | depends on whether the neutrino mass states follow normal or inverted ordering or they are quasi-degenerate.
Normal ordering (NO) : m 1 < m 2 << m 3 with Inverted ordering (IO) : 3 ) for NO (IO). Fig. 1 shows m ββ as a function of the lightest neutrino mass for both NO and IO. The pink region is for NO with the standard solution for θ 12 and the red band is for NO with θ D12 , corresponding to the DLMA solution. The dark blue band is for IO with the standard θ 12 value and the cyan band (which overlaps with the blue band) is for IO with θ D12 . The gray band (0.071 − 0.161 eV) corresponds to the current upper limit from combined results of GERDA and KamLAND-Zen experiments. The region above this is disallowed. The range corresponds to the NME uncertainty [5,25,26]. The black dashed line represents the future 3σ sensitivity of the nEXO experiment : T 1/2 = 5.7 × 10 27 years [9], which, for the highest value of NME, translates to m ββ = 0.007 eV. This can probe a small part of the NO region with the LMA solution for m lightest > ∼ 0.005 eV, whereas the upper edge of the DLMA region can be probed even for small values of m lightest . The yellow region is disfavored by the cosmological constraints on the sum of the light neutrino masses [27]. In obtaining this plot, all the oscillation parameters are varied in their 3σ ranges [24] and the Majorana phases are varied from 0 to π.
From the figure, we can see that for NO, m ββ for the DLMA solution is higher than that for the standard LMA solution, shifting into the gap between IO and NO. The effect is more pronounced for lower values of m lightest . There is some overlap in the predictions between the maximum value of m ββ for the LMA with the minimum value of this for the DLMA solution, which increases as m lightest increases. One noteworthy feature is the absence of the cancellation region for the DLMA solution. For IO, the predicted values of m ββ remain the same for LMA and DLMA solutions. Since the predictions of m ββ for NO with LMA and IO with DLMA are well separated, the generalized hierarchy degeneracy [16] is not present.
The behavior of m ββ can be understood by considering the limiting cases for different mass schemes.
In this region, m ββ is independent of m 3 and is bounded from above and below by a maximum and minimum value given by [28], m ββ IOmax = |c 2 13 ∆m 2 atm | (α 2 = 0, π), m ββ IOmin = |c 2 13 cos2θ 12 ∆m 2 atm | (α 2 = π/2). The maximum value is independent of θ 12 while for the minimum value, we can see from Table I, that the 3σ range for |cos2θ 12 | is the same for both LMA and DLMA solutions. This explains why the prediction for m ββ is the same for both the cases in this region.  This is maximum for α 2 = α 3 = 0 and is again independent of θ 12 . Also, m ββ IO is minimum for α 2 = π/2 and α 3 = 0 or π/2 depending on whether we take θ 12 or θ D12 . But since, s 2 13 is very small, this is almost independent of what we choose for α 3 and effectively, the minimum of m ββ IO in this regime is approximated as, which is independent of the solution for θ 12 . Normal Ordering: Unlike in IO, the behavior of m ββ is different for the LMA as well as the DLMA solutions of θ 12 . For very small values of m 1 such that m 1 << m 2 ≈ ∆m 2 sol << m 3 ≈ ∆m 2 atm , m ββ can be written as, The maximum value of this corresponds to α 2 = α 3 = 0, π and the minimum value corresponds to α 2 = 0 and α 3 = π/2. These will be higher for higher values of sin 2 θ 12 . This explains why the prediction for m ββ for the DLMA solution in this region is higher.
Moving on to the cancellation region, the typical values of masses are m 1 ∼ 0.005 eV, m 2 ∼ 0.01 eV and m 3 ∼ 0.05 eV. Then, the minimum of m ββ (α 2 = α 3 = π/2) can be approximated as, For the values of s 2 12 and s 2 13 as listed in the Table I, complete cancellation is possible in the LMA region. However, for s 2 12 in the DLMA region, such a cancellation is not possible because of higher values of s 2 12 . As we increase the value of m 1 and reach the limit of partial hierarchy where m 1 ≈ m 2 ≈ ∆m 2 sol << m 3 ≈ ∆m 2 atm , the maximum value of m ββ is given by, which is independent of θ 12 . Hence the maximum values of m ββ for the two LMA solutions tend to overlap. In QD limit, m ββ varies linearly with the common mass scale m 0 and both maximum and minimum values are independent of θ 12 . At this point it is worthwhile to note that if we assume the existence of a fourth sterile neutrino as suggested by the LSND/MiniBooNE results, then even for NO the predicted m ββ can be in the desert region [29,30]. In fact, depending on the value of the mass squared difference governing the LSND/MiniBooNE oscillations, the prediction can even overlap with the IO prediction for three generation and hence, can be probed by the near future experiments.
Sensitivity in the future experiments : Here, we discuss a simple method to obtain the sensitivity of the DLMA region in the future 136 Xe experiments following the discussion in reference [8]. The discovery sensitivity is prescribed as the value of T 1/2 for which an experiment has a 50% probability of measuring a 3σ signal above the background. It is defined as, Here, N A is the Avogadro number, m a is the atomic mass of the isotope, B = β is the expected background where and The NME values [5,25] and the phase space factors [26] used in the calculation are also given.
β denote the sensitive exposure and background respectively ; S 3σ is the value for which half of the measurements would give a signal above B assuming a Poisson signal and is calculated from the relation C 3σ denotes the number of counts for which the cumulative Poisson distribution with mean B follows CDF P oisson (C 3σ |B) = 3σ. To avoid the discrete variations that would arise in the discovery sensitivity if C 3σ is restricted to be integer valued, we use the following definition of CDF P oisson as a continuous distribution in C using the normalized upper incomplete gamma function, CDF P oisson (C|µ) = Γ(C + 1, µ) Γ(C + 1) .
Using the above equations, the T 1/2 discovery sensitivities of 136 Xe as a function of for various values of β are shown in Fig. 2. In this plot, the red shaded band corresponds to the new allowed region of m ββ ∼ 0.004 − 0.0075 eV for the DLMA solution. This band in m ββ which is due to the variation of the parameters in the PMNS matrix, is converted to a band in T 1/2 using equation (1), by taking into account the NME uncertainty as given in Table II. The pink band corresponds to m ββ = 10 −3 eV, which is the minimum of the NO regime for lower values of m lightest with the LMA solution. In Fig. 2, the dotted black line corresponds to the future 3σ sensitivity of nEXO, which is T 1/2 = 5.7 × 10 27 years [9]. The yellow, black, brown and blue lines correspond to different values of the sensitive background levels of 0, 10 −5 , 10 −4 and 10 −3 cts/(kg iso yr) respectively. From the figure, we can see that for a sensitive background level of 10 −4 cts/(kg iso yr), the DLMA region could be probed with a sensitive exposure greater than ∼ 5000 kg iso yr. To probe the 10 −3 regime shown by the dashed lines requires lower background levels and/or higher sensitive exposure. In Table  II, we have given the T 1/2 ranges corresponding to the DLMA region, m ββ = 0.004−0.0075 eV for three different isotopes.
Conclusion : Searching for 0νββ process is of utmost importance since it can establish the Majorana nature of the neutrinos which implies they are their own antiparticles. This will in-turn signify a lepton number violating Majorana mass term for the neutrinos, which may hold the key in explaining why neutrino masses are much smaller than the other fermion masses. This can have profound implications for a deeper understanding of physics beyond the Standard Model of particle physics. So far these searches have yielded negative results and have put an upper bound on the effective mass governing 0νββ. Assuming light Majorana neutrino exchange as the sole mechanism for 0νββ, the predictions of effective mass for IO and NO are separated by a "desert region". The current upper bound is just above the IO region (∼ 0.1 eV ) and several future experiments with sensitivity reach ∼ 0.015 eV are expected to probe the IO parameter space completely. However if no positive signal is found in these searches then the projected sensitivity reach of these experiments are in the ballpark of 0.005 eV which can explore only a small part of the NO region for lightest neutrino mass > ∼ 0.005 eV [9]. The next frontier that is envisaged is ∼ 10 −3 eV [31]. In this letter, we show for the first time, that if the Dark-LMA solution to the solar neutrino problem is true, then the effective mass for NO shifts into the intermediate "desert zone" between NO and IO. Therefore, in an incremental advancement, a new goal for the 0νββ experiments can be to first explore this region ∼ 0.004 − 0.0075 eV, which is possible even for very low values of the lightest neutrino mass. This not only defines a newer sensitivity goal of future 0νββ experimental program for the NO scenario, but can also provide an independent confirmation/refutal of the Dark-LMA solution to the solar neutrino problem in presence of non-standard interactions.