Non-standard interactions in propagation at the Deep Underground Neutrino Experiment

Journal of High Energy Physics, Mar 2016

We study the sensitivity of current and future long-baseline neutrino oscillation experiments to the effects of dimension six operators affecting neutrino propagation through Earth, commonly referred to as Non-Standard Interactions (NSI). All relevant parameters entering the oscillation probabilities (standard and non-standard) are considered at once, in order to take into account possible cancellations and degeneracies between them. We find that the Deep Underground Neutrino Experiment will significantly improve over current constraints for most NSI parameters. Most notably, it will be able to rule out the so-called LMA-dark solution, still compatible with current oscillation data, and will be sensitive to off-diagonal NSI parameters at the level of ε ∼ \( \mathcal{O} \)(0.05 − 0.5). We also identify two degeneracies among standard and non-standard parameters, which could be partially resolved by combining T2HK and DUNE data.

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Non-standard interactions in propagation at the Deep Underground Neutrino Experiment

HJE Non-standard interactions in propagation at the Deep Underground Neutrino Experiment Pilar Coloma 0 1 0 P. O. Box 500, Batavia, IL 60510 , U.S.A 1 Theoretical Physics Department, Fermi National Accelerator Laboratory We study the sensitivity of current and future long-baseline neutrino oscillation experiments to the e ects of dimension six operators a ecting neutrino propagation through Earth, commonly referred to as Non-Standard Interactions (NSI). All relevant parameters entering the oscillation probabilities (standard and non-standard) are considered at once, in order to take into account possible cancellations and degeneracies between them. We nd that the Deep Underground Neutrino Experiment will signi cantly improve over current constraints for most NSI parameters. Most notably, it will be able to rule out the so-called LMA-dark solution, still compatible with current oscillation data, and will be sensitive to o -diagonal NSI parameters at the level of " Beyond Standard Model; Neutrino Physics; CP violation - Underground O(0:05 0:5). We also identify two degeneracies among standard and non-standard parameters, which could be partially resolved by combining T2HK and DUNE data. The formalism of NSI in propagation Simulation details Sampling of the parameter space Experimental setups 5 Conclusions A Implementation of prior constraints 1 Introduction 2 3 4 3.1 3.2 4.1 4.2 4.3 Results Expected sensitivities for the DUNE experiment Degeneracies Comparison to other facilities and to prior experimental constraints (LcL ~ )( ~yLL) ; where LL stands for the lepton doublet, ~ = i 2 , being the SM Higgs doublet, and is the scale of New Physics (NP) up to which the e ective theory is valid to. In eq. (1.1), cd=5 is a coe cient which depends on the high energy theory responsible for the e ective operator at low energies. Interestingly enough, the Weinberg operator is the only SM gauge invariant d = 5 operator which can be constructed within the SM particle content. Furthermore, it beautifully explains the smallness of neutrino masses with respect to the rest of fermions in the SM through the suppression with a scale of NP at high energies. When working in an e ective theory approach, however, an in nite tower of operators would in principle be expected to take place. The e ective Lagrangian at low energies would be expressed as: L e = LSM + cd=5 O d=5 + cd=6 take place via d = 6 four-fermion e ective operators,1 in a similar fashion as in the case of Fermi's theory of weak interactions. Four-fermion operators involving neutrino elds can be divided in two main categories: 1. Operators a ecting charged-current neutrino interactions. These include, for instance, operators in the form (l PL )(q P q0), where l stands for a charged lep ton, P stands for one of the chirality projectors PR;L 5), and are lepton 2. Operators a ecting neutral-current neutrino interactions. These are operators in the form ( PL )(f P f ). In this case, f stands for any SM fermion. Operators belonging to the rst type will a ect neutrino production and detection processes. For this type of NSI, near detectors exposed to a very intense neutrino beam would be desired, in combination with a near detector, in order to collect a large enough event sample [4]. Systematic uncertainties would play an important role in this case, since for neutrino beams produced from pion decay the ux cannot be computed precisely.2 For recent studies on the potential of neutrino oscillation experiments to study NSI a ecting neutrino production and detection, see e.g., refs. [7{12]. For operators a ecting neutral-current neutrino interactions the situation is very different since these can take place coherently, leading to an enhanced e ect. Therefore, longbaseline neutrino oscillation experiments, with L O(500 1000) km, could potentially place very strong constraints on NSI a ecting neutrino propagation. Moreover, unlike atmospheric neutrino oscillation experiments [13{16], at long-baseline beam experiments the beam is well-measured at a near detector, keeping systematic uncertainties under control. Future long-baseline facilities, combined with a dedicated short-baseline program [17{19] to determine neutrino cross sections precisely, expect to be able to bring systematic uncertainties down to the percent level. Therefore, they o er the ideal benchmark to constrain NSI in propagation. This will be the focus of the present work. As a benchmark setup, we consider the proposed Deep Underground Neutrino Experiment [20] (DUNE) and determine the bounds that it will be able to put on NSI a ecting neutrino propagation through matter. For comparison, we will also show the sensitivity reach for the current generation of long-baseline neutrino oscillation experiments, 1In principle, the largest e ects from NSI are expected to come from d = 6 operators since they appear at low order in the expansion. However, this is might not be always the case [2]. The situation might be 2A di erent situation would take place at beams produced from muon decay, such as Neutrino Factories or the more recently proposed nuSTORM facility. In this case, the ux uncertainties are expected to remain { 2 { i.e., T2K [21] and NOvA [22]. Finally, we will also compare its reach to a proposed future neutrino oscillation experiment with much larger statistics but a much shorter baseline, to illustrate the importance of the long-baseline over the size of the event sample collected. As an example, we will consider the reach of the T2HK experiment [23]. The impact of NSI in propagation at long-baseline experiments has been studied extensively in the literature, see refs. [24{32] for an incomplete list, or see refs. [33, 34] for recent reviews on the topic. In particular, the reach of the LBNE experiment (very similar to the DUNE setup considered in this work) was studied in ref. [35]. However, this study was performed under the assumption of a vanishing 13, and only one non-standard parameter was switched on at a time. In the current work, we will follow the same approach as in ref. [32]: all NSI parameters are included at once in the simulations, in order to explore possible correlations and degeneracies among them. As we will see, this will reveal two important degeneracies, potentially harmful for standard oscillation analyses. The recent determination of 13 also has important consequences for the sensitivity to NSI parameters. On one hand, the large value of 13 makes it possible for the interference terms between standard and non-standard contributions to the oscillation amplitudes to become relevant (see, e.g., ref. [36] for a recent discussion). In addition, the value of 13 has now been determined to an extremely good accuracy by reactor experiments [37{39], while the current generation of long-baseline facilities expects to signi cantly improve the precision on the atmospheric parameters in the upcoming years [40]. At the verge of the precision Era in neutrino experiments, it thus seems appropriate to reevaluate the sensitivity of current and future long-baseline experiments to NSI parameters and, in particular, of the DUNE proposal. The paper is structured as follows. In section 2 we introduce the NSI formalism; section 3 describes the simulation procedure and the more technical details of the experimental setups under study; section 4 summarizes our results, and we present our conclusions in section 5. Finally, appendix A contains some more technical details regarding the implementation of previous constraints on the oscillation parameters in our simulations. 2 The formalism of NSI in propagation NSI a ecting neutrino propagation (from here on, we will refer to them simply as NSI) take place through the following four-fermion e ective operators: LNSI = p contribution of a given operator with coe cient "fP , but only on their sum over avours and chirality. The e ects of these operators appear in the neutrino evolution equation, in { 3 { HJEP03(216) the avour basis,3 as: 0 B i d (2.2) where ij = (1=ne) Pf;P nf mi2j =2E, U is the lepton avor mixing matrix, A fP , with nf the f -type fermion number density and GF the Fermi coupling p 2 2GF ne and " constant. The three diagonal entries of the modi ed matter potential in eq. (2.2) are real parameters, while the o -diagonal parameters are generally complex. . the Hamiltonian. The three complex NSI parameters "e ; "e and " will be parametrized Due to the requirement of SM gauge invariance, in principle any operators responsible of neutrino NSI would be generated simultaneously with analogous operators involving charged leptons [2, 42{44]. Thus, the tight experimental constraints on charged lepton avor violating processes can be automatically applied to operators giving NSI, rendering the e ects unobservable at neutrino experiments. However, there are ways in which the charged lepton constraints can be avoided, e.g., if the NSI are generated through operators involving the Higgs, or from interactions with a new light gauge boson, see e.g., refs. [2, 42, 43, 45]. At this point, however, model dependence comes into play. In the present work, we will explore how much the current bounds can be improved from a direct measurement at neutrino oscillation experiments, without necessarily assuming the viability of a model which can lead to large observable e ects. Direct constraints on NSI can be derived either from4 scattering processes [43, 48{ 50] or from neutrino oscillation data [51{54]. Currently, the strongest bounds for NSI in propagation come from the global t to neutrino oscillation data in ref. [54]. At the 90% CL, most constraints on the e ective " parameters are around this is "~ee, for which only O(1) can be derived from current data. An important conclusion derived from the global ts performed in refs. [51{54] is the presence of strong degeneracies in the data. In presence of NSI in propagation, global analyses of neutrino oscillation data are fully compatible with two solutions: the LMA solution: the standard Large Mixing Angle (LMA) solution corresponds to mixing angles fully compatible with the results obtained from a global t to neutrino oscillation data in absence of NSI. The results are fully compatible with the hypothesis 3If production or detection NSI were present, though, the e ective production and detection avour eigenstates would not coincide with the standard avour ones [41]. However, for simplicity we will consider in this work that no signi cant NSI a ecting production or detection are present. 4Stronger limits can be derived from mono-jet and multi-lepton constraints at colliders [46, 47]. However, these bounds are somewhat model-dependent and, in particular, fade away for models where the NSI come from interactions via a new light mediator. { 4 { of no NSI. There is a slight preference for a non-zero value of "~ee in the t, which arises from the non-observation of the up-turn in the solar neutrino transition probability. the LMA-dark solution: this solution is obtained for "~ee 3. In this case, all the oscillation parameters remain essentially unchanged, except for 12 which now lies in the higher octant [51]. It should be stressed that this solution is fully compatible with all current oscillation data, and there is no signi cant tension in the t. In this work, we will consider that both solutions are equally viable, and will be considered literature. Perturbative expansions of the relevant oscillation probabilities to this work can be found, for instance, in ref. [25, 32, 55]. The main impact of NSI on the probabilities can be summarized as follows: The major impact on the ! e and ! e oscillation probabilities is expected to come from the " e and " e parameters, as well as from "~ee. The dependence with " e and " e appears at the same order in the perturbative expansion, and therefore non-trivial correlations are expected to take place between them. The dependence with the CP-violating phases ( , e and e) is also expected to be non-trivial. On the other hand, the disappearance channels ! and ! are mainly a ected by the presence of "~ and " . The dependence of the oscillation probability on these parameters will be brie y discussed in section 4.2. Before nalizing this section it should be mentioned that, in the event of sizable NSI e ects in propagation, the currently measured values of the oscillation parameters may be a ected. In our simulations, we leave the atmospheric parameters free within their current experimental priors, and all parameters (standard and non-standard) will be tted simultaneously. However, some comments are in order. Firstly, the measured value of 13 observed at the Daya Bay experiment is not expected to be signi cantly a ected, due to the short baseline and low neutrino energies involved. It can thus be considered as precise input for the long-baseline analyses. A di erent situation may take place for the atmospheric mixing angle 23, though, since its determination comes mainly from atmospheric and long-baseline experiments, where NSI could be sizable. Nevertheless, in refs. [53, 54] it was found that the determination of the atmospheric parameters is not signi cantly a ected by the addition of a generalized matter potential. Finally, long-baseline experiments are not very sensitive to the solar parameters, and in this case they have to rely in previous measurements. We will consider the input values and priors at 1 from ref. [54], where the allowed con dence regions were obtained under the assumption of a generalized matter potential with NSI e ects. { 5 { 3.1 Sampling of the parameter space In our simulations, all relevant standard and non-standard parameters are marginalized over. This amounts to a total of fourteen parameters: six standard oscillation parameters (the three mixing angles, the CP-violating phase and the two mass splittings), ve moduli for the non-standard parameters ("~ee; "~ ; j" ej; j" ej and j" j) and three non-standard CP-violating phases ( e ; e and ). In order to sample all parameters e ciently, a Monte Carlo Markov Chain (MCMC) algorithm is used. The Monte Carlo Utility Based Experiment Simulator (MonteCUBES) C library [ 58 ] has been used to incorporate MCMC sampling into the General Long Baseline Experiment Simulator (GLoBES) [59, 60]. For the implementation of the NSI probabilities in matter, we use the non-Standard Interaction Event Generator Engine (nSIEGE), distributed along with the MonteCUBES package. Parameter estimation through MCMC methods is based on Bayesian inference. The aim is to determine the probability distribution function of the di erent model parameters given some data set d, i.e., the posterior probability P ( j d): P = P ( j d) = L(d j )P ( ) : P (d) (3.1) where L(d j ) is the likelihood, i.e., the probability of observing the data set d given a certain set of values for the parameters , and P (d) is the total probability of measuring the data set d and can be regarded as a normalization constant. The prior P ( ) is the probability that the parameters assume the value regardless of the data d, that is, our prior knowledge of the parameters. For the standard parameters, the assumed priors are taken to be gaussian, and in agreement with the current experimental uncertainties (see the pro les shown for the NSI with up quarks in gure 6 in ref. [54], rescaled accordingly as " 3 "u , see ref. [54] for details. At least 50 MCMC chains have been used in all our simulations, and the number of distinct samples after combination always exceeds 106. The convergence of the whole sample improves as R ! 1, with R being the ratio between the variance in the complete sample and the variance for each chain. We have checked that, for most of the parameters the convergence of the whole sample is much better than R 1 = 5 10 3, and in all cases is better than 10 2. More technical details related to the sampling of the parameter space can be found in appendix A. 3.2 Experimental setups In this work we have considered several facilities among the current and future generation of neutrino oscillation experiments: DUNE. We consider a 40 kton ducial liquid argon detector placed at 1300 km from the source, on-axis with respect to the beam direction. The neutrino beam con guration considered in this work corresponds to the 80 GeV con guration from ref. [62], with { 6 { HJEP03(216) a beam power of 1.08 MW. The detector performance has been simulated following ref. [62], with migration matrices for neutral current backgrounds from ref. [63]. Three years of running time are assumed in both neutrino and antineutrino modes. Systematic uncertainties of 2% and 5% are assumed for the signal and background rates, respectively. NOvA. The NOvA experiment has a baseline of 810 km, and the detector is exposed to an o -axis (0:8 ) neutrino beam produced from 120 GeV protons at Fermilab. The implementation of the NOvA experiment follows refs. [22, 64]. The ducial mass of the detector is 14 kton, and 6:0 1020 protons on target (PoT)/year are assumed. Again, a running time of 3 years in both neutrino and antineutrino modes is considered. T2K+NOvA. In this case, the expected results for the T2K experiment after 30 PoT in neutrino mode5 are added to the NO A results. The Super-KamiokaNDE detector is placed o -axis (2:5 ) with respect to the beam direction at L = 295 km, and has a ducial mass of 22.5 kton. The neutrino uxes have been taken from ref. [65]. The signal and background rejection e ciencies have been set to match the event rates and sensitivities from ref. [21] for the same exposure, and rescaled up to the larger statistics considered here. Given the much larger uncertainties in antineutrino mode, only neutrino data is considered for T2K. T2HK. The T2HK experiment is a proposed upgrade for the T2K experiment, with a much larger detector (560 kton ducial mass) located at the same o -axis angle and at the same distance as for the T2K experiment [23]. In this case, the signal and background rejection e ciencies have been taken as in ref. [66]. The number of events as well as the physics performance is consistent with the values reported in tables VIII and IX in ref. [67]. These correspond to 3(7) years of data taking in (anti)neutrino mode with a beam power of 750 MW. Systematic uncertainties of 5% and 10% are assumed for the signal and background rates, respectively. For all the setups simulated in this work, systematic uncertainties are taken to be correlated among all contributions to the signal and background event rates, but uncorrelated between di erent oscillation channels. In principle, a more detailed systematics implementation should be performed, taking into account the possible impact of a near detector, correlations between systematics a ecting di erent channels, etc. However, a careful implementation of systematic errors would add a large number of nuisance parameters to the problem, which would have to be marginalized over during the simulations. This would considerably complicate the problem, and is beyond the scope of the present work. For reference, the total expected event rates for the four experiments considered in this work are summarized in table 1. The true values assumed for the oscillation parameters are in good agreement with the best- t values from ref. [ 56 ]: 12 = 33:5 , sin2 2 13 = 0:085, 23 = 42 , = study the sensitivities of neutrino oscillation experiments to the NSI parameters, their true 5This corresponds to roughly ve times the PoT accumulated by the beginning of 2015 [21]. { 7 { ! e ! e ! (unosc.) DUNE NO A T2K 1136/287 111/232 82/28 95/23 12/17 {/{ T2HK considered in this work. The rates for the appearance channels are provided for the oscillation parameters assumed in our simulations (under the assumption of no NSI), while for the disappearance channels we provide the number of unoscillated events. Signal and background rejection e ciencies have been taken into account in all cases. values are set to zero in all cases. The matter density is xed to the value given by the Preliminary Reference Earth Model [68]. We have checked that allowing it to vary within a 2% range does not signi cantly a ect our nal sensitivities to NSI parameters, while it slowed down the simulations. 4 Results This section summarizes the results obtained for the expected sensitivities to NSI in propagation for the setups considered in this work. We will rst summarize the expected results for the DUNE experiment in more detail in section 4.1; a discussion of the degeneracies found among standard and non-standard parameters will be performed in section 4.2; nally, a comparison to the expected results from T2K, NOvA and from the T2HK experiment will then be performed in section 4.3. Our results will be presented in terms of credible intervals, or credible regions, which are obtained as follows. The total sample of points collected during the MCMC is projected onto a particular plane in the parameter space. After projection, the regions containing a given percentage (68%, 90% and 95%, in this work) of the distinct samples are identi ed. 4.1 Expected sensitivities for the DUNE experiment The DUNE sensitivities to NSI parameters are summarized in gure 1. The gure shows one- and two-dimensional projections of the MCMC results onto several planes. The parameters used in the projections are indicated in the left and low edge of the collection of panels. In the one-dimensional distributions, the vertical band indicates the credible interval at 68% level, while the dashed line shows the value which maximizes the posterior probability. In the two-dimensional projections, the red, green and blue lines show the 68%, 90% and 95% credible regions. In our simulations, all standard and non-standard parameters are left free and marginalized over. Similar projections for the standard oscillation parameters can be found in appendix A, see gure 7. { 8 { The vertical green bands indicate the credible intervals at 68%. Several features can be observed from gure 1. Most notably, two important degeneracies appear in the sensitivities: the rst a ects the determination of "~ , while the second degeneracy is observed in the "~ee " e plane. We will discuss these degeneracies in more detail in section 4.2. A second important conclusion that can be derived from gure 1 is that DUNE will already be able to explore the LMA dark solution at more than 90% CL. This can be observed in the leftmost column in gure 1, where the range of values of "~ee compatible with the LMA-dark solution are disfavoured at more than 90%. We will return to this point again in section 4.2. When considering operators which are not diagonal in avor space, it is important to bear in mind that they may be accompanied by new sources of CP-violation. The presence of such new phases may considerably a ect our sensitivity to the moduli of the { 9 { Φ -50 -100 planes. Dashed green lines indicate the results when no prior constraints are included on the NSI parameters, while solid blue lines indicate the results after imposing prior constraints on the NSI parameters. For reference, the vertical lines indicate prior constraints (at 90% CL, 1 d.o.f.) as extracted from ref. [54]. NSI parameters, due to destructive and constructive interference e ects. For this reason, we show in gure 2 the two-dimensional projections for the expected credible regions but in this time after projecting the MCMC results on the j" j planes. As can be seen from the gure, the e ect is rather large for the three operators considered, and the bounds are modi ed by a factor of between two and three in all cases. The dependence with the CP-phases is also di erent depending on the parameter under study. The case where the dependence of the sensitivity with the CP phase is most notable is the case of " . In this case, the sensitivity for values of close to =2 can be up to a factor of three worse than the sensitivity around CP-conserving values. While in the former case the sensitivity would not be able to improve over current constraints, in the latter case DUNE would be able to improve over current constraints by a factor of two. The dependence with can be well understood from the leading order expansion of the disappearance channel [25, 32, 55]: P = P std Ref" g (AL) sin ( 31L) + O("2) ; (4.1) p where A 2 2GF ne stands for the standard matter potential, ij = ( mi2j =2E), and P std is the oscillation probability in absence of NSI. Additional terms, which depend on both the real and imaginary parts of " , enter the probability at second order in the perturbative expansion, and provide some sensitivity in the regions with =2. At second order, the probability P also depends on "~ , and will be further discussed in section 4.2. The situation is a bit more convoluted for " e and " e due to their combined e ect on the appearance oscillation probabilities, see for instance ref. [55]. In the case of " e, we nd that DUNE will improve over current constraints regardless of the value of its associated CP-phase. The sensitivity changes by a factor of 2 depending on the value of e, and uctuates between 0.05 and 0.1. The results for " e also show a sizable dependence with the value of e. However, in this case the prior constraints play a very relevant role, as can be seen from the comparison between the dashed green and solid blue lines in the panel for " e in gure 2. Whereas before imposing prior constraints on the NSI parameters negative values of e are perfectly allowed in the t, once the prior constraints on NSI are imposed this is no longer the case. This has important consequences in the analysis, and implies that DUNE will be sensitive to values of " e down to 0.05 for values of e =2. The reason for this is as follows. As it was shown in gure 1, DUNE is insensitive to large values of "~ee and j" ej as long as their moduli lie along the two lines identi ed in gure 1 (see the projected allowed regions in the "~ee " e plane). For negative values of "~ee, the degeneracy condition can only be satis ed for values of e =2, as we will discuss in more detail in section 4.2. However, prior constraints on NSI rule out a large fraction of the parameter space for "~ee 2 ( 2; 0). Therefore, once these are included in the t, the degeneracy condition can no longer be satis ed, which is translated into an increased sensitivity at DUNE for " e, at the level of 0.05 for e . Finally, it is important to keep in mind that the new CP-violating phases could have an impact on standard CP-violating searches, see for instance ref. [32] for a study in the context of Neutrino Factories, or ref. [69] for a pseudo-analytical study at DUNE. This will be further discussed in section 4.2. 4.2 Degeneracies When studying the sensitivity of DUNE to NSI, we have identi ed two important degeneracies between both standard and non-standard parameters. The rst one has been previously reported in the literature (see, e.g., refs. [32, 55, 70, 71]), and takes place between the parameters "~ and 23 23 =4. This degeneracy can be understood analytically at the level of the oscillation probabilities. As already mentioned in section 2, the sensitivity to the "~ parameter comes from the and disappearance channels. A perturbative oscillation probability on 23, " where A stands for the standard matter potential, ij = ( mi2j =2E), and P std is the oscillation probability in absence of NSI. Note the di erent combination of oscillatory L L 50 DUNE+T2HK NSI w priors NSI no priors NSI w priors Θ45 40 combination with T2HK data. Three cases are shown for DUNE: the standard case when no NSI are allowed in the t, a case where marginalization is performed over NSI parameters within previous constraints, and a case where no previous constraints are assumed over NSI during the t. The combination with T2HK data is only shown in the case where prior NSI constraints are imposed in the t. Right: same results, projected in the 23 "~ plane. The dot indicates the true input values considered. phases in the terms in eq. (4.2). The second term in principle should be subleading with respect to the rst term, since it depends quadratically on a combination of 23 ( 0:05, in our case) and ", as opposed to the rst term which is linear. However, for energies matching the oscillation peak, the rst term will be strongly suppressed with the oscillatory phase. Due to the simultaneous dependence of P on 23 and "~ , a degeneracy appears in this plane. In fact, while in the standard scenario the DUNE experiment is able to successfully resolve the octant of 23 (see gure 8 in appendix A), when NSI are marginalized over in the t this is no longer the case, and the fake solution in the higher octant reappears. This is explicitly shown in gure 3. The left panel shows the results projected onto the 23 plane for three di erent scenarios: when no NSI are considered in the analysis (solid yellow), when NSI are marginalized over within current priors (dashed green) and when NSI are marginalized over with no priors on the NSI parameters (dotted blue). As it can be seen from the gure, the higher octant solution is not allowed by the data when NSI are not included in the t, but reappears if they are marginalized over (see also gures 7 and 8 in appendix A). The reason is that there is a strong degeneracy between "~ and 23, explicitly shown in the right panel. In the case where no prior uncertainties are assumed for the NSI parameters (dotted blue line), two additional solutions appear around 23 = 45 . However, these take place for values of "~ in tension with current constraints, and are therefore partially removed when the prior on the " parameter is imposed (dashed green lines). Finally, we nd that when T2HK is added to the DUNE data the degeneracy is almost completely solved, as it is shown by the dot-dashed gray contours. 1.0 0.8 È 0.6 e Τ ¶ È DUNE - no priors DUNE - w priors T2HK+DUNE - w priors -2 -1 0 Ž ¶ ee L ° H e Τ Φ 100 50 0 -50 -100 -150 1 2 3 -3 -2 -1 1 2 3 0 Ž ¶ ee j" ej plane for DUNE and for DUNE+T2HK, as indicated in the legend. For DUNE we also show the resulting region when no prior uncertainties are imposed on NSI during the t. In all cases, the contours enclose the 90% credible regions. The second degeneracy we found in this study takes place between the CP violating phase , and the NSI parameters "~ee and " e (including its CP phase). In this case, due to the large values of "~ee involved, perturbation theory cannot be used to understand the interplay of parameters. The degeneracy is explicitly shown in gure 4, for DUNE and for DUNE+T2HK, in the planes "~ee j" ej (left panel) and "~ee e (right panel). As can be seen from this gure, there is a non-trivial dependence with the CP-violating phase which is responsible of this degeneracy: while for small values of "~ee all values of e equally probable, as the value of "~ee increases only certain values of e are possible (namely, a negative phase for "~ee < 0, while only positive phases are allowed if "~ee > 0). This also illustrates why in gure 2 the sensitivity to " e improves so dramatically in the region where e < 0. Again in this case, when T2HK is added to the DUNE data the degeneracy is again partially solved, although not completely, as can be seen from the solid contours in gure 4. The fact that this degeneracy depends on the value of e suggests that it might have a relevant impact on CP-violation searches. This is shown explicitly gure 5, where the oscillation probabilities are shown for the ! e and ! oscillation channels at L = 1300 km as a function of the neutrino energy, for three di erent cases. The solid blue lines show the probabilities in the standard case, with true values of the oscillation parameters matching the best- t values from ref. [ 56 ] and = 90 . The dashed red line, on the other hand, shows the probabilities for "~ee = 2 and " e = 0:45, e = 150 , where the rest of the NSI parameters are taken to be zero and the standard ones are unchanged with respect to the standard scenario. Finally, the dotted green line shows the probabilities for "~ee = 1, " e = 0:25, = 90 . The three probabilities are identical, as can be seen from the gure, which could eventually lead to a misinterpretation of the data and a wrong determination of the value of . To the best HJEP03(216) 2 4 6 8 10 E HGeVL ! HJEP03(216) lation channels, under the assumption of standard oscillations only, and two di erent set of NSI parameters. Set (a) corresponds to "~ee = set (b) assumes "~ee = 1, j" ej = 0:25, 2 and j" ej = 0:45, e = of our knowledge, this degeneracy has not been studied previously in the literature.6 A detailed study would be needed to address its impact on CP violation searches at DUNE. This remains beyond the scope of this work and is left for future studies. 4.3 Comparison to other facilities and to prior experimental constraints It is interesting to compare the DUNE sensitivities to current constraints as well as to other oscillation experiments currently in operation (such as T2K and/or NOvA) or being planned for the future (such as T2HK). Our results from this comparison are presented in gure 6, where the colored bands indicate the credible intervals found at 90% found for each of the NSI parameters, either for the experiments alone or in combination with one another. Results are presented for the moduli of the di erent NSI parameters, after marginalization over the remaining oscillation parameters and the CP-phases. The results are compared to the constraints from previous experiments (see table 1 or gure 6 in ref. [54]), indicated by the dashed vertical lines. We have found that the combination of T2K and NOvA is not sensitive to NSI below the current constraints derived in ref. [54], due to the presence of strong degeneracies among di erent oscillation parameters, and therefore their results are not shown in this gure. The most important feature in gure 6 can be seen in the uppermost panel, where the sensitivity to "~ee is shown and compared to the currently allowed regions by global ts to neutrino oscillation data. As can be seen from this panel, under the assumption of no relevant NSI e ects in the oscillation probability, both DUNE and T2HK will be able to probe the LMA-dark solution. The possibility of ruling out the LMA-dark solution with long6The degeneracy in the "~ee " e plane shows similar features to the degeneracy studied in refs. [70{72]. Both degeneracies might be related but there are important di erences. While the degeneracy studied in refs. [70{72] appeared in the disappearance probabilities, our degeneracy takes place in the appearance channels instead and involves the new CP-phases. Furthermore, the relation between " e and "~ee is also di erent: while in our case the degeneracy imposes a linear relation between the two parameters, in refs. [70{ 72] the degeneracy took place along a parabola. This indicates that a possible way to break this degeneracy could be through combination with atmospheric neutrino data. baseline experiments was already pointed out previously in the literature. For instance, in ref. [45] it was found that NOvA could rule out this solution at approximately 85% CL. We nd, however, that the NOvA experiment on its own (or in combination with T2K) will not be able to rule out the LMA-dark solution. Due to the strong degeneracy between "~ee and " e (see section 4.2), it is always possible to reconcile the t and the simulated data by assuming simultaneously large values for "~ee and " e. This degeneracy is partially solved when prior constraints are imposed on " e; however, we nd that a small region of the parameter space around "~ee 3 and j" ej 0:45 still provides a good t to the data. Conversely, DUNE and/or T2HK will be sensitive enough to the presence of NSI in order to rule out the LMA-dark solution on their own. The rejection power is then increased if prior constraints on NSI parameters are included, as expected (dark bands in gure 6). According to our results, the DUNE experiment will also be able to improve current constraints on " e and " e by a factor of between 2 and 5, and at least by a factor of two with respect to the results expected at T2HK alone, as can be seen from the comparison of the light colored bands. In the case of " , the sensitivity when no prior is imposed goes above the current experimental constraint, indicating that the sensitivity to this parameter is somewhat limited. However, as it was shown in gure 2, the sensitivity to this parameter depends strongly on the value of its CP-violating phase, and DUNE is expected to improve over the current limit as long as 6 = =2, see gure 2. Finally, it is worth pointing out that, on its own, DUNE will not be able to improve over current constraints for "~ , for the set of true oscillation parameters assumed in this work. In this case, combination with T2HK would be essential. As can be seen from the second panel in gure 6, before combination none of the two experiments is able to improve over current experimental constraints, although they favour di erent regions in the parameter space. Thus, after combination, the sensitivity to "~ is notably improved, yielding a slightly better result than the ones from current limits. 5 Conclusions Neutrino physics is entering the precision Era. After the discovery of the third mixing angle in the leptonic mixing matrix, and in view of the precision measurements performed by the reactor experiments (most notably, Daya Bay) and long-baseline experiments (MINOS, T2K and, in the near future, NO A), it appears timely to reevaluate the sensitivity of current and future oscillation experiments to possible Non-Standard neutrino Interactions (NSI). We have focused on the impact of NSI on neutrinos in propagation through matter, something for which the planned Deep Underground Neutrino Experiment (DUNE) is very well suited for, due to its relatively high energies and very long baseline. Given the current experimental and theoretical e ort to keep systematic uncertainties below the 2%-5% level, it o ers a very well-suited environment to conduct New Physics searches. In this work, a Monte Carlo Markov Chain (MCMC) has been used to explore the multidimensional parameter space surrounding the global minimum of the 2. The total number of parameters which are allowed to vary in the t is fourteen: six standard oscillation parameters, ve moduli for the non-standard parameters, and three new CP-violating phases. Prior experimental constraints, completely model-independent, have been implemented in Credible Intervals at 90% rak d T2HK+DUNE A A M M L L -4 -3 -2 1 2 3 Credible Intervals at 90% -0.6 -0.4 -0.2 ¶ΜΜ T2HK+DUNE ¶ΜΤ and after combining their respective data sets. Darker (Lighter) bands show the results when priors constraints on NSI parameters are (not) included in the t. The vertical gray areas bounded by the dashed lines indicate the allowed regions at 90% CL (taken from the SNO-DATA lines for f=u in ref. [54]). DUNE with no priors on NSI DUNE with priors Current constraint "~ee "~ j" ej j" ej j " j cients accompanying the NSI four-fermion operators a ecting neutrino propagation in matter. The rede nition "~ " " has been used, see section 2 for details. For comparison, the last column shows the current constraints at 90% CL extracted from a global t to neutrino oscillation data (taken from the SNO-DATA lines for f=u in ref. [54]). our simulations, see section 3.1 and appendix A for details. By including all (standard and non-standard) parameters at once in the simulation, we derive conservative and completely model-independent limits on each of the coe cients accompanying the new operators entering the e ective operator expansion. At the same time, we fully take into account possible degeneracies among di erent parameters entering the oscillation probabilities. We have identi ed two potentially important degeneracies among standard and nonstandard parameters. The rst one takes place in the disappearance channels between 23 and "~ , and could be potentially harmful for the octant sensitivity of the DUNE experiment. While in the standard case we nd that the DUNE experiment is able to reject the higher octant solution, this is no longer the case if the "~ parameter is marginalized over during the t. The second degeneracy takes place between "~ee, " e, e and in the appearance channels. The interplay between the di erent parameters in this case is nontrivial and it involves one of the non-standard CP-violating phases, e. This degeneracy could potentially pose a challenge for standard CP-violating searches and a more careful study will be left for future work. One of the most relevant results shown in the present study is that the DUNE experiment will be able to probe the so-called LMA-dark solution. The LMA-dark solution, which is fully compatible with current oscillation data [54], favors a large non-standard matter potential driven by "~ee 3 and a solar mixing angle in the second octant, 12 > =4. We nd that, for the true oscillation parameters assumed in this work, the credible regions at 90% do not include the LMA-dark region, see gures 4 and 6. We nd that DUNE will be able to improve over current constraints on " e by at least a factor of ve, and on " e by at least a 20%. The sensitivity to " e shows a signi cant (and non-trivial) dependence with the value of its associated CP-phase and, in particular, is HJEP03(216) signi cantly a ected by the current prior on "~ee (see gures 4 and 2). Regarding " , DUNE will be able to improve over current constraints as long as =2, see gure 2. Finally, we nd that DUNE will not be able to improve over current constraints on "~ , for the set of 6 = true oscillation parameters assumed in this work. For convenience, the expected sensitivity of DUNE to NSI parameters is summarized in table 2, where the credible intervals are given at 90%. Finally, we have also compared the expected reach for the DUNE experiment to that of the current generation of long-baseline experiments and to the future T2HK proposal. We found that the combination of T2K and NOvA will not be sensitive enough to the presence of NSI in order to improve over current constraints from oscillation data. The T2HK experiment on its own will not be able to improve over current constraints either for most parameters, with the exception of " e. Interestingly enough, we nd that the combination of T2HK and DUNE is able to partially resolve the degeneracies discussed in section 4.2. In particular, the combination of DUNE and T2HK would yield a strong improvement in the determination of "~ and solve almost completely the degeneracy between "~ and 23, see gure 3. Note added: the preprint version of ref. [73] was made available online two days before the present manuscript. In ref. [73], a very similar analysis was performed for non-standard interactions in propagation at DUNE. Acknowledgments I am especially grateful to Enrique Fernandez-Martinez for support regarding the use of the MonteCUBES software as well as for useful discussions and comments on the manuscript. I would like to thank Jacobo Lopez-Pavon and Stephen Parke for useful comments on the manuscript, and Alexander Friedland, Andre de Gouvea and Thomas Schwetz for useful discussions. I would also like to thank David Vanegas Forero for his help in writing the T2K les with the 2013 uxes, and Michele Maltoni for useful communications regarding the prior constraints on NSI coming from current oscillation data. I acknowledge partial support by the European Union through the ITN INVISIBLES (Marie Curie Actions, PITN-GA-2011-289442- INVISIBLES). Fermilab is operated by the Fermi Research Alliance under contract DE-AC02-07CH11359 with the U.S. Department of Energy. A Implementation of prior constraints In order to restrict the region sampled by the MCMC to the physical region of interest, priors have been implemented for all parameters (standard and non-standard) in our simulations, with the only exception of the standard CP-violating phase , since current hints only have a limited statistical signi cance at the 1 2 CL (see, however, refs. [ 56, 74 ] for recent discussions on this topic). Since the measurements on 13 and 23 do not come from a direct measurement of the angles themselves, these priors have been implemented according to the quantities that are directly measured at oscillation experiments. For 13 this amount to imposing a gaussian prior on sin2 2 13. In the case of 23, however, the situation is a bit more complicated. The most precise determination of 23 comes from the observation of disappearance at long-baseline experiments, which measure an \effective" mixing angle sin2 2 , see e.g., refs. [75, 76]. Given the large value of 13, the Prior (at 68%) 0.02 3% 3% agreement with the current uncertainties from ref. [ 56 ], except for sin2 2 23 for which the prior has been relaxed by a factor of two. correspondence $ 23 no longer takes place. Instead, the following relation holds: sin = sin 23 cos 13 : (A.1) HJEP03(216) Therefore, a gaussian prior a ecting 23 has been implemented on this e ective angle instead, since this is the quantity which is actually constrained by long-baseline experiments. The DUNE experiment will provide the most precise determination of this parameter, though. Therefore, in this case only a mild prior has been imposed, relaxing the current constraints by a factor of two, in order to ease convergence of the simulations. Finally, for the solar mixing angle we have implemented a gaussian prior on sin2 2 12 since, in practice, this is the only quantity that can be determined from current oscillation data. Table 3 summarizes the priors implemented for the standard oscillation parameters, which are assumed to be gaussian. For the NSI parameters, we have implemented non-gaussian priors, extracted from the results for SNO-DATA lines from gure 6 in ref. [54], for f=u. These have been rescaled according to the relation " = 3:051"u . We have considered that both the LMA and LMA-dark solutions are equally allowed by the data. Finally, a typical problem usually encountered when a multi-dimensional parameter space is explored using a MCMC has to do with the existence of multiple minima. If the 2 between di erent minima is large enough, the MCMC will generally tend to sample only one of them, leaving the rest unexplored. This is specially relevant in neutrino oscillations, where degeneracies are expected to arise between di erent parameters, even in absence of NSI [78{81]. This problem is dealt with in our simulations by the use of \degeneracy steps", chosen speci cally to make sure that all possible degeneracies are explored by the MCMC. For example, since a non-maximal value of 23 has been considered in our simulations, an obvious choice in this case is to add a larger step in the 23 direction so as to guarantee that the octant degeneracy is appropriately sampled. Additional steps in the " directions have also been set up in order to guarantee that all possible degenerate solutions are found in the simulations (for instance, in order to guarantee that the LMA-dark solution is appropriately sampled, we have added a step in the "~ee direction with "~ee = 4). Figure 7 shows explicitly that the octant degeneracies are well sampled in our simulations. This gure shows the same type of one- and two-dimensional projections of the MCMC results as in gure 1, for the standard oscillation parameters,7 assuming no priors over the NSI parameters. As it can be clearly seen from this gure, the octant degeneracy 7Long-baseline experiments are not sensitive to the solar parameters and therefore their measurement is not expected to improve over the assumed priors. For this reason we only show the projections for 13; 23; m321 and . Nevertheless, solar parameters are always left free during marginalization, within the assumed priors listed in table 3. 23 0.8 2.48 δ 2 2 for the standard oscillation parameters, after marginalizing over all NSI parameters. No prior constraints on NSI parameters are have been imposed. The red, green and blue lines indicate the credible regions at 68%, 90% and 95%. The vertical green bands indicate the credible intervals at 68%. in the 23 axis has been properly sampled by our MCMC, and three well separated regions are obtained. For comparison, gure 7 shows the same projections when no NSI are allowed in the t (i.e., only standard parameters are allowed in the t). In this case, the octant degeneracies disappear, in agreement with the results in previous literature (see, e.g., refs. [35, 82]). Finally, it should be mentioned that the T2HK experiment [23] is not sensitive to the neutrino mass ordering at high con dence level for all possible values of the CP-violating phase and all values of the atmospheric mixing angle. Therefore, degeneracies in the m231 direction are expected to take place, and should be explored as well. Nevertheless, the determination of the mass ordering might come instead from a combination of di erent facilities [83{89], from atmospheric data at HK [23], or from the combination of T2K+NO A at some level, if the current hint for =2 persists in the future. Therefore, we will adopt an optimistic approach in this paper and assume that the neutrino mass ordering is determined by the time these experiments nish taking data. Normal ordering has been assumed in all our simulations. 0.85 δ This article is distributed under the terms of the Creative Commons Attribution License (CC-BY 4.0), which permits any use, distribution and reproduction in any medium, provided the original author(s) and source are credited. [INSPIRE]. JHEP 09 (2009) 038 [arXiv:0906.1461] [INSPIRE]. [4] R. Alonso et al., Summary report of MINSIS workshop in Madrid, arXiv:1009.0476 [5] nuSTORM collaboration, D. Adey et al., nuSTORM | neutrinos from STORed Muons: proposal to the Fermilab PAC, arXiv:1308.6822 [INSPIRE]. [6] ISS Physics Working Group collaboration, A. Bandyopadhyay, Physics at a future neutrino factory and super-beam facility, Rept. Prog. Phys. 72 (2009) 106201 [arXiv:1305.4350] [INSPIRE]. [arXiv:1310.5917] [INSPIRE]. [9] I. Girardi, D. Meloni and S.T. Petcov, The Daya Bay and T2K results on sin2 2 13 and non-standard neutrino interactions, Nucl. Phys. B 886 (2014) 31 [arXiv:1405.0416] reactor neutrino experiments, J. Phys. G 42 (2015) 065003 [arXiv:1411.5330] [INSPIRE]. [11] S.K. Agarwalla, P. Bagchi, D.V. Forero and M. Tortola, Probing non-standard interactions at Daya Bay, JHEP 07 (2015) 060 [arXiv:1412.1064] [INSPIRE]. [12] M. Blennow, S. Choubey, T. Ohlsson and S.K. Raut, Exploring source and detector non-standard neutrino interactions at ESS SB, JHEP 09 (2015) 096 [arXiv:1507.02868] [13] S. Choubey, A. Ghosh, T. Ohlsson and D. Tiwari, Neutrino physics with non-standard interactions at INO, JHEP 12 (2015) 126 [arXiv:1507.02211] [INSPIRE]. [14] S. Choubey and T. Ohlsson, Bounds on non-standard neutrino interactions using PINGU, Phys. Lett. B 739 (2014) 357 [arXiv:1410.0410] [INSPIRE]. [15] T. Ohlsson, H. Zhang and S. Zhou, E ects of nonstandard neutrino interactions at PINGU, Phys. Rev. D 88 (2013) 013001 [arXiv:1303.6130] [INSPIRE]. [16] I. Mocioiu and W. Wright, Non-standard neutrino interactions in the mu-tau sector, Nucl. Phys. B 893 (2015) 376 [arXiv:1410.6193] [INSPIRE]. [17] CAPTAIN collaboration, H. Berns et al., The CAPTAIN detector and physics program, in Community summer study 2013: Snowmass on the Mississippi (CSS2013), Minneapolis MN U.S.A. July 29{August 6 2013 [arXiv:1309.1740] [INSPIRE]. [18] MINER A collaboration, L. Fields, CCQE results from MINER A, AIP Conf. Proc. 1663 (2015) 080006 [INSPIRE]. [19] ArgoNeuT and MicroBooNE collaborations, A.M. Szelc, Recent results from ArgoNeuT and status of MicroBooNE, Nucl. Part. Phys. Proc. 265-266 (2015) 208 [INSPIRE]. [20] DUNE collaboration, R. Acciarri et al., Long-Baseline Neutrino Facility (LBNF) and Deep Underground Neutrino Experiment (DUNE) conceptual design report volume 2: the physics program for DUNE at LBNF, arXiv:1512.06148 [INSPIRE]. [21] T2K collaboration, K. Abe et al., Measurements of neutrino oscillation in appearance and disappearance channels by the T2K experiment with 6:6 D 91 (2015) 072010 [arXiv:1502.01550] [INSPIRE]. 1020 protons on target, Phys. Rev. arXiv:1209.0716 [INSPIRE]. long-baseline neutrino oscillation experiment using a J-PARC neutrino beam and [INSPIRE]. [INSPIRE]. [INSPIRE]. [24] P. Huber, T. Schwetz and J.W.F. Valle, Confusing nonstandard neutrino interactions with oscillations at a neutrino factory, Phys. Rev. D 66 (2002) 013006 [hep-ph/0202048] interactions, Phys. Rev. D 78 (2008) 053007 [arXiv:0804.2261] [INSPIRE]. [31] D. Meloni, T. Ohlsson, W. Winter and H. Zhang, Non-standard interactions versus non-unitary lepton avor mixing at a neutrino factory, JHEP 04 (2010) 041 [arXiv:0912.2735] [INSPIRE]. [INSPIRE]. 044201 [arXiv:1209.2710] [INSPIRE]. [32] P. Coloma, A. Donini, J. Lopez-Pavon and H. Minakata, Non-standard interactions at a neutrino factory: correlations and CP-violation, JHEP 08 (2011) 036 [arXiv:1105.5936] [34] O.G. Miranda and H. Nunokawa, Non standard neutrino interactions: current status and future prospects, New J. Phys. 17 (2015) 095002 [arXiv:1505.06254] [INSPIRE]. [35] P. Huber and J. Kopp, Two experiments for the price of one? The role of the second oscillation maximum in long baseline neutrino experiments, JHEP 03 (2011) 013 [Erratum ibid. 05 (2011) 024] [arXiv:1010.3706] [INSPIRE]. [36] A. Friedland and I.M. Shoemaker, Searching for novel neutrino interactions at NO A and beyond in light of large 13, arXiv:1207.6642 [INSPIRE]. [37] Daya Bay collaboration, F.P. An et al., Observation of electron-antineutrino disappearance at Daya Bay, Phys. Rev. Lett. 108 (2012) 171803 [arXiv:1203.1669] [INSPIRE]. [arXiv:1204.0626] [INSPIRE]. [39] Double CHOOZ collaboration, Y. Abe et al., Indication for the disappearance of reactor electron antineutrinos in the Double CHOOZ experiment, Phys. Rev. Lett. 108 (2012) 131801 [41] P. Langacker and D. London, Lepton number violation and massless nonorthogonal HJEP03(216) neutrinos, Phys. Rev. D 38 (1988) 907 [INSPIRE]. [42] Z. Berezhiani and A. Rossi, Limits on the nonstandard interactions of neutrinos from e+e colliders, Phys. Lett. B 535 (2002) 207 [hep-ph/0111137] [INSPIRE]. [43] S. Davidson, C. Pena-Garay, N. Rius and A. Santamaria, Present and future bounds on nonstandard neutrino interactions, JHEP 03 (2003) 011 [hep-ph/0302093] [INSPIRE]. [44] S. Antusch, J.P. Baumann and E. Fernandez-Martinez, Non-standard neutrino interactions with matter from physics beyond the standard model, Nucl. Phys. B 810 (2009) 369 [arXiv:0807.1003] [INSPIRE]. [45] Y. Farzan, A model for large non-standard interactions of neutrinos leading to the LMA-dark solution, Phys. Lett. B 748 (2015) 311 [arXiv:1505.06906] [INSPIRE]. [46] A. Friedland, M.L. Graesser, I.M. Shoemaker and L. Vecchi, Probing nonstandard standard model backgrounds with LHC monojets, Phys. Lett. B 714 (2012) 267 [arXiv:1111.5331] [47] D.B. Franzosi, M.T. Frandsen and I.M. Shoemaker, New or missing energy? Discriminating dark matter from neutrino interactions at the LHC, arXiv:1507.07574 [48] J. Barranco, O.G. Miranda, C.A. Moura and J.W.F. Valle, Constraining non-standard interactions in ee or ee scattering, Phys. Rev. D 73 (2006) 113001 [hep-ph/0512195] [49] C. Biggio, M. Blennow and E. Fernandez-Martinez, Loop bounds on non-standard neutrino interactions, JHEP 03 (2009) 139 [arXiv:0902.0607] [INSPIRE]. [50] C. Biggio, M. Blennow and E. Fernandez-Martinez, General bounds on non-standard neutrino interactions, JHEP 08 (2009) 090 [arXiv:0907.0097] [INSPIRE]. [51] O.G. Miranda, M.A. Tortola and J.W.F. Valle, Are solar neutrino oscillations robust?, JHEP 10 (2006) 008 [hep-ph/0406280] [INSPIRE]. [52] F.J. Escrihuela, O.G. Miranda, M.A. Tortola and J.W.F. Valle, Constraining nonstandard neutrino-quark interactions with solar, reactor and accelerator data, Phys. Rev. D 80 (2009) 105009 [Erratum ibid. D 80 (2009) 129908] [arXiv:0907.2630] [INSPIRE]. [53] M.C. Gonzalez-Garcia, M. Maltoni and J. Salvado, Testing matter e ects in propagation of atmospheric and long-baseline neutrinos, JHEP 05 (2011) 075 [arXiv:1103.4365] [INSPIRE]. [54] M.C. Gonzalez-Garcia and M. Maltoni, Determination of matter potential from global analysis of neutrino oscillation data, JHEP 09 (2013) 152 [arXiv:1307.3092] [INSPIRE]. [55] T. Kikuchi, H. Minakata and S. Uchinami, Perturbation theory of neutrino oscillation with nonstandard neutrino interactions, JHEP 03 (2009) 114 [arXiv:0809.3312] [INSPIRE]. MonteCUBES, Comput. Phys. Commun. 181 (2010) 227 [arXiv:0903.3985] [INSPIRE]. HJEP03(216) experiments with GLoBES (General Long Baseline Experiment Simulator), Comput. Phys. Commun. 167 (2005) 195 [hep-ph/0407333] [INSPIRE]. of neutrino oscillation experiments with GLoBES 3:0: General Long Baseline Experiment Simulator, Comput. Phys. Commun. 177 (2007) 432 [hep-ph/0701187] [INSPIRE]. [61] Super-Kamiokande collaboration, G. Mitsuka et al., Study of non-standard neutrino interactions with atmospheric neutrino data in Super-Kamiokande I and II, Phys. Rev. D 84 (2011) 113008 [arXiv:1109.1889] [INSPIRE]. [62] LBNF letter of intent, submitted to the Fermilab PAC P-1062, U.S.A. December 2014. [63] LBNE collaboration, T. Akiri et al., The 2010 interim report of the Long-Baseline Neutrino Experiment collaboration physics working groups, arXiv:1110.6249 [INSPIRE]. [64] M. Blennow, P. Coloma, A. Donini and E. Fernandez-Martinez, Gain fractions of future neutrino oscillation facilities over T2K and NO A, JHEP 07 (2013) 159 [arXiv:1303.0003] [INSPIRE]. [INSPIRE]. [65] T2K collaboration, K. Abe et al., T2K neutrino ux prediction, Phys. Rev. D 87 (2013) 012001 [Addendum ibid. D 87 (2013) 019902] [arXiv:1211.0469] [INSPIRE]. [66] P. Coloma, P. Huber, J. Kopp and W. Winter, Systematic uncertainties in long-baseline neutrino oscillations for large 13, Phys. Rev. D 87 (2013) 033004 [arXiv:1209.5973] [67] K. Abe et al., Letter of intent: the Hyper-Kamiokande experiment | detector design and physics potential, arXiv:1109.3262 [INSPIRE]. Interiors 25 (1981) 297 [INSPIRE]. [68] A.M. Dziewonski and D.L. Anderson, Preliminary reference earth model, Phys. Earth Planet. [69] M. Masud, A. Chatterjee and P. Mehta, Probing CP-violation signal at DUNE in presence of non-standard neutrino interactions, arXiv:1510.08261 [INSPIRE]. [70] A. Friedland, C. Lunardini and M. Maltoni, Atmospheric neutrinos as probes of neutrino-matter interactions, Phys. Rev. D 70 (2004) 111301 [hep-ph/0408264] [INSPIRE]. [71] A. Friedland and C. Lunardini, Two modes of searching for new neutrino interactions at MINOS, Phys. Rev. D 74 (2006) 033012 [hep-ph/0606101] [INSPIRE]. [72] A. Friedland and C. Lunardini, A test of tau neutrino interactions with atmospheric neutrinos and K2K, Phys. Rev. D 72 (2005) 053009 [hep-ph/0506143] [INSPIRE]. [73] A. de Gouv^ea and K.J. Kelly, Non-standard neutrino interactions at DUNE, arXiv:1511.05562 [INSPIRE]. 1350093 [arXiv:1209.5658] [INSPIRE]. [arXiv:1406.2551] [INSPIRE]. JHEP 10 (2001) 001 [hep-ph/0108085] [INSPIRE]. superbeams using liquid argon detectors, JHEP 03 (2014) 087 [arXiv:1304.3251] [INSPIRE]. [arXiv:1306.2500] [INSPIRE]. experiments: an `adequate' con guration for LBNO, JHEP 03 (2014) 094 [arXiv:1308.5979] [INSPIRE]. PINGU and Daya Bay II, JHEP 09 (2013) 089 [arXiv:1306.3988] [INSPIRE]. T2K, NO A and reactor experiments, JHEP 04 (2013) 009 [arXiv:1212.1305] [INSPIRE]. [1] S. Weinberg , Baryon and lepton nonconserving processes , Phys. Rev. Lett . 43 ( 1979 ) 1566 [2] M.B. Gavela , D. Hernandez , T. Ota and W. Winter , Large gauge invariant non-standard neutrino interactions , Phys. Rev. D 79 ( 2009 ) 013007 [arXiv: 0809 .3451] [INSPIRE]. [3] M.B. Gavela , T. Hambye , D. Hernandez and P. Hernandez , Minimal avour seesaw models, [7] A.N. Khan , D.W. McKay and F. Tahir , Sensitivity of medium-baseline reactor neutrino mass-hierarchy experiments to nonstandard interactions , Phys. Rev. D 88 ( 2013 ) 113006 [8] T. Ohlsson , H. Zhang and S. Zhou , Nonstandard interaction e ects on neutrino parameters at medium-baseline reactor antineutrino experiments , Phys. Lett. B 728 ( 2014 ) 148 [22] NO A collaboration , R.B. Patterson , The NO A experiment: status and outlook , [ 23 ] Hyper-Kamiokande proto- collaboration, K. Abe et al., Physics potential of a Hyper-Kamiokande, Prog. Theor. Exp. Phys . 2015 ( 2015 ) 053C02 [arXiv: 1502 .05199] [25] J. Kopp , M. Lindner , T. Ota and J. Sato , Non-standard neutrino interactions in reactor and superbeam experiments , Phys. Rev. D 77 ( 2008 ) 013007 [arXiv: 0708 .0152] [INSPIRE]. [26] J. Kopp , P.A.N. Machado and S.J. Parke , Interpretation of MINOS data in terms of non-standard neutrino interactions , Phys. Rev. D 82 ( 2010 ) 113002 [arXiv: 1009 .0014] [27] J. Kopp , M. Lindner and T. Ota , Discovery reach for non-standard interactions in a neutrino factory , Phys. Rev. D 76 ( 2007 ) 013001 [ hep -ph/0702269] [INSPIRE]. [28] M. Blennow , T. Ohlsson and J. Skrotzki , E ects of non-standard interactions in the MINOS experiment , Phys. Lett. B 660 ( 2008 ) 522 [ hep -ph/0702059] [INSPIRE]. [29] M. Blennow , D. Meloni , T. Ohlsson , F. Terranova and M. Westerberg , Non-standard interactions using the OPERA experiment , Eur. Phys. J. C 56 ( 2008 ) 529 [30] J. Kopp , T. Ota and W. Winter , Neutrino factory optimization for non-standard [33] T. Ohlsson, Status of non-standard neutrino interactions , Rept. Prog. Phys . 76 ( 2013 ) disappearance in the RENO experiment , Phys. Rev. Lett . 108 ( 2012 ) 191802 experiment , Prog. Theor. Exp. Phys . 2015 ( 2015 ) 043C01 [arXiv: 1409 .7469] [INSPIRE]. [56] M.C. Gonzalez-Garcia , M. Maltoni and T. Schwetz , Updated t to three neutrino mixing: status of leptonic CP-violation , JHEP 11 ( 2014 ) 052 [arXiv: 1409 .5439] [INSPIRE]. [57] A. Friedland , C. Lunardini and C. Pena-Garay , Solar neutrinos as probes of neutrino matter interactions , Phys. Lett. B 594 ( 2004 ) 347 [ hep -ph/0402266] [INSPIRE]. [58] M. Blennow and E. Fernandez-Martinez , Neutrino oscillation parameter sampling with [59] P. Huber , M. Lindner and W. Winter , Simulation of long-baseline neutrino oscillation [60] P. Huber , J. Kopp , M. Lindner , M. Rolinec and W. Winter , New features in the simulation [74] J. Elevant and T. Schwetz , On the determination of the leptonic CP phase , JHEP 09 ( 2015 ) [75] S.K. Raut , E ect of non-zero 13 on the measurement of 23, Mod . Phys. Lett. A 28 ( 2013 ) [76] P. Coloma , H. Minakata and S.J. Parke , Interplay between appearance and disappearance channels for precision measurements of 23 and , Phys. Rev. D 90 ( 2014 ) 093003 [77] Daya Bay collaboration , L. Zhan, Recent results from Daya Bay , PoS(NEUTEL2015) 017 [78] J. Burguet-Castell , M.B. Gavela , J.J. Gomez-Cadenas , P. Hernandez and O. Mena , On the measurement of leptonic CP-violation , Nucl. Phys. B 608 ( 2001 ) 301 [hep- ph/0103258]


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Pilar Coloma. Non-standard interactions in propagation at the Deep Underground Neutrino Experiment, Journal of High Energy Physics, 2016, 16, DOI: 10.1007/JHEP03(2016)016