Can Lorentz Invariance Violation affect the Sensitivity of Deep Underground Neutrino Experiment?

We examine the impact of Lorentz Invariance Violation (LIV) in measuring the octant of $\theta_{23}$ and CP phases in the context of Deep Underground Neutrino Experiment (DUNE). We consider the CPT-violating LIV parameters involving $e - \mu$ ($a_{e\mu}$) and $e - \tau$ ($a_{e\tau}$) flavors, which induce an additional interference term in neutrino and antineutrino appearance probabilities. This new interference term depends on both the standard CP phase $\delta$ and the new dynamical CP phase $\varphi_{e\mu}$/$\varphi_{e\tau}$, giving rise to new degeneracies among ($\theta_{23}$, $\delta$, $\varphi$). Considering a small value of $|a_{e\mu}| = |a_{e\tau}| = 5 \times 10^{-24}$ GeV (taken one at-a-time), we find that the octant discovery potential of DUNE gets substantially deteriorated for unfavorable combinations of $\delta$ and $\varphi_{e\mu}$/$\varphi_{e\tau}$. The octant of $\theta_{23}$ can only be resolved at $3\sigma$ if $\theta_{23}$ turns out to be at least $5^{\circ}$ to $7^{\circ}$ away from maximal mixing for any choices of $\delta$ and $\varphi$. Interestingly, we also observe that DUNE can regain its octant resolution capability if we consider both the LIV parameters $a_{e\mu}$ and $a_{e\tau}$ together in the analysis. We also reconstruct the CP phases $\delta$ and $\varphi_{e\mu}$/$\varphi_{e\tau}$. The typical $1\sigma$ uncertainty on $\delta$ is $10^{\circ}$ to $15^{\circ}$ and the same on $\varphi_{e\mu}$/$\varphi_{e\tau}$ is $25^{\circ}$ to $30^{\circ}$.


Introduction
New opportunities have emerged on the neutrino oscillation frontier where almost all the available data can be nicely accommodated in a standard three-flavor oscillation framework [1], except few intriguing anomalies uncovered by the very-short-baseline experiments (for recent reviews see [2,3]). There are six fundamental parameters in the three-neutrino (3ν) mixing paradigm: a) three leptonic mixing angles (θ 12 , θ 13 , θ 23 ), b) one Dirac CP phase (δ), and c) two distinct mass-squared splittings 1 (∆m 2 21 , ∆m 2 32 ). After establishing the phenomena of neutrino oscillation conclusively, neutrino physics has now entered into the precision era with an aim to address the following three fundamental pressing issues at unprecedented confidence level.
• Determining the value of charge-parity (CP) violating phase δ -where establishing a value differing from both zero and π would symbolize the discovery of CP-violation (CPV) in the leptonic sector.
• Settling the pattern of neutrino masses. The present oscillation data cannot resolve whether ∆m 2 31 (≡ m 2 3 − m 2 1 ) is positive or negative. It allows us to arrange the 1 ∆m 2 21 (≡ m 2 2 − m 2 1 ) governs the oscillation in the solar sector and ∆m 2 32 (≡ m 2 3 − m 2 2 ) is responsible for the oscillation in the atmospheric sector. Here, the neutrino mass eigenstate m3 has the smallest electron component.
Presently running long-baseline neutrino oscillation experiments Tokai to Kamioka (T2K) [4] and NuMI Off-axis ν e Appearance (NOνA) [5] have already started shading light on the above mentioned issues. Latest T2K results [6] hint towards a HO value for sin 2 θ 23 = 0.53 +0.03 −0.04 for both NH and IH. For the first time, T2K has been able to rule out a large range of values of δ around π/2 at 3σ C.L. irrespective of mass hierarchy. The CP conserving choices of δ (both 0 and π) are also excluded at 95% C.L. by the same data. The most recent measurements by the NOνA Collaboration [7] using both neutrinos and antineutrinos point towards NH, disfavoring IH at 1.9σ C.L. and shows a weak preference for θ 23 in HO over LO at a C.L. of 1.6σ. The NOνA data excludes most of the choices near δ = π/2 for IH at a C.L.
3σ. But, these experiments still have a long way to go and hopefully, their results will be strengthened further with more statistics in near future. The global analyses of world neutrino data [8][9][10][11] also indicate towards NH at more than 3σ C.L. and a non-maximal θ 23 around 2σ with a mild preference for HO. However, the value of the standard CP phase δ is still uncertain by a large extent.
The upcoming high precision long-baseline neutrino oscillation experiments are expected to resolve these crucial issues at high confidence level and to provide a rigorous test of the three-flavor neutrino oscillation framework in the presence of Earth's matter effect [12][13][14]. These experiments include Deep Underground Neutrino Experiment (DUNE) [15,16], Tokai to Hyper-Kamiokande (T2HK) [17], Tokai to Hyper-Kamiokande with a second detector in Korea (T2HKK) [18], and European Spallation Source ν Super Beam (ESSνSB) [19,20]. These mega facilities are supposed to make the measurements with a precision below 1% and therefore, these next generation neutrino experiments may be sensitive to various Beyond the Standard Model (BSM) scenarios [21], which will complement the search for new physics at the ongoing LHC and future collider facilities. In this paper, we consider a specific BSM scenario of Lorentz Invariance Violation (LIV) [22,23] and analyze its impact on the measurements of θ 23 octant and CPV at the DUNE facility.
The Standard Model (SM) is considered to be a low-energy effective gauge theory of a more fundamental framework that also unifies gravitational interactions along with Strong, Weak and Electromagnetic interactions. The natural mass scale of that theory is governed by the Planck mass (M P ∼ 10 19 GeV). There exist studies that propose spontaneous LIV and CPT violations 2 in that more complete framework [25][26][27][28][29]. In the observable low-energy limit, this spontaneous violation of CPT/Lorentz symmetry can give rise to a minimal extension of the standard model through small perturbative terms suppressed by M P . In the present work, we consider this minimal extension of the SM (as developed in [22,23,[30][31][32]) which violates Lorentz invariance as well as CPT symmetry.
Neutrino experiments may feel the presence of Lorentz/CPT violation via the possible changes in neutrino oscillation probabilities, which can happen due to various reasons such as neutrino-antineutrino mixing, energy dependent effects on mass splittings, and time or direction dependent effects [22,23,33,34]. Several neutrino oscillation experiments such as Liquid Scintillator Neutrino Detector (LSND) [35], Main Injector Neutrino Oscillation Search (MINOS) [36][37][38], Mini Booster Neutrino Experiment (MiniBooNE) [39], Double Chooz [40], Super-Kamiokande (SK) [41], IceCube [42,43], and T2K [44] have searched for these LIV/CPT-violating effects in their datasets and have placed competitive constraints on these LIV/CPT-violating parameters. Besides the above mentioned studies by the official Collaborations, there are also several other independent attempts on constraining LIV/CPT-violating parameters in the context of long-baseline accelerator neutrinos [45][46][47][48][49][50][51], short-baseline reactor antineutrinos [52], atmospheric neutrinos [53][54][55], solar neutrinos [56], and high energy astrophysical neutrinos [57][58][59]. Hadron colliders such as LHC can also provide unique opportunity to test LIV/CPT-violating effects at high energy [60,61]. A comprehensive list of the constraints on all the relevant LIV/CPT-violating parameters is available in Ref. [62]. In a recent work, the authors of [50] have performed a detailed analysis to put stronger bounds on the most relevant CPT-violating LIV parameters by simulating the upcoming DUNE experiment. Using these more tightly constrained CPT-violating LIV parameters, we study here for the first time, the octant sensitivity of DUNE in presence of the LIV parameters (|a eµ |, ϕ eµ ) and (|a eτ |, ϕ eτ ). Also, we have explored the capability of DUNE to reconstruct the true values of the standard Dirac CP phase δ and the LIV phases ϕ eµ and ϕ eτ . Our analyses include the presence of both of these sets of LIV parameters individually as well as collectively. For recent status of searches of various BSM physics other than LIV using neutrino experiments, see [2,3,[63][64][65][66][67][68][69] and the references therein.
This paper is organized as follows. Section 2 gives a short overview of the theoretical background pertaining to LIV scenario and provides an analytical discussion on how LIV parameters alter the neutrino and antineutrino appearance probability expressions by introducing an additional interference term, which depends on both the standard CP phase δ and the new dynamical CP phase ϕ eµ /ϕ eτ , giving rise to new degeneracies among θ 23 , δ, and ϕ. In the same section, we also derive approximate analytical expressions to show how these new degeneracies affect the measurement of octant of θ 23 . Section 3 discusses the important detector properties and the ∆χ 2 analysis procedure. In Sec. 4, we show how various LIV parameters affect the exact numerical transition probability P µe . In the same section, we also give bi-event plots to depict how much variation one can expect in the neutrino and antineutrino appearance event rates due to various LIV parameters. We present our main results concerning the octant discovery potential and the capability of reconstruction of the CP phases in Sec. 5. Finally, in Sec. 6, we summarize our results and conclude.

LIV formalism
Lorentz Invariance violating neutrinos and antineutrinos are effectively described by the Lagrangian density [22,32], where,Q is a generic Lorentz Invariance violating operator and the spinor ψ describes the neutrino field. The first term on the right hand side (RHS) of Eq. 2.1 is the usual kinetic term, the second part involves the mass term with the mass matrix M and the 3rd term gives rise to the Lorentz Invariance violating effect, which is small and perturbative in nature, possibly arising from Planck-suppressed effects. Considering only the renormalizable Dirac couplings of the theory, we can start from the Lorentz Invariance violating Lagrangian [32], The observable effect on the left handed neutrinos is controlled by the combinations which are constant hermitian matrices in the flavor space that can modify the standard vacuum Hamiltonian. The first combination is relevant for CPT-violating neutrinos, whereas the second combination is only relevant for CPT-even Lorentz-violating neutrinos. In this work, we will focus on the isotropic component of the Lorentz-violating terms and therefore, we will fix the (µ,ν) indices to zero (0). To simplify our notation, from now on, we will denote 3 the parameter (a L ) 0 αβ as a αβ and (c L ) 00 αβ as c αβ . Explicitly, one can write the Lorentz-violating contribution to the full oscillation Hamiltonian such that, where, U is the neutrino mixing matrix, m i 's are the neutrino mass eigenstates, G F is the Fermi coupling constant, and N e is the electron density along the neutrino trajectory.
The a αβ 's and c αβ 's are the LIV parameters. In Eq. 2.6, the factor −4/3 in front of the second term arises from the non-observability of the Minkowski trace of c L , which forces the components xx, yy, and zz to be related to the 00 component [22]. In this work, we consider the presence of Lorentz-violating effects only due to the first type of terms 4 in Eq. 2.6. Updated constraints on a αβ 's, mainly from Super-Kamiokande, can be found in Refs. [41,62]. Note that, after considering only the CPT-violating LIV terms (a αβ 's), the LIV effect looks similar to the effect of neutral current (NC) non-standard interaction (NSI) during neutrino propagation, which can be described in the following fashion where the NSI term is parameterized as Here, N e corresponds to the electron number density along the neutrino trajectory and the parameters ε m αβ denote the strength of the NSI. One thus finds a correlation between the NSI and LIV scenario through the following relation [70], However, there are important differences between these two scenarios [70,71]. NSI during neutrino propagation is basically an exotic matter effect and hence, plays no role in vacuum, whereas the type of LIV considered here is an intrinsic effect, present even in vacuum. Nevertheless, the equivalence in Eq. 2.9 allows the study of the LIV parameters in longbaseline experiments following an approach, which is quite similar to the treatment of NSI in neutrino propagation.
In this paper, we only consider the LIV parameters a eµ (≡ |a eµ |e iϕeµ ) and a eτ (≡ |a eτ |e iϕeτ ) since these parameters influence the most ν µ → ν e appearance channel, which drives the CPV and octant sensitivity in a typical long-baseline experiment such as DUNE. The probability expression for ν µ → ν e oscillation channel in presence of the LIV parameters a eµ and a eτ can be written as (following the similar expressions in presence of the NSI parameters ε eµ and ε eτ in Refs. [72][73][74]): where, the three terms on the RHS are described below. The first term originating from the standard interaction (SI) of neutrinos with the Earth's matter is given by, where, (2.12) In writing the expression for P µe (SI) in Eq. 2.11, we neglect the solar term α 2 sin 2 2θ 12 c 2 23 sin 2Â ∆ A 2 . This is due to the fact that by considering the values of the oscillation parameters as θ 12 = 34.5 • , θ 13 = 8.45 • , θ 23 = 47.7 • , ∆m 2 21 = 7.5 × 10 −5 eV 2 , ∆m 2 31 = 2.5 × 10 −3 eV 2 (which are in agreement with [8][9][10][11]), we find that the solar term, being proportional to α 2 , is roughly suppressed by 3 to 4 orders of magnitude as compared to the other two terms as shown in Eq. 2.11.
To describe the second and the third terms of the RHS of Eq. 2.10, describing the effect of LIV due to the presence of a eµ and a eτ respectively, we take the similar approach as followed in the context of NC NSI in [72][73][74] with the NSI parameter ε αβ replaced appropriately (as in Eq. 2.9). Thus, the LIV terms in Eq. 2.10 can be written in the following compact form: where, (2.14) We note that the factorÂ ∆ √ 2G F Ne in Eq. 2.13 becomes L/2 (see Eq. 2.12.), thereby making the LIV effect considered here explicitly matter independent.
Following [73], now we explain the issue of octant sensitivity of θ 23 by expressing the atmospheric mixing angle as: such that the positive angle η quantifies the deviation from the maximal mixing. The positive (negative) sign corresponds to HO (LO). The current three-flavor global analyses [8][9][10][11] indicate that θ 23 cannot deviate from 45 • by more than ∼ 6 • , i.e., sin 2 θ 23 must be in the range [0.4, 0.6]. Therefore, one has η 0.1, and we can use the expansions, An experiment is sensitive to the octant of θ 23 if at the probability level the following difference between the true octant (tr) and test octant (ts) is nonzero at a detectable level. ∆P = P tr µe (θ tr 23 , δ tr , ϕ tr ) − P ts µe (θ ts 23 , δ ts , ϕ ts ) . (2.17) Since P µe consists of the three terms in Eq. 2.10, we can write, To analyse the three terms on the RHS of Eq. 2.18, we take the case of HO (LO) as true (test) octant as an example. Then for the SI term, where, The LIV contribution to Eq. 2.18 can be written as, where, In DUNE, neutrinos and antineutrinos travel the distance of L = 1300 km and for this baseline, the line-averaged constant Earth matter density turns out to be ρ = 2.95 gm/cc [75]. We also assume that Earth's matter is electrically neutral and isoscalar for which we have N e = N p = N n , where N p , N n are the proton and neutron densities respectively. Under this assumption, the relative number density Y e (≡ Ne Np+Nn ) comes out to be 0.5. Also note that for DUNE baseline, the first oscillation maximum (∆ π/2) occurs at E ≈ 2.5 GeV assuming ∆m 2 31 = 2.5 × 10 −3 eV 2 . With these benchmark choices of parameters, we obtain the following approximate numerical values: where, −(+) sign is for β = µ(τ ). It is clear from Eqs. 2.24 and 2.25 that for |a eµ |(|a eτ |) 10 −24 GeV, ∆P µe (a eµ ) (∆P µe (a eτ )) becomes comparable to the standard interference term in ∆P µe (SI). Moreover, ∆P µe (a eµ ) and ∆P µe (a eτ ) depend not only on the standard CP phase δ, but also on the new dynamical CP phase ϕ eµ /ϕ eτ related to the LIV. Due to this extra degree of freedom in ∆P µe (a eµ )/∆P µe (a eτ ), the octant sensitivity can potentially become worse for unfavorable combinations of δ and ϕ eµ /ϕ eτ . In addition, we note that the first terms in ∆P µe (a eµ ) and ∆P µe (a eτ ) appear with the opposite sign. It suggests that when both the LIV parameters a eµ and a eτ are present together, their effect may get cancelled to a large extent, and the chances of measuring octant in DUNE remain intact.

Simulation details
The proposed Deep Underground Neutrino Experiment (DUNE) is a world-class facility which is going to unravel some fundamental issues in neutrino sector, namely, the measurement of leptonic CP-violation, the determination of the neutrino mass ordering, and the precision measurement of the neutrino mixing parameters [15,16,76,77]. In order to simulate DUNE, we use the GLoBES package [78,79] with the most recent DUNE configuration files provided by the collaboration [80]. To analyze the Lorentz-violating scenario, we perform our simulation of the DUNE experiment using the GLoBES-extension snu.c as described in Refs. [81,82]. This extension was originally introduced in GLoBES software to study non-standard neutrino interactions and sterile neutrinos in the context of long-baseline experiments. For the present analysis, we modify the definition of the neutrino oscillation probability function inside snu.c by implementing the Lorentz-violating Hamiltonian as given in Eq. 2.6. We assume a total run-time of 7 years with 3.5 years in the neutrino mode and the remaining 3.5 years in the antineutrino mode with an on-axis 40 kiloton liquid argon far detector (FD) housed at the Homestake Mine in South Dakota over a baseline of 1300 km. The optimized neutrino beam is obtained from a G4LBNF simulation [83,84] of the LBNF beam line using NuMI-style focusing. The neutrino beam is generated using 80 GeV proton beam having a beam power of 1.07 MW, which can deliver 1.47 × 10 21 protons on target per calendar year. It corresponds to a total exposure of 300 kt·MW·yrs.
To simulate the DUNE event spectra, we consider the reconstructed neutrino and antineutrino energy range of 0 to 20 GeV for both appearance and disappearance channels. While preparing our sensitivity plots, we perform a full spectral analysis with total 71 bins in the entire energy range having non-uniform bin widths. We have total 64 bins each having a width of 0.125 GeV in the energy range of 0 to 8 GeV and 7 bins with variable widths beyond 8 GeV [80]. While estimating the signal and background event rates in the appearance and disappearance modes, we properly take into account the "wrongsign" components, which are present in the beam. We do so for both ν e /ν e and ν µ /ν µ candidate events. We calculate the full three-flavour neutrino oscillation probabilities in matter considering the line-averaged constant Earth matter density of 2.95 gm/cc following the standard Preliminary Reference Earth Model (PREM) [85].
The main sources of backgrounds for the appearance events in neutrino and antineutrino modes are the intrinsic ν e /ν e contamination in the beam, the µ − /µ + events which are misidentified as e − /e + events, backgrounds arising from ν τ /ν τ appearance, and the NC events. For the disappearance events in neutrino and antineutrino modes, the main backgrounds stem from the NC events and ν τ /ν τ appearance. We incorporate the systematic uncertainties following Ref. [80]. We consider an independent normalization uncertainty of 2% on both ν e andν e signal modes, while the ν µ andν µ signal modes have uncorrelated normalization errors of 5%. As far as the normalization uncertainties on various backgrounds are concerned, they vary in the range of 5% to 20% with possible correlations among various sources of backgrounds.
To obtain the sensitivity results, we numerically calculate the ∆χ 2 between the true and test event spectra using GLoBES. Unless mentioned otherwise, we consider a fixed value of |a eβ | = 5 × 10 −24 GeV (where β can be µ or τ ) while generating the true and test event spectra. For a true value of δ and ϕ eβ , the true number of events in the i-th energy bin N i (θ true 23 , δ true , ϕ true eβ ) is estimated by assuming a true octant scenario, which can be either true lower octant (i.e., θ true 23 < π/4) or true higher octant (i.e., θ true 23 > π/4). The fixed true and test values of the solar oscillation parameters and 1-3 mixing angle are θ 12 = 34.5 • , ∆m 2 21 = 7.5×10 −5 eV 2 , and θ 13 = 8.45 • . As far as the atmospheric mass-squared difference is concerned, we generate the data with a true value of ∆m 2 31 = 2.5 × 10 −3 eV 2 and we marginalize over test ∆m 2 31 in the fit in its present 3σ allowed range of (2.41 − 2.6) × 10 −3 eV 2 . We assume NH both in data and theory 5 . The theoretical event spectra are generated assuming the opposite/wrong octant scenario, where θ test 23 is marginalized over all possible values in the wrong octant only. δ test and ϕ test eβ are marginalized over the full parameter space of [−π, π]. The ∆χ 2 thus gives a quantitative idea about the capability of the experiment to distinguish the true octant scenario from the wrong octant 6 .

Transition probability and bi-event plots
To demonstrate the impact of LIV, we have plotted P µe as a function of energy in Fig. 1 for both SI (black curves) and in presence of LIV (red curves). The left (right) panels assume the presence of the single LIV parameter a eµ (a eτ ). The top panels refer to representative CP conserving values [0, 0] of the two relevant phases [δ, ϕ eβ ] as indicated in each panel. The bottom panels are for representative maximal CP-violating choices [-π/2, -π/2] of the two CP phases [δ, ϕ eβ ] as mentioned in each panel. For the purpose of illustration, here, we consider a relatively large strength of the LIV parameter (|a eµ | or |a eτ | is taken to be 2 × 10 −23 GeV). As far as the three-flavor oscillation parameters are concerned, we consider the values θ 12 = 34.5 • , θ 13 = 8.45 • , θ 23 = 47.7 • , ∆m 2 21 = 7.5 × 10 −5 eV 2 , ∆m 2 31 = 2.5 × 10 −3 eV 2 , and assume NH. Figure 1 clearly demonstrates that the modifications in ν µ → ν e transition probability due to the presence of LIV parameters depend upon the values of the CP phases (δ, ϕ eµ/eτ ). The excellent energy resolution in DUNE may enable us to study the changes in the reconstructed event spectra due to different choices of the CP phases (δ, ϕ eµ/eτ ), which in turn, may help us to reconstruct the values of these CP phases with reasonable accuracy. Now, we introduce the bi-event plots (see Fig. 2) in which the x-axis (y-axis) denotes the total number of appearance events in neutrino (antineutrino) mode. In all the panels, the solid/dashed ellipses depict the SI case, while the colored blobs portray the SI+LIV scheme. The ellipses are obtained by varying the standard Dirac CP phase δ in the range [−π, π]. In case of SI+LIV, there are more than one CP phase and due to the simultaneous variation of these phases in their allowed ranges, we have a convolution of an infinite ensemble of ellipses with different orientations, which give rise to the colored blobs, In left (middle) panel, we obtain the blobs by varying the CP phases δ, ϕ eµ (δ, ϕ eτ ). In right panel, we vary three CP phases δ, ϕ eµ , and ϕ eτ at the same time in their allowed ranges of [−π, π]. In all the panels, the strength of the LIV parameter is taken to be 5 × 10 −24 GeV, which is consistent with [50]. For both SI and SI+LIV, we study four possible cases: two possible mass hierarchies (NH and IH) together with two possible octants (LO and HO), as mentioned in the figure legends. The black solid (dashed) ellipse correspond to the NH-LO (IH-LO) case, while the red solid (dashed) ellipse represents the NH-HO 5 Since the sensitivity of DUNE to exclude the wrong mass hierarchy is very high [77], we keep the hierarchy same in both true and test datasets while performing our simulation. We have checked that DUNE can discriminate between NH and IH at high confidence level even in presence of the LIV parameters. It becomes possible due to the crucial spectral information provided by the on-axis wide-band muon-(anti)neutrino beam in DUNE. 6 The ∆χ 2 is calculated using the method of pull [86][87][88][89]. Also, this ∆χ 2 is valid in the frequentist method of hypotheses testing [87,90]. (IH-HO) scenario. In case of NH, we take the values of the oscillation parameters as θ 12 = 34.5 • , ∆m 2 21 = 7.5 × 10 −5 eV 2 , θ 13 = 8.45 • , ∆m 2 31 = 2.5 × 10 −3 eV 2 , and θ 23 = 42.3 • (47.7 • ) for LO (HO) case [8,9]. For the IH case, the values of the solar oscillation parameters (θ 12 and ∆m 2 21 ) remain the same and for the remaining oscillation parameters, we consider θ 13 = 8.53 • , ∆m 2 31 = −2.42 × 10 −3 eV 2 , and θ 23 = 42.1 • (47.9 • ) for LO (HO) scenario [8,9]. For the SI case, there is a clear separation between the black (LO) and red (HO) ellipses for both NH and IH. Once we introduce the LIV parameters a eµ (left panel) and a eτ (middle panel) one at-a-time, the LO and HO blobs show significant overlap among each other for both possible mass hierarchies. It suggest that in presence of a single LIV parameter, the θ 23 octant separation capability of DUNE may get deteriorated significantly, which we confirm with the help of octant sensitivity plots in the next section. Interestingly, when both the LIV parameters a eµ and a eτ are present together in the scenario (see right panel of Fig. 2), the amount of overlap between the LO and HO blobs gets reduced considerably as compared the single LIV parameter case. This feature is consistent with our previous discussion in Sec. 2 (in connection with Eq. 2.25) that when both the LIV parameters a eµ and a eτ are present together, they may cancel out the impact of each other to a significant extent. In fact, we corroborate this reality while showing DUNE's octant discovery potential in our results section.

Our results
In this section, we present our sensitivity results. We start the discussion by showing the octant discovery potential of DUNE as a function of true values of the standard CP phase δ for both SI and SI+LIV schemes.  5 × 10 −24 GeV, and it remains fixed both in data and theory. As discussed in Sec. 3, in the test dataset, θ test 23 has been marginalized over its all possible values in the wrong/opposite octant including the maximal value (45 • ). In the SI case, we perform the marginalization over δ test in its entire range of [−π, π], while in the SI+LIV scheme, we marginalize over both δ test and ϕ test eβ (where β can be µ or τ ) in their full parameter space of [−π, π]. We note the following features from Fig. 3.

Octant discovery potential as a function of true δ
• For true LO (see top panels), the octant sensitivity for the SI case lies roughly between 4.5σ to 5.2σ depending on the true value of δ. In presence of |a eµ | = 5 × 10 −24 GeV (both in data and theory), the sensitivity can be as low as ∼ 1σ depending on the value of true δ and true ϕ eµ (see top left panel). Similar degradation in the sensitivity is also observed in presence of a eτ (see top middle panel). Since the standard CP phase δ, as well as the LIV CP phases ϕ eµ and ϕ eτ are still undetermined, such spoiling of octant sensitivities is very much possible.
• For true HO (see bottom panels), the octant sensitivity for the SI case is relatively lower (approximately 2.2σ to 2.7σ). Here, in presence of a eµ or a eτ , one can observe similar reduction in the sensitivity as we notice in the true LO case. The sensitivity may decrease to very small values ( 1σ) for many choices of true values of δ and ϕ eµ/eτ (see bottom left and bottom middle panels).
• In the right panels, in presence of both the LIV parameters a eµ and a eτ with the same magnitude, the worsening in the octant sensitivity is significantly less than what we observe for the single LIV parameter case. For true LO (HO), the sensitivity does not go below ∼ 3.2σ (1.5σ). As we have discussed in sections 2 and 4, this is due to the fact that a eµ and a eτ effectively nullify the impact of each other to a significant extent (due to the presence of a relative sign between the ∆P µe (a eµ ) and ∆P µe (a eτ ) terms in Eq. 2.25). This very interesting and counterintuitive impact of LIV on octant sensitivity is discussed for the first time in the present work.
• The ∆χ 2 curves in presence of LIV have prominent peaks, which are more apparent for true LO. In presence of the LIV parameter a eµ , the choice of CP-conserving true values of ϕ eµ = 0, π (i.e., red and green curves, respectively) roughly produces peaks around maximal CP-violating true values of δ π/2, −π/2, respectively. Conversely, maximal CP-violating true values of ϕ eµ = π/2, −π/2 (i.e., blue and magenta curves, respectively) approximately produce peaks near CP-conserving true values of δ 0, ±π, respectively. This trend can also be observed in presence of a eτ with the location of the peaks interchanged. In presence of both a eµ and a eτ , such a prominent feature is not noticed.

Octant discovery potential in [sin
The exact value of sin 2 θ 23 is still to be determined. Therefore, we consider all the allowed values of sin 2 θ 23 and portray in Fig. 4, the discovery potential of the true octant in the parameter space of true sin 2 θ 23 -true δ at 2σ (solid blue curves), 3σ (dashed magenta curves), and 4σ (dotted black curves) confidence levels (

Octant discovery potential as a function of LIV strength
So far, we have kept the modulus of the LIV parameters |a eµ | and |a eτ | fixed in our analyses. Now, it would be quite interesting to see how the octant discovery potential gets modified if we vary the strength of the LIV parameters |a eµ | and |a eτ |. We present the result of this analysis in Fig. 5, which exhibits the discovery potential of the θ 23 octant as a function of the strength of the LIV parameter |a eµ | (|a eτ |) in left (right) panel assuming NH both in data and theory. The true and test values of |a eµ | and |a eτ | are same in the simulation.
In both the panels, we marginalize over the test values of θ 23 in the wrong octant and the standard CP phase δ (both true and test) in its full range of [−π, π]. In addition to this, in the left (right) panel, the true and test values of the new CP phase ϕ eµ (ϕ eτ ) have been marginalized away in the entire range of [−π, π]. We show the results at three different confidence levels (1 d.o.f.): 2σ (solid blue curves), 3σ (dashed magenta curves), and 4σ (dotted black curves). It is clear that as the strength of the LIV parameter increases, the discovery potential of the true octant gets deteriorated gradually. We notice that as the strength of the LIV parameters approaches towards 10 −25 GeV, the sensitivities slowly get improved and attain the values which we obtain in the SI case.

Reconstruction of the CP phases
In the previous subsections, we discuss in detail how the standard CP phase δ and the new dynamical CP phase ϕ eµ / ϕ eτ would affect the measurement of the octant of θ 23 in DUNE.
In this subsection, we explore the capability of DUNE in reconstructing the true values of the CP phases δ and ϕ eβ (where β can be µ or τ ). Fig. 6 shows the reconstructed regions for the two CP phases δ and ϕ eµ (top panels) at 1σ, 2σ, and 3σ (1 d.o.f.) confidence levels assuming NH both in data and theory. The bottom panels in Fig. 6   for the two CP phases δ and ϕ eτ . The two left panels refer to the typical CP-conserving true values of the phases [0, 0], while the two right panels deal with the illustrative CPviolating true values of the phases [−π/2, −π/2]. In all the panels, the strength of the LIV parameter is assumed to be 5 × 10 −24 GeV, and it remains fixed both in data and theory. While generating the prospective data for DUNE, we consider the true value of θ 23 to be 45 • and in the fit, we marginalize over the test values of θ 23 in its 3σ allowed range of 41.8 • to 50.7 • . DUNE can measure the CP phases δ and ϕ eµ quite efficiently providing a unique reconstructed region around δ true = ϕ true eµ = 0 • at 3σ confidence level (see top left panel). But, in presence of a eτ (see bottom left panel), the reconstruction becomes quite poor for ϕ eτ at 2σ and above. For maximal CP-violating choices (−π/2, −π/2) of the true CP phases (see top right and bottom right panels), the reconstruction of δ true becomes slightly worse as compared to the CP-conserving scenarios at 1σ confidence level, while the reconstruction of ϕ true eµ and ϕ true eτ remains more or less same. In Table 1, we mention the typical 1σ allowed ranges around the true values of the CP phases δ and ϕ eβ (where β can be µ or τ ) assuming the strength of the LIV parameters |a eµ | and |a eτ | to be 5×10 −24 GeV, which remains fixed both in data and theory. We have also checked that the reconstruction of the CP phases becomes worse as θ 23 deviates from the maximal mixing.  Table 1. The typical 1σ allowed ranges around the true values of the CP phases δ and ϕ eβ (where β can be µ or τ ) assuming the strength of the LIV parameters |aeµ| and |aeτ | to be 5 × 10 −24 GeV, which remains fixed both in data and theory.

Summary and conclusion
We have a well-defined neutrino roadmap to resolve the remaining fundamental unknowns, in particular, the determination of neutrino mass hierarchy, the clear demonstration of leptonic CP-violation (CPV), and the precision measurement of the oscillation parameters with the help of upcoming high-precision long-baseline neutrino oscillation experiment DUNE. This experiment will perform a rigorous test of the three-flavor oscillation framework and play an important role to test the existence of various new physics scenarios if they at all exist in Nature. One such new physics scenario is Lorentz Invariance Violation (LIV).
In this paper, we study the impact of LIV in determining the octant of θ 23 and in reconstructing the CP phases considering the Deep Underground Neutrino Experiment (DUNE) as a case study. We discuss in detail how the two most relevant CPT-violating LIV parameters a eµ (≡ |a eµ |e iϕeµ ) and a eτ (≡ |a eτ |e iϕeτ ) affect neutrino and antineutrino appearance probabilities. These LIV parameters (a eµ or a eτ ) introduce an additional interference term in ν µ → ν e andν µ →ν e oscillation channels. This new interference term depends on both the standard CP phase δ and the new dynamical CP phase ϕ eµ /ϕ eτ . This term gets summed up with the well-known interference term related to the standard CP phase δ and gives rise to new degeneracies among θ 23 , δ, and ϕ. These new degeneracies spoil the measurement of octant of θ 23 . We show that for values of the LIV parameter (taken one at-a-time) as small as |a eµ | = |a eτ | = 5 × 10 −24 GeV, the octant discovery potential of DUNE deteriorates considerably for unfavorable combinations of the two CP phases δ and ϕ eµ /ϕ eτ . DUNE can only resolve the octant ambiguity of θ 23 at 3σ confidence level for any choices of δ and ϕ if θ 23 turns out to be at least 5 • to 7 • away from maximal mixing. We also perform the analysis considering both the LIV parameters a eµ and a eτ together and observe for the first time that they largely nullify the effect of each other due to the apparent relative sign between the a eµ -term and the a eτ -term in the probability expressions. For this reason, DUNE can retrieve its octant resolution capability if both the LIV parameters a eµ and a eτ are present together in the analysis. We also study how the deterioration of the θ 23 octant discovery potential varies with the magnitude of the LIV parameters in the [sin 2 θ 23 (true) -|a eβ | (true)] plane where β can be µ or τ . We also address how well DUNE can reconstruct the standard CP phase δ and the new dynamical CP phase ϕ eµ /ϕ eτ . Our analysis reveal that the typical 1σ uncertainty on δ is 10 • to 15 • and the same on ϕ eµ /ϕ eτ is 25 • to 30 • . So, at the end, we conclude that a small amount of Lorentz Invariance Violation (LIV) may affect the measurements of octant of 2-3 mixing angle and the CP phases at DUNE and we hope that our present study will be a valuable addition to the landscape of new physics scenarios beyond the standard three-neutrino oscillation paradigm which can be probed using the DUNE facility.