# Searches for sterile neutrinos with IceCube DeepCore

## Abstract

We show that study of the atmospheric neutrinos in the 10–100 GeV energy range by DeepCore sub-array of the IceCube Neutrino Observatory can substantially constrain the mixing of sterile neutrinos of mass eV with active neutrinos. In the scheme with one sterile neutrino we calculate and oscillation probabilities as well as zenith angle distributions of (charge current) events in different energy intervals in DeepCore. The distributions depend on the mass hierarchy of active neutrinos. Therefore, in principle, the hierarchy can be identified, if exists. After a few years of exposure the DeepCore data will allow to exclude the mixing indicated by the LSND/MiniBooNE results. Combination of the DeepCore and high energy IceCube data will further improve sensitivity to mixing parameters.

###### pacs:

14.60.Pq, 14.60.St## I Introduction

Mixing of sterile neutrinos of eV mass scale with active neutrinos, as is indicated by the LSND/MiniBooNE results (1); (2), significantly affects the atmospheric neutrino fluxes (3); (4); (5); (6); (7). The primary effect arises in the TeV energy range due to the MSW resonant enhancement of oscillations while neutrinos pass through the matter of the Earth. As a result, the flux, and consequently, number of events at the detectors deplete. The oscillations lead to distortion of the zenith angle and energy distributions of events.

In this paper we will show that the atmospheric neutrino fluxes at low energies, TeV, are also strongly affected by the oscillations in spite of the fact that the resonance enhancement occurs in the TeV range. Therefore studies of the low energy fluxes can substantially contribute to searches for sterile neutrinos. With a densely spaced array of phototubes in the middle of the IceCube array, DeepCore sub-array (8), (9) significantly enhances IceCube sensitivity to GeV neutrinos. This makes possible to study the atmospheric neutrino oscillations with DeepCore at low energies (10); (11); (12); (13).

As it was realized in Ref. (5), the effects depend not only on relevant for the LSND/MiniBooNE results but also on the admixture . There are two special cases: (i) , which corresponds to the so called flavor-mixing scheme, and (ii) which determines the mass-mixing scheme for maximal 2-3 mixing. In the latter case mixes with the active neutrinos through the mass eigenstate . At energies below TeV in the mass-mixing scheme the effects are strong, whereas in the flavor-mixing scheme the oscillation probabilities are unaffected (5). In this paper for illustration we consider a scheme with one sterile neutrino, as was favored by recent MINOS data (14); (15) and global fit (16) and focus on the mass-mixing scheme. We show that the mixing angle with the active neutrinos can be significantly constrained by GeV atmospheric neutrino data collected in DeepCore (8).

We present oscillation probabilities in the mass-mixing scheme at low energies in Sec. II. In Sec. III we calculate the event rate in DeepCore produced by atmospheric neutrinos. We study the zenith and energy distributions of these events. We estimate the sensitivity of DeepCore to the mixing with active neutrinos in Sec. IV. Sec. V contains discussion and conclusions.

## Ii Oscillation Probabilities

At high energies to a good approximation one can consider mixing of the three flavor states in the mass eigenstates , neglecting the mixing of (5). In the mass-mixing scheme, the mixing matrix , defined as , depends on the angle and new “sterile” angle , so that in

For , when the state decouples and the 3evolution reduces to 2evolution, the survival probability is given by

(1) |

Here is the length of neutrino trajectory characterized by the zenith angle , and is the radius of the Earth. In our numerical estimations we use eV and .

According to Eq. (1) the first oscillation minimum (dip) is at energy

(2) |

For neutrinos moving along the Earth’s diameter, , we obtain GeV.

If , the oscillation probability changes substantially due to matter effect. For GeV to a good approximation the effect is described by oscillations in uniform medium with the average density along the neutrino trajectory. In turn, for constant density and for energies below 0.5 TeV the probability is given by (5)

(3) | |||||

after averaging over fast oscillations driven by the mass squared difference eV. Here is the average matter potential: , and is the average number density of neutrons along the trajectory. The lower “” (the upper “”) sign in front of in Eq. (3) corresponds to antineutrinos (neutrinos). Thus, in the first approximation the effect is reduced to appearance of an additional contribution to the oscillation phase. This contribution has different signs in the and channels as well as for normal (NH) and inverted (IH) mass hierarchies of the active neutrinos (i.e. for the positive and negative signs of ).

According to Eq. (3) the energy of the first oscillation dip changes due to mixing as

(4) | |||||

where the lower sign in denominator corresponds to antineutrinos for the normal mass hierarchy and to neutrinos for the inverted mass hierarchy. For , fixed , NH and (an average density g cm) the oscillation dips are at GeV and GeV for neutrinos and antineutrinos, respectively. This induced shift of the oscillation dip can be used to constrain the mixing angle .

We computed the oscillation probabilities as functions of neutrino energy and zenith angle by numerically solving the evolution equation (5) with the density profile given by the Preliminary Reference Earth Model (18). The features of the obtained results can be easily understood with Eqs. (1) to (4).

Figure 1 shows the (top panel) and (bottom panel) oscillation probabilities as functions of neutrino energy for different but fixed zenith angle . The energies of the oscillation dips are in good agreement with the approximate values from Eqs. (2) and (4). According to Fig. 1 the energy of resonant oscillation dip in the channel is proportional to . In contrast, at energies GeV the probabilities depend on very weakly, which can be seen explicitly in Eq. (3). From the bottom panels, we find that at low energies mainly transforms to , whereas at high energies transition is significant.

Figure 2 shows the probabilities and as functions of neutrino energy for different values of , but fixed and and for NH. With decrease of the length of the neutrino trajectory decreases and becomes smaller. Furthermore, the difference of probabilities with and without decreases.

In Figure 3 we show dependence of the survival probabilities on the absolute value of and on its sign, i.e. on mass hierarchy of active neutrinos. A variation of also shifts the dip. However, due to dependence of on and energy dependence of the usual () term in Eq. (3) the effects of variations and of sterile neutrino are different. Thus, studies of the energy and zenith angle dependence of the event rates will allow to disentangle the two effects. Change of the mass hierarchy leads to interchange of and probabilities at low energies. As a result, for IH the probability is below the probability in whole energy range, and there is no intersection of the two at 0.5 - 0.7 TeV. As follows from Figure 3, the effect of uncertainty (within 68% CL region allowed by the MINOS results (17)) on the probabilities, is relatively small. However, it becomes significant when events from and interactions sum up.

## Iii Event rates in DeepCore

We calculate the (charged current) event rate in DeepCore. The flux at the detector equals , where the original atmospheric flux, , is larger than the original flux, , by a factor in the energy range under consideration. Furthermore, and mostly converts into (5). So, we will neglect the effect of transition. However, we do take into account contributions from the tau leptons, created by the interactions. Tau leptons decay into muons with branching ratio being recorded as events. The flux at the detector equals . To be detected as a event in the same muon energy bin the energy needs to be times higher than a energy. Thus, the rate of events in the neutrino energy and zenith angle bin equals

(5) | |||||

We use the DeepCore “Filter” effective area from Ref. (8) and the atmospheric neutrino fluxes model of Ref. (19). The DeepCore effective area is largely insensitive to the zenith angle (20) so that . The contribution of the decays to the total event rate (the second term in Eq. (5)) is . Since at low energies secondary leptons from the interactions are scattered at larger angle from the directions of the primary neutrinos, we use large zenith angle bins , as compared to the bins for GeV data (21). We assume that for events the neutrino energy will be reconstructed with factor of 2 accuracy which implies detection of both muon and the associated (hadron) cascade. Therefore we use the energy bins .

Figure 4 shows the zenith angle distributions of events at DeepCore in different energy intervals. The histograms represent the event rates with and without mixing correspondingly for NH (left) and IH (right). The rates decrease with increase of which reflects the dip in the oscillation probability. The decrease is steeper in the low energy range which covers the minimum of the dip. With decrease of the mixing the difference of histograms decreases as . Due to summation of the neutrino and antineutrino signals the total effect on the number of events is smaller than the effect on probabilities. Still the compensation is not complete due to difference of the original fluxes and cross-sections of the neutrinos and antineutrinos. For IH the effect is smaller than for NH, especially for deep (near vertical) trajectories. The reason is that for IH relative deviation of the survival probability from that without mixing is smaller than deviation for probability (see Fig. 3). This is compensated by larger flux and cross section of . Notice that difference of the event numbers in each of the zenith angle bins can reach 2 - 3 after 1 year exposure.

We define the suppression factor as the ratio of the rate with mixing to the same rate without mixing (see also Ref. (5)). Figures 5 and 6 show the suppression factors as functions of zenith angle in different energy ranges for NH and IH correspondingly. As can be seen from Fig. 5 for NH the mixing mostly affects the vertically upcoming events in the lowest, 15–30 GeV, energy bin. The excess of events in this bin is due to enhanced survival probability near the oscillation minimum at GeV (see Figs. 1 and 2). For IH (Fig. 6) the next bin rate is equally affected. The distributions depend on weakly.

In the bottom panels of Figures 5 and 6 we show possible modification of the ratio due to inprecise knowledge of . This is illustrated by the ratio of the two distributions without for two different values of : the “true” (observed) value and the “fit” value. Variations of produce shift of the dip and therefore qualitatively similar distortion of the ratio. Quantitatively the effects are different: the effect of variations is smaller than the one of at high energies. For IH and the two effects have opposite signs, etc.. In analysis of data one should use as fit parameter varying in the range allowed by accelerator experiment measurements. In future will be determined with accuracy eV which will substantially reduce the uncertainty.

## Iv Estimation of sensitivity to mixing

Exposure | ||||
---|---|---|---|---|

0.02 | 1 yr | 7.62 [3.47] | 1.03 [1.03] | [] |

(NH) | 5 yr | 38.1 [5.59] | 1.03 [1.03] | [] |

0.04 | 1 yr | 41.1 [18.7] | 1.06 [1.06] | [] |

(NH) | 5 yr | 205 [29.7] | 1.06 [1.05] | [] |

0.02 | 1 yr | 4.50 [1.84] | 1.00 [1.00] | 0.04 [ 0.04] |

(IH) | 5 yr | 22.5 [2.92] | 1.00 [1.00] | 0.04 [ 0.04] |

0.04 | 1 yr | 14.8 [5.49] | 1.01 [1.01] | 0.09 [ 0.10] |

(IH) | 5 yr | 73.8 [8.47] | 1.01 [1.00] | 0.09 [ 0.10] |

To estimate sensitivity of the DeepCore to sterile neutrinos we perform a simple analysis of the data generated in assumption of zero mixing. We assume that is known precisely. We fit these “data”with number of events obtained in the presence of mixing. To take into account possible systematic errors, as in Ref. (5), we introduce an overall normalization factor and a tilt parameter for the zenith angle distribution of the event rates in Eq. (5) as

(6) |

We use eV. Defining the “null” distribution of zenith angle events without mixing as , we calculate value as

(7) |

Then is minimized by varying and . The results, and the corresponding values of and are listed in the Table 1 for 1 yr and 5 yr of exposure and for two different values of . According to Fig. 4, already after 1 year of data taking the statistical error in each bin is expected to be –. However, as pointed out in Ref. (7), systematic errors for IceCube are not well defined yet and will likely dominate statistical errors. To illustrate this effect on the sensitivity to we performed analysis by introducing a uncorrelated systematic error for each bin in addition to the statistical and correlated systematic (slope and normalization) errors. The values of and () in this case are reported in Table 1 within brackets. The values in the Table should be compared with which corresponds to zero mixing with .

For NH the obtained values with 2 degrees of freedom mean that even with additional systematic uncertainties, or can be excluded at CL with one year of DeepCore data. As a result, the oscillation interpretation of LSND/MiniBooNE data (1); (2) that requires for eV will be severely constrained.

In the case of or five years of DeepCore data would be required to reach CL for exclusion. This is comparable with the current bound from the MINOS experiment (14). A mixing angle smaller than cannot be excluded with DeepCore data alone. For IH the effects is substantially smaller and only can be tested.

We estimate that the present uncertainty in reduces the sensitivity to mixing by factor of 2, i.e. (for NH) can be excluded at CL after 4 years of the data taking.

## V Discussion and Conclusion

A combined analysis of the IceCube high-energy data which cover the MSW resonance dip at TeV energies, together with DeepCore low energy data will improve greatly the sensitivity to mixing parameters. Furthermore, a distinction between the flavor- and mass-mixing schemes will be possible since DeepCore event distributions are affected in the case of mass-mixing only, as we have studied here, while the IceCube event distributions are affected in both mixing schemes (5).

Notice that search for sterile neutrinos with IceCube and DeepCore are complementary to that with MINOS and other accelerator experiments. Indeed, IceCube measures the mass squared difference and mixing at much higher energies and with large matter effect. In scenarios with energy and enviroment dependent neutrino masses, the mass and mixing parameters may turn out to be substantially different in this two setups.

We considered the oscillation effects for specific mixing scheme and specific values of parameters and presented an illustrative analysis of simulated data. General analysis would include the sub-leading effects of the non-zero 1-3 mixing, possible effects of the CP-violation associated to existence of sterile neutrino, consideration of different values of , etc.

In conclusion, we have found that mixing of the eV scale mass indicated by LSND/MiniBooNE, substantially affects the oscillation probabilities in the range 15 - 120 GeV accessible to IceCube DeepCore experiment. The effect is opposite in and channels and can reach size at the probability level. The mixing produces a shift and modifies shape of the oscillation dip. The effect is different for the normal and inverted mass hierarchies of the active neutrinos. Therefore, in principle, the hierarchy can be identified, if the sterile neutrinos with relatively large mixing exist. The zenith angle distributions of the events in different energy ranges are changed. However, due to summation of and signals the effect of mixing and oscillations on the number of events is much weaker. Uncertainty in reduces sensitivity of DeepCore to sterile neutrinos. Nevertheless we find that Deep Core can probe the mixing down to for wide range of .

## Acknowledgments

We are grateful to D. F. Cowen and J. Koskinen for correspondence on the design and performance of the IceCube DeepCore. Work of S.R. was funded by NASA, and performed at and while under contract with the U.S. Naval Research Laboratory. S.R. would also like to thank the Abdus Salam ICTP for hospitality while completing the final manuscript.

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