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Advances in High Energy Physics
Volume 2013 (2013), Article ID 439532, 14 pages
Evidence and Search for Sterile Neutrinos at Accelerators
Los Alamos National Laboratory, Los Alamos, NM 87545, USA
Received 11 June 2013; Accepted 13 August 2013
Academic Editor: Leslie Camilleri
Copyright © 2013 W. C. Louis. This is an open access article distributed under the Creative Commons Attribution License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
The LSND short-baseline neutrino experiment has published evidence for antineutrino oscillations at a mass scale of ~1 eV2. The MiniBooNE experiment, designed to test this evidence for oscillations at an order of magnitude higher neutrino energy and distance, observes excesses of events in both neutrino mode and antineutrino mode. While the MiniBooNE neutrino excess has a neutrino energy spectrum that is softer than expected from LSND, the MiniBooNE antineutrino excess is consistent with neutrino oscillations and with the LSND oscillation signal. When combined with oscillation measurements at the solar and atmospheric mass scales, assuming that the LSND and MiniBooNE signals are due to neutrino oscillations, these experiments imply the existence of more than three neutrino mass states and, therefore, one or more sterile neutrinos. Such sterile neutrinos, if proven to exist, would have a big impact on particle physics, nuclear physics, and astrophysics and would contribute to the dark matter of the universe. Future experiments under construction or proposed at Fermilab, ORNL, CERN, and in Japan will provide a definitive test of short-baseline neutrino oscillations and will have the capability of proving the existence of sterile neutrinos.
Neutrino oscillations have been clearly observed at the solar mass scale of and the atmospheric mass scale of . However, evidence for neutrino oscillations at the mass scale has also been given by the LSND [2–6] and MiniBooNE [7–9] experiments. If the signals reported by LSND and MiniBooNE are indeed due to neutrino oscillations, then there is a problem with the three-neutrino paradigm, because it is not possible to explain oscillations at the three different mass scales with only three types of neutrinos. In order to solve this problem, additional “sterile” neutrinos have been proposed [10–14]. Other explanations include, for example, Lorentz violation [15, 16] and sterile neutrino decay [17, 18]. These additional neutrinos would need to be sterile to the weak interaction due to measurements of the width of the boson, which determine that there are three and only three active neutrinos . The evidence for neutrino oscillations from LSND and MiniBooNE will be discussed in the following sections, followed by a discussion of global fits to the world data and future experiments, which will have the capability of proving whether short-baseline neutrino oscillations at the ~1 mass scale and light, sterile neutrinos exist in nature.
2. The LSND Experiment
The LSND experiment  was designed to search for oscillations with high sensitivity and to measure cross-sections. A photograph of the inside of the detector tank is shown in Figure 1. The main characteristics of the LSND experiment are given in Table 1. LSND had the advantage of a very high proton intensity, a large detector mass, and good particle identification. LSND made use of a high-intensity, 798 MeV proton beam that interacted in an absorber to produce a large number of pions.
2.1. Neutrino Beam
LSND made use of the LAMPF accelerator, which was an intense source of low energy neutrinos produced with a proton current of 1 mA at 798 MeV kinetic energy. For the 1993–1995 running period, the production target consisted of a 30 cm long water target (20 cm in 1993) followed by a water-cooled Cu beam dump, while for the 1996–1998 running period, the production target was reconfigured with the water target replaced by a close-packed, high- target. The resulting decay-at-rest (DAR) neutrino fluxes are well understood because almost all detectable neutrinos arise from or decay; and that stop are readily captured in the Fe of the shielding and Cu of the beam stop [21, 22]. The production of kaons or heavier mesons is negligible at these proton energies. The flux is calculated to be only ~8 × 10−4 as large as the flux in the MeV energy range, so that the observation of a event rate significantly above the calculated background would be evidence for oscillations. Figure 2 shows the neutrino energy spectra from and DAR.
The LSND detector  consisted of an approximately cylindrical tank 8.3 m long by 5.7 m in diameter. A schematic drawing of the detector is shown in Figure 3. The center of the detector was 30 m away from the neutrino source. On the inside surface of the tank, 1220 8-inch Hamamatsu PMTs covered 25% of the area with photocathode. The tank was filled with 167 t of liquid scintillator consisting of mineral oil and 0.031 g/L of b-PBD. This low scintillator concentration allows the detection of both Cherenkov light and scintillation light and yields an attenuation length of more than 20 m for wavelengths greater than 400 nm . A typical 45 MeV electron created in the detector produced a total of ~1500 photoelectrons, of which ~280 photoelectrons were in the Cherenkov cone. PMT time and pulse-height signals were used to reconstruct particle tracks with an average RMS position resolution of ~14cm, an angular resolution of ~12°, and an energy resolution of ~7% at the Michel endpoint of 52.8 MeV. The Cherenkov cone for relativistic particles and the time distribution of the light, which is broader for nonrelativistic particles , gave excellent separation between electrons and particles below Cherenkov threshold. Identification of neutrons was accomplished through the detection of the MeV from neutron capture on a free proton. The veto shield enclosed the detector on all sides except the bottom. Additional counters were placed below the veto shield after the 1993 run to reduce cosmic-ray background entering through the bottom support structure. The main veto shield  consisted of a 15 cm layer of liquid scintillator in an external tank and 15 cm of lead shot in an internal tank. This combination of active and passive shielding tagged cosmic-ray muons that stopped in the lead shot. A veto inefficiency of <10−5 was achieved for incident charged particles.
2.3. Oscillation Results
The primary oscillation search in LSND is for oscillations, where the arise from DAR in the beam stop and the are identified through the reaction . This reaction allows a two-fold signature of a positron with a 52.8 MeV endpoint and a correlated 2.2 MeV from neutron capture on a free proton. There are only two significant neutrino backgrounds with a positron/electron and a correlated neutron. The first background is from DAR in the beam stop followed by scattering in the detector. This background is highly suppressed due to the requirements that a be produced, the decays in flight, and the decays at rest prior to capture. The second background is from decay in flight (DIF) in the beam stop followed by scattering in the detector. Additional contributions are from and scattering. This background will mimic the oscillation reaction if the is sufficiently low in energy that it is below the threshold of 18 hit PMTs, corresponding to MeV. Table 2 shows the estimated number of events in the MeV energy range satisfying the electron selection criteria for 100% transmutation and for the two beam-related backgrounds with neutrons.
Table 3 shows the LSND statistics for events that satisfy the selection criteria for the primary oscillation search. An excess of events is observed over that expected from beam-off and neutrino background that is consistent with neutrino oscillations [2–6]. A fit to the distribution, as shown in Figure 4, gives ( DOF), which leads to a beam on-off excess of events with a correlated neutron. is the likelihood that the is a correlated from neutron capture divided by the likelihood that the is an accidental , while is the fraction of electron candidate events with a correlated . Subtracting the neutrino background from DAR followed by scattering ( events) and DIF followed by scattering ( events) (this background also includes contributions from and ) leads to a total excess of events. This excess corresponds to an oscillation probability of ()%, where the first error is statistical and the second error is the systematic error arising from uncertainties in the backgrounds, neutrino flux (7%), efficiency (7%), and efficiency (7%).
A clean sample of oscillation candidate events can be obtained by requiring , where, as shown in Table 3, the beam on-off excess is events, while the estimated neutrino background is only events. Figure 5 displays the energy distribution of events with . The shaded regions show the combination of neutrino background plus neutrino oscillations at low . The data agree well with the oscillation hypothesis. Finally, Figure 6 shows the distribution for events with and MeV, where is the distance travelled by the neutrino in meters and is the neutrino energy in MeV determined from the measured positron energy and angle with respect to the neutrino beam. The data agree well with the expectation from neutrino background plus neutrino oscillations at low ( D.O.F.) or high ( D.O.F.).
The likelihood () fitter is applied to beam-on events in the final oscillation sample and calculates a likelihood in the plane in order to extract the favored oscillation parameters. The product in the plane is formed over the individual beam-on events that pass the oscillation cuts. This three-dimensional contour is sliced to arrive finally at the LSND allowed oscillation region. The beam-related backgrounds are determined from Monte Carlo (MC) event samples for each individual background contribution. The MC contains the trigger simulation and generally very well reproduces the tank response to all particles of interest. Agreement between the data and MC is excellent.
The oscillation parameter fit for the entire data sample, MeV, is shown in Figure 7. The fit includes both and oscillations (although the latter contribution is very small), as well as all known neutrino backgrounds. The inner and outer regions correspond to 90% and 99% CL allowed regions, while the curves are 90% CL limits from the Bugey reactor experiment  and the KARMEN experiment at ISIS . Note that the Bugey limit has been relaxed recently due to the reactor neutrino anomaly . The most favored allowed region is the band from to , although a region around is also possible.
3. The MiniBooNE Experiment
The MiniBooNE experiment was designed to test the LSND neutrino oscillation signal with a neutrino energy and distance that were an order of magnitude higher than LSND but with an ratio that was approximately the same as for LSND. Due to the higher neutrino energies, the backgrounds and systematic errors are completely different between the two experiments.
3.1. Neutrino Beam
A schematic drawing of the MiniBooNE experiment at FNAL is shown in Figure 8. The experiment is fed by 8 GeV kinetic energy protons from the Booster that interact in a 71 cm long Be target located at the upstream end of a magnetic focusing horn. The horn pulses with a current of 174 kA and, depending on the polarity, either focuses and and defocuses and to form a pure neutrino beam or focuses and and defocuses and to form a somewhat pure antineutrino beam. The produced pions and kaons decay in a 50 m long pipe, and a fraction of the neutrinos and antineutrinos  interact in the MiniBooNE detector, which is located 541 m downstream of the Be target. For the MiniBooNE results presented here, a total of POT were collected in neutrino mode and POT were collected in antineutrino mode.
The MiniBooNE detector  consists of a 12.2 m diameter spherical tank filled with approximately 806 tons of mineral oil (CH2). A schematic drawing of the MiniBooNE detector is shown in Figure 9, while a photograph of the inside of the tank is shown in Figure 10. There are a total of 1280 8-inch detector phototubes (covering 10% of the surface area) and 240 veto phototubes. The fiducial volume has a 5 m radius and corresponds to approximately 450 tons. A comparison between the LSND and MiniBooNE experiments is given in Table 1.
3.3. Oscillation Results
Figure 11 shows the estimated neutrino fluxes for neutrino mode and antineutrino mode, respectively. The fluxes are fairly similar (the intrinsic electron-neutrino background is approximately 0.6% for both modes of running), although the wrong-sign contribution to the flux in antineutrino mode (~18%) is much larger than in neutrino mode (~6%). The average plus energies are 0.96 GeV in neutrino mode and 0.77 GeV in antineutrino mode, while the average plus energies are 0.79 GeV in neutrino mode and 0.66 GeV in antineutrino mode. The estimated backgrounds in the two modes are very similar, especially at low energy.
Figure 12 shows the reconstructed neutrino and antineutrino energy distributions, , for candidate and data events (points with error bars) compared to the MC simulation (histogram) [7–9], while Figure 13 shows the event excesses in neutrino and antineutrino mode as a function of . assumes that the events are due to charged-current quasi-elastic scattering. The magnitude and energy shape of the excess in antineutrino mode are very similar to what is expected from neutrino oscillations based on the LSND signal, as shown by the pink and green LSND reference histograms. In neutrino mode, the magnitude of the excess is consistent with LSND; however, the energy shape is softer than the pink and green LSND reference histograms.
Table 4 shows the number of data, background, and excess events for neutrino mode, antineutrino mode, and combined in the neutrino oscillation energy range from 200 to 1250 MeV. The uncertainties include both statistical and constrained systematic errors, where the charged-current data sample is used to normalize the backgrounds. All known systematic errors are included in the systematic error estimate. In neutrino mode, an excess of events, corresponding to , is observed, while in antineutrino mode, the observed excess is events, corresponding to . Combining the data in neutrino and antineutrino modes, the total excess is events, corresponding to .
Figure 14 shows the MiniBooNE oscillation allowed regions [7–9] from fits to the antineutrino data (a) and neutrino data (b). In antineutrino mode, the probability of the best fit is good (66%, corresponding to a ), and the MiniBooNE allowed region overlaps well with the LSND allowed region for , while the KARMEN experiment  rules out most of the LSND allowed region for . Therefore, the MiniBooNE antineutrino data are consistent with simple two-neutrino oscillations and with the LSND oscillation signal. In neutrino mode, the probability of the best fit is not as good (6.1%, corresponding to a ), and the MiniBooNE allowed region overlaps a smaller fraction of the LSND allowed region at low , which is already ruled out by the ICARUS experiment . Therefore, in neutrino mode, the data are marginally compatible with a simple two-neutrino oscillation formalism. Indeed, the initial MiniBooNE oscillation publication  showed that there is hardly any excess of events above 475 MeV in neutrino mode, ruling out simple two-neutrino oscillations as an explanation of the LSND signal. However, expanded models with several sterile neutrinos can reduce the incompatibility by allowing for CP violating effects between neutrino and antineutrino oscillations [10, 11].
Figure 15 shows the MiniBooNE oscillation allowed regions from a combined fit to the antineutrino plus neutrino data samples . As in neutrino mode, the probability of the best fit is not very good (6.7%). However, as discussed above, expanded models with several sterile neutrinos can improve the fit probability by allowing for CP violating effects between neutrino and antineutrino oscillations [10, 11].
4. Global Neutrino Oscillation Analyses
Several global oscillation analyses have been performed on the world neutrino data that include both long-baseline and short-baseline oscillation experiments, including both and appearance data and and disappearance data . In general, the analyses assume a model with 3 light, mostly active neutrinos, heavier, mostly sterile neutrinos, and neutrino mass eigenstates. Precision measurements of the width have determined that the number of active neutrinos is approximately 3 ( ), so that additional neutrinos beyond the three active neutrinos would need to be sterile to the weak interaction. Note that neutrino oscillations depend on the superposition of neutrino mass eigenstates and do not depend on whether neutrinos are active or sterile, so that the neutrino mass eigenstates would result in independent values. Note also that, for , there would exist CP violation parameters for both short-baseline and long-baseline experiments. Finally, note that, for models, neutrinos in general would be a superposition of both active and sterile components.
Table 5 shows the best fit values from recent global fits to the world neutrino data from [10, 11]. (Additional global fits can be found in .) Reference  includes data from the LSND, MiniBooNE, KARMEN, NOMAD, CCFR, CDHS, MINOS, Bugey, SAGE, and GALLEX experiments, while  also includes data from the E776 and ICARUS experiments. For both global fits, the best fit value of is ~0.9 and the goodness of fit probabilities (GOF) are reasonable at 55% and 19%, respectively. However, the parameter goodness of fit probabilities (PGOF) are very low at and , respectively. The PGOF  is based on the difference between the overall best fit chi square and the sum of the best fit chi squares for the appearance-only and disappearance-only experiments. Although there is tension between the appearance and disappearance experiments, we believe that fake data studies would need to be performed in order to calculate the PGOF true probabilities .
Table 6 shows the best fit values from recent global fits to the world neutrino data from [10, 11]. (Additional global fits can be found in .) The GOF probabilities are improved from the fits, although the PGOF probabilities are worse. As mentioned above, we believe that fake data studies would need to be performed in order to calculate the PGOF true probabilities . Figures 16 and 17 show the best fit versus values for the two global fits. Figure 17 also shows the best fit, where the two mostly sterile neutrinos have masses less than and greater than the masses of the mostly active neutrinos.
5. Future Short-Baseline Accelerator Neutrino Experiments
Future accelerator neutrino experiments will have the capability of testing the current evidence for sterile neutrinos. At Fermilab, MINOS+ and MicroBooNE provide a well-coordinated program of experiments that should help determine in the near future whether or not sterile neutrinos can explain the existing short-baseline neutrino anomalies. MINOS+ involves running the MINOS detectors with the NuMI beam in medium energy mode for the NoVA experiment, which provides a much higher flux of neutrinos above a few GeV. High disappearance into sterile neutrinos can be searched for by comparing the event rates in the near and far detectors at higher energies, where the effect of neutrino oscillations at the atmospheric scale is small . MINOS+ should begin taking data later in 2013. The MicroBooNE experiment is under construction in the Booster Neutrino Beam (BNB) just upstream of MiniBooNE at a distance of 0.47 km from the neutrino source. MicroBooNE  consists of a 170-ton (86-ton active volume) liquid argon TPC, that will be able to determine whether the excess of events observed by MiniBooNE is due to electron events, as expected for oscillations, or to photon events, which would indicate some other process. Figure 18 shows the MicroBooNE sensitivity to oscillations. MicroBooNE should begin taking data in 2014.
NuSTORM  is a far future proposal that involves building a muon storage ring with central momentum of 3.8 GeV/c, and it can be built at either Fermilab or CERN. NuSTORM produces fluxes of neutrinos with well-understood energy spectra: and for a stored beam and and for a stored beam. Two magnetized iron neutrino detectors will be built downstream of the storage ring at distances of ~30 m and ~1500 m in order to search for appearance and and disappearance. The allowed LSND and MiniBooNE oscillation regions can be covered at the level, as shown in Figure 19.
ICARUS-NESSIE  is another far future proposal for an experiment at CERN to test the LSND and MiniBooNE oscillation signals. A new neutrino beamline would be built from the SPS with both near and far liquid argon TPC detectors (ICARUS) and muon spectrometers (NESSIE). The near detector location would be at a distance of 300 m from the neutrino source and would contain a 150-ton (T150) liquid argon TPC followed by a muon spectrometer with a dipole magnetic field and iron slabs. The far detector location would be at a distance of 1600 m from the neutrino source and would contain a 600-ton LAr TPC (T600) followed by a muon spectrometer. ICARUS-NESSIE will be able to search for both disappearance and appearance. Figure 20 shows the expected sensitivities for oscillations (a) and oscillations (b) after one year and two years of data taking, respectively. ICARUS-NESSIE will fully cover the LSND and MiniBooNE oscillation allowed regions.
The OscSNS and IsoDAR proposals offer the unique opportunity to observe actual oscillations in the detector (i.e., an oscillation of the number of events in the detector as a function of distance from the neutrino source, correcting for the falloff of the neutrino flux), which would be unmistakable proof for short baseline neutrino oscillations. The OscSNS proposal  involves building a cylindrical detector approximately 60 m from the SNS spallation target . The 1.4 MW beam power of the SNS is a prodigious source of neutrinos from the decay of and at rest. These decays produce a well specified flux of neutrinos via , s and , s. The low duty factor of the SNS (~695 ns beam pulses at 60 Hz, ) is more than 1000 times less than that found at LAMPF. This smaller duty factor provides a reduction in backgrounds due to cosmic rays, and allows the induced events from decay to be separated from the and induced events from decay. The OscSNS detector will be centered at a location 60 meters from the SNS target, in the backward direction. The cylindrical detector design is based upon the LSND and MiniBooNE detectors and will consist of an 800-ton tank of mineral oil (with a small concentration of b-PBD scintillator dissolved in the oil) that is covered by approximately 3500 8-inch phototubes, yielding a photocathode coverage of 25%. Figure 21 shows the expected sensitivity for appearance after two and six calendar years of run time. The LSND allowed region is fully covered by more than .
The IsoDAR proposal  involves the construction of a high-intensity proton cyclotron near an underground detector to search for disappearance. The proposed cyclotron would accelerate ions up to 60 MeV/amu at an intensity of 5 mA. The 60 MeV proton beam then interacts on a 9Be target that is surrounded by a 7Li sleeve. Neutrons produced in the Be target interact in the sleeve to produce 8Li, which decay to produce with an average energy of 6.4 MeV. The can then interact in a kiloton underground detector, such as KamLAND  in Japan. By fitting for oscillations in the detector, IsoDAR would have excellent sensitivity to disappearance, as shown in Figure 22.
The LSND and MiniBooNE experiments both observe excesses of candidate events at the level. Combining these two experiments results in a total excess that is over in significance. Whereas no standard model explanation for these excesses has yet been found, oscillation models with 3 light, mostly active neutrinos and heavy, mostly sterile neutrinos provide a fairly good fit to the world neutrino oscillation data, although there is some tension at present between appearance and disappearance oscillation experiments. Future experiments at Fermilab, CERN, ORNL, and in Japan will test this neutrino oscillation evidence and have the potential to prove the existence of light, sterile neutrinos. Such sterile neutrinos would have a big impact on particle physics, nuclear physics, and astrophysics.
The author thanks the Department of Energy for support. This work was made possible by the dedicated efforts of the LSND and MiniBooNE collaborations.
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