Vol. 40 (2009) ACTA PHYSICA POLONICA B No 9
A REVIEW OF LONG-BASELINE NEUTRINO
OSCILLATION EXPERIMENTS"
David A. Petyt
Tate Laboratory of Physics and Astronomy, University of Minnesota
116 Church St. SE, Minneapolis 55455, USA
(Received July 8, 2009)
In this paper, I will review the status of current and planned accelerator-
based long-baseline neutrino oscillation experiments which are sensitive to
the oscillation parameters associated with the atmospheric neutrino mass-
scale, and are designed to precisely determine the parameters of the PMNS
neutrino mixing matrix.
PACS numbers: 14.60.Lm, 14.60.Pq, 14.60.St, 29.27. a
1. Introduction
The phenomenon of neutrino oscillations is now firmly established by
a variety of experiments detecting solar and atmospheric neutrinos (see [1]
and references therein). The measurements are described by mixing between
the three neutrino flavour and mass eigenstates, which is conventionally de-
scribed in the PMNS parameterisation as a 3×3 unitary mixing matrix with
three Euler angles (¸12, ¸13, ¸23), and one non-trivial CP-violating phase, ´.
Simplifying to the two-flavour approximation, the probability for a neu-
trino of flavour Ä… with energy E (in GeV) to oscillate to a different flavour ²
after travelling a distance L (in km) can be written as:
1.27"m2L
P (½Ä… ½²) = sin2 2¸ sin2 , (1)
E
where "m2 = m2 - m2, is the squared-difference between the neutrino mass
i j
eigenstates i and j. The current experimental data can be explained by two
independent mass-splittings associated with solar and atmospheric neutrino
oscillations: "m2 = 2.4 × 10-3 eV2 and "m2 = 7.7 × 10-5 eV2. The
atm
sol
"
Presented at the 45th Winter School in Theoretical Physics Neutrino Interactions:
From Theory to Monte Carlo Simulations , Lądek-Zdrój, Poland, February 2 11,
2009.
(2629)
2630 D.A. Petyt
mixing angles associated with solar and atmospheric oscillations are large,
sin2 ¸12 = 0.304+0.022 and sin2 ¸23 = 0.50+0.07. The angle ¸13 is as yet
-0.016 -0.06
unmeasured but is known to be small (sin2 ¸13 < 0.035, 90% C.L.) [1]. In
addition, the value of the CP-violating phase, ´, and the ordering of the
neutrino masses, either normal hierarchy (m3 m1) or inverted hierarchy
(m1 m3), are unknown. Neutrino oscillation models invoking a fourth
(sterile) neutrino species are strongly constrained by existing data, including
the recent results from the MiniBooNE experiment [2].
Experiments using accelerator-based sources of neutrinos and long exper-
imental baselines are important tools to address these currently unanswered
questions in neutrino physics, and to precisely measure the oscillation param-
eters. In such experiments, the flavour content, neutrino energy spectrum
and experimental baseline are chosen to maximise the size of the oscillation
effect predicted by Eq. (1).
A significant advantage of long-baseline experiments lies in the use of
two similar detectors. In this approach a Near detector placed close to
the accelerating source measures the initial neutrino energy spectrum and
flavour composition, and a Far detector measures the energy spectrum and
flavour composition after the neutrinos have travelled a sufficient distance
for flavour oscillations to occur. The large uncertainties in neutrino flux
prediction and neutrino cross-sections (which are poorly known in the few-
GeV energy region [3]) significantly cancel when data from the two detectors
are compared.
In this paper I will focus on existing and future accelerator-based long-
baseline experiments which typically employ ½µ beams (produced chiefly
from pion decays) and are sensitive to the atmospheric neutrino mass split-
ting (L/E <" 102 km/GeV). The role of reactor-based experiments, which
are also an important tool to measure the unknown parameter ¸13 of the
PMNS mixing matrix, are described elsewhere [4].
2. Past/current experiments
2.1. K2K
K2K [5] was the first accelerator-based long-baseline neutrino oscilla-
tion experiment. The neutrino beam was provided by 12 GeV protons at
the KEK PS, which produced a 98.8% pure ½µ + ½µ beam peaked at ap-
Å»
proximately 1 GeV. The beam was pointed at the existing 50 kT Super-
Kamiokande Water Cherenkov detector, providing an experimental baseline
of 250 km. Several Near detectors were used, including a 1 kiloton Water
Cherenkov device to measure the neutrino flux at the KEK site, and two fine-
grained detectors to measure the rate of quasi-elastic (QE) and non-QE scat-
tering processes, the ½e beam content and the rate of Ä„0 production, which
A Review of Long-Baseline Neutrino Oscillation Experiments 2631
is the main background for ½µ ½e searches. The prediction of the neutrino
flux at Super-Kamiokande was obtained by multiplying the measured flux
from the Near detectors with the Far/Near flux ratio derived from particle
production data measured on the K2K aluminium target. K2K collected
data from June 1999 to August 2004, accumulating a total of 0.922 × 1020
protons on target (POT).
The ½µ disappearance results from K2K are summarised in Fig. 1. In to-
tal, 112 ½µ charged-current candidates were observed in Super-Kamiokande,
with an expectation of 158.1 (assuming no oscillations). In addition, a dis-
tortion of the Far detector energy spectrum was measured in 58 single
Cherenkov ring events (mainly ½µ QE interactions) consistent with neu-
trino oscillations. The allowed range of the mixing parameters, assuming
½µ ½Ä oscillations, are sin2 2¸23 > 0.6 and 1.9 < "m2 < 3.1 × 10-3 eV2,
atm
with a best-fit of "m2 < 2.8 × 10-3 eV2, sin2 2¸23 = 1.0 [5]. The allowed
atm
region (90% C.L., 2 d.o.f.) shown in Fig. 1 is in good agreement with the
Super-Kamiokande atmospheric neutrino analysis [6].
4.0
4×10
3.5
3.5
3.0
3
2.5
2.5
MINOS best oscillation fit
2.0
2
MINOS 90%
Super-K 90%
1.5 MINOS 68%
1.5 Super-K L/E 90%
MINOS 2006 90%
K2K 90%
1.0
10.6 0.7 0.8 0.9 1
sin2(2¸)
Fig. 1. Allowed regions for the mixing parameters "m2 and sin2 2¸23 for MINOS
atm
and K2K, compared to results from the Super-Kamiokande atmospheric experi-
ment.
A search for sub-dominant ½µ ½e oscillations at the atmospheric neu-
trino mass-scale was also carried out by K2K, by looking for an excess of neu-
trino candidates with electron-like Cherenkov rings in Super-Kamiokande.
A single candidate event was observed, consistent with the background esti-
mate from single Ä„0 production and the intrinsic ½e component of the beam.
From this data, a limit on the mixing angle ¸13 was derived. At the best-fit
2
2
-3
|
"
m | (10 eV )
2632 D.A. Petyt
value of "m2 , a limit of sin2 2¸13 < 0.26 was obtained at 90% C.L. [7].
atm
This compares to the current best experimental limit of sin2 2¸13 < 0.1 from
the CHOOZ reactor experiment [8].
2.2. MINOS
The MINOS experiment utilises a 250 kW neutrino beam provided by
120 GeV protons from the Fermilab Main Injector, and two similar iron/scin-
tillator sampling calorimeters: a 980 T Near detector located at the Fermilab
site, and a 5.4 kT Far detector situated in the Soudan Underground Mine,
MN, at a distance of 735 km from the neutrino source. The neutrino beam
(98.5% ½µ + ½µ) is produced from decays of pions and kaons created by
Å»
the protons impinging on a graphite target. The position of the target can
be adjusted relative to the first focussing horn, producing a continuously
variable neutrino energy spectrum. The most recent results published by
MINOS were derived from 3.36×1020 POT recorded between May 2005 and
July 2007 [9], which consisted of 3.2 × 1020 POT recorded in the low energy
beam configuration (peak energy <" 3 GeV) and 0.15 × 1020 POT in the high
energy configuration (peak energy <" 10 GeV).
The primary physics goal of MINOS is a precision measurement of the
oscillation parameters "m2 and sin2 2¸23 via ½µ disappearance. The ½µ
atm
charged-current energy spectrum at the Far detector location is predicted
using the measured energy spectrum in the Near detector. A beam transfer
matrix is used to translate the true energy spectrum from Near to Far, after
correcting for energy smearing and event selection efficiencies. A total of
730 muon-like events recorded in the low energy beam configuration was
observed in the Far detector, with a no-oscillation expectation of 936. In
the high energy configuration, 118 events were observed with an expectation
of 129. A strong energy-dependent suppression of the event rate is seen, and
the best fit oscillation parameters are "m2 = 2.43 Ä… 0.13 × 10-3 eV2
atm
and sin2 2¸23 = 1.0-0.1 (90% C.L., 1 d.o.f.) [9]. The allowed region shown in
Fig. 1 is in good agreement with K2K and Super-Kamiokande, and represents
the most precise measurement of "m2 to date.
atm
MINOS has also presented a measurement of the neutral current energy
spectrum in the Far detector, for 2.45 × 1020 POT, in order to search for
½µ ½s oscillations, where ½s is a sterile neutrino. Such a transition would
produce a deficit in the number of observed neutral current interactions.
No significant depletion is observed, which provides additional support to
the ½µ ½Ä oscillation hypothesis, and sets a limit on the fraction, fs,
of ½µ oscillating to ½s at the atmospheric mass-scale of fs < 0.68 (90%
C.L.) [10]. MINOS also has sensitivity to sub-dominant ½µ ½e oscilla-
tions via the search for an excess of events in the Far detector with energy
A Review of Long-Baseline Neutrino Oscillation Experiments 2633
depositions consistent with electromagnetic showers. The sensitivity of this
analysis, with the existing data sample, is expected to be competitive with
the CHOOZ limit1.
2.3. OPERA
The OPERA experiment [12] is designed to search for ½Ä appearance
via the observation of tau decay kinks in a high-resolution nuclear emulsion
based detector. The experiment uses a high energy ( E½ = 17 GeV) wide
band ½µ beam (LNGS) produced by the CERN SPS and a hybrid emul-
sion/tracking detector situated in the Gran Sasso Laboratory and has an
experimental baseline of 732 km. The active detector mass of 1.35 kT is
composed of 77,000 emulsion bricks, which consist of alternate layers of lead
absorber (1 mm thickness) and nuclear emulsion (44 µm thickness). The
location of interaction vertices within a particular brick is determined from
extrapolation of measured tracks in scintillator tracking planes which are
located between the 58 brick walls . The bricks containing the candidate
interaction vertices are then removed for scanning and event reconstruction.
A total of 1.782×1019 POT were recorded during the 2008 LNGS run.
Two candidate charm events were observed, consistent with expectations.
Analysis of the exposed emulsion bricks is ongoing. Assuming maximal ½µ
½Ä oscillations with "m2 = 2.5 × 10-3 eV2, this dataset should contain
atm
1 2 ½Ä candidates. A five-year exposure of the LNGS beam is planned.
The expected ½Ä signal, assuming 4.5×1019 POT/year is 10.4 events, with
a background of less than one event. Due to its fine granularity, the OPERA
detector also has good sensitivity to sub-dominant ½µ ½e oscillations, with
a projected limit from a five-year exposure of sin2 2¸13 < 0.06 at 90% C.L.
assuming "m2 = 2.5 × 10-3 eV2.
atm
3. Near-future experiments
The primary goal of the next generation of long-baseline experiments is to
search for evidence of a non-zero value of ¸13. In order to achieve this, large
and fine-grained detectors are required to separate ½e charged-current events
from background (chiefy single Ä„0 events); and increased beam power, in or-
der to probe oscillation probabilities that may be of the order of 1%. Two
projects are planned: the T2K experiment, which uses a newly-constructed
neutrino beamline at the J-PARC facility in Tokai, Japan and the existing
Super-Kamiokande detector (L = 295 km) [13]; and the NOvA experiment,
1
Following this conference, the MINOS experiment released the first results of this
analysis for an exposure of 3.2 × 1020 POT. No significant excess of electron-like
events is observed in the Far detector and a limit of sin2 2¸13 < 0.29 (90% C.L.) is
obtained for "m2 = 2.43×10-3 eV2, assuming the normal hierarchy and ´ = 0 [11].
atm
2634 D.A. Petyt
which will use an upgraded neutrino beam provided by the existing NuMI
facility at Fermilab, and a newly-constructed 15 kT segmented liquid scin-
tillator detector located at Ash River, MN (L = 810 km) [14]. Both ex-
periments use the off-axis beam concept, in which the low-energy neutrino
flux is enhanced (and the high-energy tail is suppressed) by placing the Far
detector one to three degrees off-axis from the neutrino beamline.
The T2K experiment will begin to take data in 2009. The current sched-
ule for NOvA, which is presently awaiting final approval, is for data tak-
ing to start in 2012 with a 2.5 kT Far detector, and for the full 15 kT to
be completed in 2014. The experiments are expected to be sensitive to
sin2 2¸13 <" 0.01 after five years of running at the nominal beam powers of
0.77(0.7) kW for T2K and NOvA, respectively. The sensitivity of the two
experiments to ¸13 also depends on the value of the CP-violating phase,
´ and the sign of "m2 [15].
31
It is possible to determine the sign of "m2 in NOvA by comparing the
31
oscillation probabilities measured in neutrino and anti-neutrino runs. Differ-
ences between oscillation probabilities are enhanced in a region of parameter
space corresponding to one half of ´ by matter effects, which are much larger
in NOvA than T2K due to the factor of three longer baseline (see the left-
hand plot of Fig. 2 which shows the potential of NOvA to resolve the sign of
Fig. 2. NOvA/T2K sensitivitity to the mass hierarchy. Left: 95% C.L. resolution
of the mass hierarchy (sign("m2 )) as a function of ´ from NOvA neutrino and
31
anti-neutrino running (normal hierarchy assumed). Right: the same plot for the
combination of NOvA and T2K measurements. The lines denote three different
assumptions for NOvA and T2K beam power. Plots courtesy [16].
A Review of Long-Baseline Neutrino Oscillation Experiments 2635
"m2 assuming the normal mass hierarchy). Measurements of P (½µ ½e)
31
by NOvA and T2K are complementary due to their different sensitivity to
matter effects. Additional sensitivity to the mass ordering in the region
0 < ´ < Ä„ is provided by the combination of NOvA and T2K measurements
as shown in Fig. 2 (right).
4. Far-future experiments
The third generation of long-baseline experiments (envisaged for the lat-
ter part of the next decade and beyond) are currently in the initial planning
stages in the USA, Japan and Europe. These experiments call for an or-
der of magnitude increase in detector mass (100 300 kT) and beam power
greater than 1 MW. The physics goals of these experiments are to provide
sensitivity to non-zero ¸13, the sign of "m2 , and search for non-zero val-
31
ues of the CP-violating phase ´, for values of ¸13 well below 10-2. Several
detector technologies are being studied, with particular emphasis on Water
Cherenkov and Liquid Argon devices. Longer baselines (1000 1300 km) are
being considered in order to enhance the matter effect (which is proportional
to L) at the first oscillation maximum. Measurements at the first and sec-
ond oscillation maxima (either by measuring the energy spectrum in a single
detector, or placing two detectors at different distances from the neutrino
source) are envisaged. Since the matter effect at the second oscillation min-
imum is much reduced, comparison of measurements at the first and second
maximum can help to distinguish between matter and CP-violating effects.
The current proposals are: in the US for a new beamline from an up-
graded accelerator complex at Fermilab (2.3 MW beam power) to a large
100 300 kT detector situated in the DUSEL Underground Laboratory (L =
1300 km) [17, 18]; in Japan and Korea for massive 270 kT Water Cherenkov
detectors situated at the first (Kamioka, L = 290 km) and second (Korea,
L <" 1000 km) oscillation maximum from an upgraded (1.66 MW) neutrino
beam from J-PARC [19]. In Europe, feasibility studies are underway to as-
sess the possibility of directing high intensity conventional beams or beta
½e beams from CERN to large (<" 100 kT) detectors situated in existing
European underground laboratories [20].
5. Summary
Since 1998, there has been a paradigm shift in neutrino oscillation stud-
ies. With the seminal solar and atmospheric neutrino measurements of
Super-Kamiokande and SNO, and their confirmation by a series of exper-
iments using terrestrial neutrino beams, the phenomenon of neutrino os-
cillations is now well-established. We are now entering into the (precision)
2636 D.A. Petyt
measurement phase of the PMNS matrix elements. In this regard, the role of
long-baseline accelerator based neutrino oscillation parameters will be cru-
cial. The current generation of experiments (K2K, MINOS and OPERA)
are providing precision measurements of the 2 3 sector of the PMNS matrix
and are testing the ½µ ½Ä interpretation of the atmospheric neutrino data.
Although these experiments have some sensitivity to ¸13 beyond current ex-
perimental limits, the next generation of long-baseline experiments (T2K
and NOvA) will greatly expand the reach of ½µ ½e oscillation searches.
By the middle of the next decade, they will provide sensitivity down to
sin2 2¸13 <" 10-2 and, in combination, may provide a resolution of the mass
hierarchy (sign of "m2 ) if sin2 2¸13 > 0.05. In order to extend the sensitiv-
31
ity to lower values of sin2 2¸13 and to provide an opportunity of observing CP
violation in the lepton sector, a third generation of experiments are planned.
These require an order of magnitude improvement in detector size and beam
power over existing experiments.
REFERENCES
[1] T. Schwetz, M. Tortola, J.W.F. Valle, New J. Phys. 10, 113011 (2008).
[2] [MiniBooNE] A.A. Aguilar-Arevalo et al., Phys. Rev. Lett. 98, 231801 (2007).
[3] [MINERvA] D.A. Harris et al.,hep-ex/0410005.
[4] M. Mezzetto,arXiv:0905.2842 [hep-ph].
[5] [K2K], M.H. Ahn et al., Phys. Rev. D74, 072003 (2006).
[6] [Super-Kamiokande] Y. Ashie et al., Phys. Rev. D71, 112005 (2005).
[7] [K2K] S. Yamamoto et al., Phys. Rev. Lett. 96, 181801 (2006).
[8] [CHOOZ] M. Apollonio et al., Eur. Phys. J. C27, 331 (2003).
[9] [MINOS] P. Adamson et al., Phys. Rev. Lett. 101, 131802 (2008).
[10] [MINOS] P. Adamson et al., Phys. Rev. Lett. 101, 221804 (2008).
[11] M. Diwan,arXiv:0904.3706 [hep-ex].
[12] [OPERA] D. Duchesneau,arXiv:0810.2476 [hep-ex].
[13] [T2K] Y. Itow et al.,hep-ex/0106019.
[14] [NOvA] D.S. Ayres et al., FERMILAB-DESIGN-2007-01.
[15] H. Nunokawa, S.J. Parke, J.W.F. Valle, Prog. Part. Nucl. Phys. 60, 338
(2008).
[16] The NOvA Experiment at Fermilab,http://www-nova.fnal.gov
[17] Fermilab Steering Group Report,
http://www.fnal.gov/pub/directorate/steering/
[18] V. Barger et al.,arXiv:0705.4396 [hep-ph].
[19] K. Hagiwara, N. Okamura, K. Senda, Phys. Rev. D76, 093002 (2007).
[20] D. Autiero et al., JCAP 0711, 011 (2007).
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