NOνA

File:Nova far detector.png

Schematic of the NOνA far detector

NOνA (NuMI Off-Axis ν_e Appearance) is a particle physics experiment designed to detect neutrinos in Fermilab's NuMI (Neutrinos at the Main Injector) beam. Intended to be the successor to MINOS, NOνA will consist of two detectors, one at Fermilab (the near detector), and one in northern Minnesota (the far detector). Neutrinos from NuMI will pass through 810 km of Earth to reach the far detector. NOνA's main goal is to observe the oscillation of muon neutrinos to electron neutrinos. By observing how many neutrinos change from one type to the other, NOνA hopes to accomplish three things:

• Measurement of the mixing angle θ₁₃
• Measurement of the CP-violating phase δ
• Determination of the neutrino mass hierarchy

Physics goals

Primary goals

Neutrino oscillation is parameterized by the PMNS matrix and the mass squared differences between the neutrino mass eigenstates. Assuming that three flavors of neutrinos participate in neutrino mixing, there are six variables that affect neutrino oscillation: the three angles θ₁₂, θ₂₃, and θ₁₃, a CP-violating phase δ, and any two of the three mass squared differences. There is currently no compelling theoretical reason to expect any particular value of, or relationship between, these parameters.

θ₂₃ and θ₁₂ have been measured to be non-zero by several experiments but the most sensitive search for non-zero θ₁₃ by the CHOOZ collaboration yielded only an upper limit. More recently, in 2012, θ₁₃ was measured at Daya Bay to be non-zero to a statistical significance of 5.2σ. The following year, T2K discovered the transition $\nu_{\mu}\rightarrow\nu_{e}$ excluding the non-appearance hypothesis with a significance of 7.3σ. No measurement of δ has been made. The absolute values of two mass squared differences are known, but because one is very small compared to the other, the ordering of the masses has not been determined.

File:Nu e appearance for various delta.png

Oscillation probabilities, ignoring matter effects and assuming θ₁₃ is near the current limit. NOνA will observe the first peak.

NOνA will be an order of magnitude more sensitive to θ₁₃ than any previous detector. It will measure it by searching for the transition $\nu_{\mu}\rightarrow\nu_{e}$ in the Fermilab NuMI beam. If a non-zero value of θ₁₃ is resolvable by NOνA, it will be possible to obtain measurements of δ and the mass ordering by also observing $\bar{\nu}_{\mu}\rightarrow\bar{\nu}_{e}.$ δ can be measured because it modifies the probabilities of oscillation in opposite ways for neutrinos and anti-neutrinos. The mass ordering, similarly, can be determined because the neutrinos pass through the Earth, which, through the MSW effect, modifies the probabilities of oscillation differently for neutrinos and anti-neutrinos.

Importance

The neutrino masses and mixing angles are, to the best of our knowledge, fundamental constants of the universe. Measuring them is a basic requirement for our understanding of physics. Knowing the value of the CP violating parameter δ will help us understand why the universe has a matter-antimatter asymmetry. Also, according to the Seesaw mechanism theory, the very small masses of neutrinos may be related to very large masses of particles that we do not yet have the technology to study directly. Neutrino measurements are then an indirect way of studying physics at extremely high energies.

In our current theory of physics, there is no reason why the neutrino mixing angles should have any particular values. And yet, of the three neutrino mixing angles, only θ₁₂ has been resolved as being neither maximal or minimal. If the measurements of NOνA and other future experiments continue to show θ₂₃ as maximal and θ₁₃ as minimal, it may suggest some as yet unknown symmetry of nature.

Relationship to other experiments

NOνA can potentially resolve the mass hierarchy because it has a very long baseline. It is the only experiment likely to run in the near future that has this ability. Many future experiments that seek to make precision measurements of neutrino properties will rely on NOνA's measurement to know how to interpret their results.

An experiment similar to NOνA is T2K, a neutrino beam experiment in Japan similar to NOνA. Like NOνA, it is intended to measure θ₁₃ and δ. It will have a 295 km baseline and will use lower energy neutrinos than NOνA, about 0.6 GeV. Since matter effects are less pronounced both at lower energies and shorter baselines, it will be unable to resolve the mass ordering.

Neutrinoless double beta decay experiments will also benefit from knowing the mass ordering, since the mass hierarchy affects the theoretical lifetimes of this process.

Reactor experiments also have the ability to measure θ₁₃. While they cannot measure δ or the mass ordering, their measurement of the mixing angle is not dependent on knowledge of these parameters. One such experiment is Daya Bay, located at the Daya Bay reactor in southern China, which uses a 2 km baseline optimized for observation of the first θ₁₃-controlled oscillation maximum.

Secondary goals

In addition to its primary physics goals, NOνA will be able to improve upon the measurements of the already measured oscillation parameters. NOνA, like MINOS, is well suited to detecting muon neutrinos and so will be able to refine our knowledge of θ₂₃.

The NOνA near detector will be used to conduct measurements of neutrino interaction cross sections which are currently not known to a high degree of precision. Its measurements in this area will complement other similar upcoming experiments, such as MINERνA, which also uses the NuMI beam.

Since it is capable of detecting neutrinos from galactic supernovas, NOνA will form part of the Supernova Early Warning System. Supernova data from NOνA can be correlated with that from SuperKamiokande to study the matter effects on the oscillation of these neutrinos.

Design

Cross section of the earth showing Fermilab, MINOS and NOνA, to scale. The red line is the central axis of the NuMI beam.

To accomplish its physics goals, NOνA needs to be efficient at detecting electron neutrinos, which are expected to appear in the NuMI beam (originally made only of muon neutrinos) as the result of neutrino oscillation.

The proposed design is a pair of finely grained liquid scintillator detectors. The near detector will be at Fermilab and will sample the unoscillated beam. The far detector will be in northern Minnesota. The far detector will consist of about 500,000 4 cm × 6 cm × 16 m cells filled with liquid scintillator. Each cell will have a loop of bare fiber optic cable to collect the scintillation light, both ends of which lead to an avalanche photodiode for readout.

The near detector will have the same general design, but will only be about 1/200 as massive. This 200 ton detector is constructed from 6 blocks of 31 planes plus a muon catcher. The beam comes from the lower left in this diagram. The upstream 6 planes form a veto region (red). The next 108 planes are the fiducial region (green) with transverse containment indicated. The fiducial volume is followed by a 72 plane shower containment region (yellow). All parts of these three sections are fully active liquid scintillator cells identical to the far detector; the colored areas just represent a logical assignment. Downstream of this active region is a 1.7 meter long muon catcher region of steel interspersed with 10 active planes of liquid scintillator (black and white). Source

Previous neutrino experiments, such as MINOS, have reduced backgrounds from cosmic rays by being underground. However, NOνA will be on the surface and will rely on precise timing information and a well-defined beam energy to reduce backgrounds. It will be situated 810 km from the origin of the NuMI beam and 14 milliradians (12 km) west of the beam's central axis. In this position, it will sample a beam that has a much narrower energy distribution than if it were centrally located, further reducing the effect of backgrounds.

Collaboration

The NOνA experiment includes scientists from a large number of institutions. Different institutions take on different tasks. The collaboration, and subgroups thereof, meets regularly via phone for weekly meetings, and in person several times a year. Participating institutions as of April 2014 are:

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History

In late 2007, NOνA passed a Department of Energy review that grants it "Critical Decision 2", meaning roughly that its design, cost, schedule, and scientific goals have been approved. This also allows for inclusion of project in the Department of Energy congressional budget request. To begin construction, NOνA will still have to pass a "Critical Decision 3" review.

On 21 December 2007, President Bush signed an omnibus spending bill, H.R. 2764, that cut the funding for high energy physics by 88 million dollars from the expected value of 782 million dollars. The budget of Fermilab was cut by 52 million dollars. This bill explicitly states that "Within funding for Proton Accelerator-Based Physics, no funds are provided for the NOνA activity in Tevatron Complex Improvements." So although the NOνA project retained its approval from both the Department of Energy and Fermilab, the lack of funds provided by Congress for the 2008 fiscal year left NOνA with no capital to build its detector, pay its staff, or to continue in the pursuit of scientific results. However, in July 2008, Congress passed and the President Bush signed a supplemental budget bill, which includes funding for NOνA, allowing the collaboration to resume the work.

The NOvA prototype near detector (Near Detector on Surface - NDOS) began running at Fermilab in November and registered its first neutrinos from the NuMI beam on 15 December 2010. As a prototype, NDOS has served the collaboration well in establishing a use case that has provided improvements to design in the detector components that will be installed as a near detector at Fermilab, and a far detector at Ash River, MN ().

Once construction of the NOvA building completed, construction on the modules began. On July 26, 2012 the first module was laid in place. Placement and gluing of the modules will continued over a year until the detector hall was filled.

The first detection occurred on February 11, 2014 and construction completed in September that year. Full operation began in October 2014.

External links

• NOνA's official website
• "NOνA: a neutrino appearance experiment" article in Symmetry magazine
• Photos of the construction of the NOνA detector