NOvA


The NOA experiment is a particle physics experiment designed to detect neutrinos in Fermilab's NuMI beam. Intended to be the successor to MINOS, NOA consists of two detectors, one at Fermilab, and one in northern Minnesota. Neutrinos from NuMI pass through 810 km of Earth to reach the far detector. NOA's main goal is to observe the oscillation of muon neutrinos to electron neutrinos. The primary physics goals of NOvA are:
  • Precise measurement, for neutrinos and antineutrinos, of the mixing angle, especially whether it is larger than, smaller than, or equal to 45°
  • Precise measurement, for neutrinos and antineutrinos, of the associated mass splitting
  • Strong constraints on the CP-violating
  • Strong constraints on 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,, and, a CP-violating phase, 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.
and have been measured to be non-zero by several experiments but the most sensitive search for non-zero by the Chooz collaboration yielded only an upper limit. In 2012, was measured at Daya Bay to be non-zero to a statistical significance of The following year, T2K discovered the transition excluding the non-appearance hypothesis with a significance of No measurement of 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.
Image:Nu e appearance for various delta.png|thumb|Oscillation probabilities, ignoring matter effects and assuming is near the current limit. NOA will observe the first peak.
NOA is an order of magnitude more sensitive to than the previous generation of experiments, such as MINOS. It will measure it by searching for the transition in the Fermilab NuMI beam. If a non-zero value of is resolvable by NOA, it will be possible to obtain measurements of and the mass ordering by also observing The parameter can be measured because it modifies the probabilities of oscillation differently 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 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 has been resolved as being neither maximal or minimal. If the measurements of NOA and other future experiments continue to show as maximal and as minimal, it may suggest some as yet unknown symmetry of nature.

Relationship to other experiments

NOA can potentially resolve the mass hierarchy because it operates at a relatively high energy. Of the experiments currently running it has the broadest scope for making this measurement unambiguously with least dependence on the value of. Many future experiments that seek to make precision measurements of neutrino properties will rely on NOνA's measurement to know how to configure their apparatus for greatest accuracy, and how to interpret their results.
An experiment similar to NOA is T2K, a neutrino beam experiment in Japan similar to NOA. Like NOA, it is intended to measure and. It will have a 295 km baseline and will use lower energy neutrinos than NOA, about 0.6 GeV. Since matter effects are less pronounced both at lower energies and shorter baselines, it is unable to resolve the mass ordering for the majority of possible values of.
The interpretation of 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. While they cannot measure or the mass ordering, their measurement of the mixing angle is not dependent on knowledge of these parameters. The three experiments that have measured a value for, in deceasing order of sensitivity are Daya Bay in China, RENO in South Korea and Double Chooz in France, which use 1–2 km baselines, optimized for observation of the first oscillation maximum.

Secondary goals

In addition to its primary physics goals, NOA will be able to improve upon the measurements of the already measured oscillation parameters. NOA, like MINOS, is well suited to detecting muon neutrinos and so will be able to refine our knowledge of.
The NOA near detector is 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 complement other similar upcoming experiments, such as MINERA, which also uses the NuMI beam.
Since it is capable of detecting neutrinos from galactic supernovas, NOA is part of the Supernova Early Warning System. Supernova data from NOA can be correlated with that from Super-Kamiokande to study the matter effects on the oscillation of these neutrinos.

Design

To accomplish its physics goals, NOA needs to be efficient at detecting electron neutrinos, which are expected to appear in the NuMI beam as the result of neutrino oscillation.
Image:Cross section of earth showing numi beam, minos and nova.png|thumb|Cross section of the earth showing Fermilab, MINOS and NOA, to scale. The red line is the central axis of the NuMI beam.
Previous neutrino experiments, such as MINOS, have reduced backgrounds from cosmic rays by being underground. However, NOA is on the surface and relies on precise timing information and a well-defined beam energy to reduce spurious background counts. It is situated 810 km from the origin of the NuMI beam and 14 milliradians west of the beam's central axis. In this position, it samples a beam that has a much narrower energy distribution than if it were centrally located, further reducing the effect of backgrounds.
The detector is designed as a pair of finely grained liquid scintillator detectors. The near detector is at Fermilab and samples the unoscillated beam. The far detector is in northern Minnesota, and consists of about 500,000 cells, each 4 cm × 6 cm × 16 m, filled with liquid scintillator. Scintillation light is captured by optical fibers made of wavelength shifter, both ends of which lead to an avalanche photodiode for readout.
The near detector has the same general design, but is only about as massive. This 222 ton detector is constructed of 186 planes of scintillator-filled cells followed by a muon catcher. Although all the planes are identical, the first 6 are used as a veto region; particle showers which begin in them are assumed to not be neutrinos and ignored. The next 108 planes serve as the fiducial region; particle showers beginning in them are neutrino interactions of interest. The final 72 planes are a "shower containment region" which observe the trailing portion of particle showers which began in the fiducial region. Finally, a 1.7 meter long "muon catcher" region is constructed of steel plates interleaved with 10 active planes of liquid scintillator.

Collaboration

The NOA 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 May 2024 are:

Funding history

In late 2007, NOA passed a Department of Energy "Critical Decision 2" review, meaning roughly that its design, cost, schedule, and scientific goals had been approved. This also allowed the project to be included in the Department of Energy congressional budget request.
On 21 December 2007, President Bush signed an omnibus spending bill, H.R. 2764, which 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 stated that "Within funding for Proton Accelerator-Based Physics, no funds are provided for the NOA activity in Tevatron Complex Improvements." So although the NOA project retained its approval from both the Department of Energy and Fermilab, Congress left NOA with no funds for the 2008 fiscal year 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 signed, a supplemental budget bill, which included funding for NOA, allowing the collaboration to resume its work.
The NOA prototype near detector began running at Fermilab in November and registered its first neutrinos from the NuMI beam on 15 December 2010. As a prototype, NDOS served the collaboration well in establishing a use case and suggesting improvements in the design of detector components that were later installed as a near detector at Fermilab, and a far detector at Ash River, MN.
Once construction of the NOA building was complete, construction of the detector modules began. On 26 July 2012 the first module was laid in place. Placement and gluing of the modules continued over a year until the detector hall was filled.
The first detection occurred on 11 February 2014 and construction completed in September that year. Full operation began in October 2014.