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005-numi-tunes
The locations of the target and second horn in the low (LE), medium (ME), and high (HE) energy NuMI tunes. MINOS currently runs in the LE configuration. The optimal NOvA configuration is to place the target at z=-1.4 meters and the second horn at z=19 meters which is close to the MINOS ME configuration shown above.Part of the NuMI upgrades for NOvA is to move the second horn downstream.
Contact: Mark Messier
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010-minos-spectra
The neutrino spectra (flux times total cross-section) produced at the MINOS far detector site for the different NuMI tunes.
Contact: Mark Messier
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020-flux
The total neutrino flux at a given angle as a function of parent pion energy. The NOvA site is at 14 mrad.
Contact: Mark Messier
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030-epi2enu
The energy of neutrinos produced at various angles as a function of parent pion energy. At 14 mrad essentially all pion decays yield neutrinos in the 1-2 GeV energy range of interest for oscillations, compensating for the decrease in flux.
Contact: Mark Messier
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040-le-spectra
The neutrino spectra (flux time cross-section) for various angles for NuMI in the LE tune. The NOvA detectors will be at 14 mrad, although we prefer the ME tune (next plot).
Contact: Mark Messier
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050-me-spectra
The neutrino spectra (flux times cross-section) for various angles in the ME NuMI tune. The 14 mrad ME tune shown in red is optimal for NOvA physics.
Contact: Mark Messier
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060-sig-and-bg-rates
Raw signal and background rates for the NOvA site (L=810 km, theta=14 mrad). The muon neutrino rates are shown with (green dotted) and without (green solid) oscillations applied. The NC rates are shown as a function of the visible energy (=neutrino energy * y) and hence pile up at low energies. The blue curve shows the intrinsic beam nue component. The red bump is a signal at the CHOOZ limit. A detector placed in this beam must be able to reject the numuCC, and NC events at a level to make the red signal bump detectable. Energy resolution helps to reduce the beam nue backgrounds.
Contact: Mark Messier
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070-ipnd-numu
The charged-current muon neutrino spectrum in the MINOS surface
building for the LE NuMI beam tune. At this location the IPND is
expected to collect 2840 numu-CC events in the region between 1.6 and
2.4 GeV in one year of NuMI operation. Likewise, the IPND should see
roughly 1100 NC events in the 1.6-2.5 GeV region. Contact: Mark
Messier
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080-ipnd-nue
The charged-current electron neutrino spectrum in the MINOS surface
building for the LE NuMI beam tune. At this location the IPND is
expected to collect 170 nue-CC events in the region between 1.6 and
2.4 GeV in one year of NuMI operation. Contact: Mark Messier
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010-thetalPP
2-sigma sensitivity of the NOvA experiment to see muon to electron
neutrino oscillations. The blue curves assume normal mass hierarchy
while the red curves show the inverted hierarchy case. The sensitivity
is calculated assuming a 15 kT detector, 10% systematic error on the
backgrounds, and 6 years of running split evenly between neutrino and
anti-neutrino horn polarities. In addition to the baseline 700 kW beam
power ("ANU"), the possibilities using 1.2 MW ("SNuMI") and 2.3 MW
("Project X") are also shown.
Contact: Gary Feldman
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020-thetalpp90
Same as previous plot, but shows the 90% C.L. sensitivity as this is
more commonly shown by other collaborations.
Contact: Gary Feldman
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030-f810_24_02
This plot demonstrates the principle by which NOvA determines the mass
hierarchy and measures the CP phase. NOvA essentially measures two
oscillation probabilities, one in neutrino mode and one in
anti-neutrino mode. For this plot it is assumed that the measurement
in neutrino mode has yielded a numu-nue oscillation probability of
0.02. The two ellipses show all the possibilities of theta_13 values,
delta_cp values, and choice of hierarchy that could yield this
measurement. The blue curve is for the normal hierarchy case and the
red curve is for the inverted hierarchy case. On each ellipse, the
choice of the CP phase delta varies as one moves around the ellipse as
indicated by the symbols. One can imagine that NOvA makes a
measurement of oscillation probability in anti-neutrino mode and
locate that point on the x-axis. Scanning vertically upward from that
point until one hits the curves will indicate which choice of
parameters are consistent with the two measurements. If the scan hits
only a red or blue curve, the mass hierarchy is resolved. If one hits
both red and blue curves the ambiguity of the choice of hierarchy and
CP phase remains unresolved.
Contact: Gary Feldman
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040-massnlPP
For oscillation parameters to right of these curves, NOvA resolves the neutrino mass hierarchy with better then 95% C.L. The curves are calculated for a 15 kT detector, 6 years of running split evenly between neutrino and anti-neutrino horn polarities. Intensities of the baseline 700 kW and possible further upgrades to 1.2 MW and 2.3 MW are also shown. The plot assumes nature has a normal mass hierarchy.
Contact: Gary Feldman
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050-massilPP
Same as previous plot, but calculated assuming nature has an inverted hierarchy.
Contact: Gary Feldman
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060-massnlPPT2K
For parameters to the right of the curves, the combination of NOvA and T2K resolves the neutrino mass hierarchy at 95% C.L or better. The calculation assumes nature has a normal hierarchy. In the region delta_CP > pi, NOvA resolves the hierarchy on its own through a comparison of its measurements using neutrino and anti-neutrinos. For the region where delta_CP < pi, the comparison of T2K's measurement using neutrinos at the first oscillation maximum which is little affected by matter effects and NOvA's measurement at the first oscillation maximum using neutrinos which is strongly affected by matter effects helps break the ambiguity in the comparison of NOvA's neutrino measurement to its anti-neutrino measurement. |
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070-massilPPT2K
Same as previous plot but for the case of the inverted hierarchy.
Contact: Gary Feldman
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080-contourNOvA15
The 1- and 2-sigma measurement contours for NOvA assuming oscillations with parameters chosen at the starred point. The hierarchy is resolved (the small red contour is the "ghost" solution assuming the inverted hierarchy) and the CP phase is constrained to the upper half plane.
Contact: Gary Feldman
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090-contourNOvA3
The 1- and 2-sigma measurement contours for NOvA assuming oscillations with parameters chosen at the starred point. The CP phase is constrained to the upper half plane. The hierarchy is nor determined as the ghost solution (shown in red) for the inverted hierarchy appears at 1-sigma.
Contact: Gary Feldman
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100-contourNOvA
The 1- and 2-sigma measurement contours for NOvA assuming oscillations with parameters chosen at the starred point. In this case, the hierarchy is not resolved as the ghost solutions for the inverted hierarchy (red) appear at 1-sigma. The ambiguity in the hierarchy choice means that the CP phase is left unconstrained.
Contact: Gary Feldman
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110-contourT2K
An estimate of the results from T2K for the starred point. No information on the CP phase or the hierarchy is obtained. However, one can compare to the NOvA case in the previous plot. The contours overlap in the region near the correct solution but miss in the upper half plane. So one expects the combination of NOvA and T2K to be useful in this part of the parameter space.
Contact: Gary Feldman
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120-contourNOvAT2K
The 1- and 2-sigma measurement contours combining NOvA and T2K. As one can see by comparison to the previous two plots the combination of NOvA and T2K has considerably more power in this part of the parameter space than either one does alone.
Contact: Gary Feldman
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130-contourNOvAt2K3
The 1- and 2-sigma contours for the combination of T2K and NOvA for the starred point. In this case, upgrades to both the T2K and NOvA intensities have been assumed. The hierarchy is resolved and the CP phase is constrained to the lower half plane.
Contact: Gary Feldman
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010-nus-spectrum-sum
The reconstructed shower energy spectrum for NC-like events. The results for 3 years of neutrino running are summed with results from 3 years of anti-neutrino running. The dashed histogram shows thee spectrum calculated at the 90% preliminary SK limit on sterile content. NOvA should push this limit about another factor of 2 further.
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020-nus-spectrum-nu
NC spectrum for 3-year neutrino run.
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030-nus-spectrum-antinu
NC-like spectrum for a 3-year anti-neutrino run.
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035-nus-annpid
Output of neutral-net particle ID parameter trained to identify NC
events. The points show the total NC-like sample, the dashed histogram
is the true NC event sample, the blue is the numu-CC sample and the
pink dashed curve is the nue-CC event sample. Plot was made for
neutrino beam focus.
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040-nus-event-table
Summary of event rates in the nu-sterile analysis after 3 stages of event selection. Final purity of the NC-like sample is 91%. The left-most column is the total number of NC-like events and the three right columns break the total down by event type. Numbers assume a three-year neutrino run at 700 kW.
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050-nus-sensitivity
Sensitivity to numu-nus oscillations assuming 5% uncertainty on
backgrounds. The top curve assumes only statistical errors, the bottom
includes 5% systematic on backgrounds. The 90% CL limits are <6.4%
sterile content (stat. only) and <11.8% (stat. + syst.).
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![[jpg]](015_Detector_Overview/006-nova-soilderfield.jpg){kind=link}