1. NO A goals & physics NO A goals & physics NO A sites & detectors NO A sites & detectors NO A now & future NO A now & future

2. Jaroslav ZalesakFZU - Atlas seminar, 15. 6. 2012 2 Neutrino Mixing Matrix and Masses atmospheric  solar  Mixed Term Pontecorvo–Maki–Nakagawa–Sakata matrix

3. Jaroslav ZalesakFZU - Atlas seminar, 15. 6. 2012 3 Atmospheric: Solar: Neutrino Mixing Matrix and Masses solar  atmospheric  Mixed Term arXiv:1108.1376

4. Jaroslav ZalesakFZU - Atlas seminar, 15. 6. 2012 4 Neutrino Mixing Matrix and Masses atmospheric  solar  Mixed Term M. Messier (Indiana) sin 2 2θ 13  Daya Bay 0.092 ± 0.017 arXiv:1203.1669v2 [hep-ex]  RENO 0.113 ± 0.023 (revised) arXiv:1204.0626v2 [hep-ex]  Reactor Average 0.099 ± 0.014  Combined Average 0.092 ± 0.012

5. Jaroslav ZalesakFZU - Atlas seminar, 15. 6. 2012 5 Mass Hierarchy Currently the mass hierarchy is unknown

6. Jaroslav ZalesakFZU - Atlas seminar, 15. 6. 2012 6 NOA Collaboration 150+ scientists and engineers from 25 institutions, 5 countries ANL / Athens / Caltech / Institute of Physics ASCR / Charles University / FNAL / Harvard India Universities Consortium / Indiana / Iowa State / Lebedev / Michigan State Minnesota, Crookston / Minnesota, Duluth / Minnesota, Twin Cities / INR Moscow / South Carolina SMU / Stanford / Tennessee / Texas, Austin / Tufts / Virginia / WSU / William & Mary

7. Jaroslav ZalesakFZU - Atlas seminar, 15. 6. 2012 7 The NOA Experiment  Long baseline neutrino oscillation experiment:  Near (ND) and far (FD) detector  Off-axis in order to have a narrow neutrino flux with the energy peak is at 2GeV  810 km long baseline from Fermilab to Ash River, Minnesota.  Physics goals:  Search for ν μ →ν e oscillations.  precision measurements of |Δm 2 31 |, θ 23 octant  determine mass hierarchy.  constrain CP violating phase.  and more: cross sections, sterile, supernova, other exotics 810 km baseline NOvA Far Detector (Ash River, MN) MINOS Far Detector (Soudan, MN)

8. Jaroslav ZalesakFZU - Atlas seminar, 15. 6. 2012 8 Extracting Nature’s Parameters ≈ + ×  The NOνA baseline (L = 810 km) and neutrino beam energy (E = 2 GeV) place our detector at the first ν μ  ν e oscillation peak.  Extract the following terms by measuring the ν e appearance rate:  sin 2 2θ 13 : the leading term in this equation has already been measured and it is large!  sin 2 θ 23 : we can gleam information about the θ 23 octant from the leading term.  δ CP : using the measured value of θ 13, we can determine the CP-violating phase angle.  Mass hierarchy: depending on the sign of Δm 2 31 ~ Δm 2 32, the oscillation probability is either enhanced or suppressed. This difference can be determined by comparing neutrino running with anti-neutrino running (30% matter effect on oscillation). _ _ +

9. Jaroslav ZalesakFZU - Atlas seminar, 15. 6. 2012 9 Neutrino Landscape Forero, Tortola, Valle 2012 arXiv:1205.4018 Latest ν Oscillations Global fit:  Our knowledge of neutrino mixing has changed dramatically over the last year  We have gone from having no information on θ 13 to knowing that: θ 13 is large ≈9° θ 13 is the most precise neutrino measurements we have. The experimental picture for neutrino physics now shifts from trying to measure if θ 13 ≠ 0 to three general experimental thrusts: 1.Is δ≠0? Is there CP violation in the ν sector? 2.Is Δm 13 > 0? Is the neutrino mass hierarchy normal or inverted? 3.Make precision measurements of θ 23, θ 13, θ 12 Over constrain the standard mixing model to look for new physics. This has dramatically changed the experimental landscape & opened up new possibilities in the ν sector

10. Jaroslav ZalesakFZU - Atlas seminar, 15. 6. 2012 10 Off-axis beam target Decay Pipe ++  ND FD Placing detectors 14 mrad off the beam axis results in 2GeV narrow band beam with Eν width ≈20%. Close to the oscillation maximum.  The detector technology, geometry and baseline are then tuned to give:  L/E for 1 st Oscillation Maximum  Energy resolution for ν μ CC events ≈ 4%  High efficiency EM shower reconstruction in sub 2GeV region

11. Jaroslav ZalesakFZU - Atlas seminar, 15. 6. 2012 11 MagnetNear Detector Far Detector p 14.6 mrad νμνμ νμ/νeνμ/νe π+π+ NuMI Beamline NuMI Beam Target  NuMI: Neutrinos at the Main Injector  Beam delivered to several neutrino experiments since 2005  MINOS, MINERνA, and ArgoNeut  Beam shutdown: May 2012 – May 2013  upgrade beam: increase beam power from 300 kW to 700 kW (6 month rump-up) reduce cycle time from 2.2 s to 1.3 s upgrade graphite target and magnetic focusing horns  4.9e13 POT/pulse or 6e20 POT/year.  near detector cavern excavation

12. Jaroslav ZalesakFZU - Atlas seminar, 15. 6. 2012 12 NOA experiment sites Far Detector (15 kT) 2012-2014 Near Det Proto Det 2010 12  It includes:  Doubling of the Fermilab NuMI beam power to 700 kW  An 15kTon totally active surface detector, 14 mrad off axis at 810km Far detector (FD) (first oscillation max for 2GeV )  A 300 Ton totally active near detector Near detector (FD)  Prototype NDOS  Optimized as a segmented low Z highly-active tracking calorimeter :  Reconstruct EM showers  Measure muon tracks  Detect nuclear recoils and interaction vertices

13. To APD 4 cm ⨯ 6 cm 1560 cm Jaroslav ZalesakFZU - Atlas seminar, 15. 6. 2012 13 NOA Detectors 15.6 m 4.1 m Fiber pairs from 32 cells 32-pixel APD  Far detector: 14-kton, fine-grained, tracking calorimeter → 360,000 channels → 77% active by mass  Near detector:  Near detector: 0.3-kton version of the same → 18,000 channels cell Extruded PVC cells filled with 11M liters of scintillator instrumented with -shifting fiber and APDs

14. Jaroslav ZalesakFZU - Atlas seminar, 15. 6. 2012 14 Far Detector (FD) 15kT “Totally Active”, Low Z, Range Stack/Calorimeter Surface Detector Liquid Scintillator filled PVC 960 alternating X-Y planes Optimized for EM shower reconstruction & muon tracking, X 0 ≈40cm, R m ≈11cm Dims: 53x53x180ft “Largest Plastic Structure built by man” Began construction May 2012 First operation est. Sep. 2012 (cosmics) Near Detector (ND) Identical to far detector 1:4 scale size Underground Detector Optimized for NuMI cavern rates -- 4x sampling rate electronics …are BIG ! NOvA Detectors …

15. Jaroslav ZalesakFZU - Atlas seminar, 15. 6. 2012 15 Near Detector(s) at Fermilab  105 m underground:  beam is aimed downward  using MINOS near detector shaft  construction will start after cavern excavation  4 m × 4 m × 14 m  266 tons = 639 modules = 20,448 channels  On the surface:  prototype detector to test detector technology  Completed in May 2011  3 m × 4 m × 14 m  222 tons = 496 modules = 15,904 channels  successful running until beam shutdown in April

16. Jaroslav ZalesakFZU - Atlas seminar, 15. 6. 2012 16 NOνA Near Detector Prototype (NDOS)  The NOνA Prototype detector (NDOS) located on the surface at Fermilab.  Uses the same materials and technologies as the Near and Far detectors.  The NDOS is ~6.1 ̊ off the NuMI beam axis (120GeV) and on the Booster beam (8GeV)  Goals:  Testing assembly techniques for the Near and Far Detectors.  Installing, operating, testing the NOνA electronics and DAQ.  Developing reconstruction and calibration methods, and physics analyses & MC.  Can measure different neutrino fluxes, beam time structures, low energy detector response, quasi-elastic cross sections

17. The Detector Technology Jaroslav ZalesakFZU - Atlas seminar, 15. 6. 2012 17  Light is generated by charged particles and collected by wavelength-shifting fiber.  Each avalanche photodiode (APD) reads out 32 cells.  Each APD is connected to a Front End Board (FEB).  The FEB digitizes signal, sends it to a Data Concentrator Module (DCM).  Each DCM can read 64 FEBs. The NDOS uses 11 DCMs. 15.5m 6.6cm 3.9cm Particle Trajectory Scintillation Light Wavelength shifting Fiber Loop To APD Readout

18. Avalanche photo-diode (APD) Jaroslav ZalesakFZU - Atlas seminar, 15. 6. 2012 18 Relatively inexpensive (about $10 per channel) 85% QE for 520 – 550 nm light. Gain of 100 @ 375 volts. Array of 32 pixels Actively cooled to -15 o C. 11,150 APDs at the Far detector NOνA Detection Cell The base detector unit 3.9x6.6cm cell 15.5m long, filled with a mineral oil based liquid scintillator. Passage of MIP through the cell (longitudinal to beam) results in dE/dx ≈12.9 MeV across the cell.  Roughly 10% of energy loss is in the PVC wall  Yields 10-12MeV of deposition in the scint. The measured light output is 30-38 p.e. from the far end of the cell into the APD readout Light yield gives a minimum Sig/Noise 10:1 (far end) Signal is amplified and shaped Channel is continuously sampled at 2MHz to obtain wave form Zero suppression is performed at (0.5-0.66) MIP (15-20 p.e.) via a dual correlated sampling (dcs) algorithm Results in a single cell, lower energy detection threshold of ≈6-8MeV (far end) Fits to the shape of the waveform recover the timing and pulse height information

19. Front-end-board (FEB) Jaroslav ZalesakFZU - Atlas seminar, 15. 6. 2012 19  Low noise ASIC amplifier is developed to maximize the sensitivity to small signals from the fiber.  Analog-to-Digital converter samples each pixel with a frequency of 2 MHz (8 MHz at the Near Detector)  Field Programmable Gate Array preselects “hits” and sends the readout information to DAQ.  Thermo Electric Cooler Controller controls the amount of drive current to supply for a Thermo Electric Cooler installed on the APD module. ASIC signal output as a function of time

20. Jaroslav ZalesakFZU - Atlas seminar, 15. 6. 2012 20 Construction Schedule  NOvA will turn on April 2013 with 5 kton of Far detector in place and beam operating at about 400 kW.  We will add detector mass at a rate of ~ 1 kton/month.  Beam intensity will ramp up to 700 kW in approximately 6 months. Far Detector at 5 kton when beam returns Six months to 700 kW NuMI 14 kton in May 2014 Evolution of detector mass and beam power…

21. Prototype Near Detector (2010-2012) Jaroslav ZalesakFZU - Atlas seminar, 15. 6. 2012 21 Designed for: Running 2010-Present Component installation, testing and integration, DAQ & readout development Calibration, reconstruction and background studies Flux and cross section measurements

22. Far Detector Building – Complete Jaroslav ZalesakFZU - Atlas seminar, 15. 6. 2012 22

23. Inside the Hall (looking south) Jaroslav ZalesakFZU - Atlas seminar, 15. 6. 2012 23

24. With the block pivoter Jaroslav ZalesakFZU - Atlas seminar, 15. 6. 2012 24

25. Simulated Event Signatures Jaroslav ZalesakFZU - Atlas seminar, 15. 6. 2012 25 ν μ charged-current long, well-defined muon track short proton track with large energy deposition at end ν e charged-current single EM shower characteristic EM shower development neutral-current with π 0 final state multiple displaced EM showers possible gaps near event vertex

26. NDOS: Cosmic Ray Muon Data Jaroslav ZalesakFZU - Atlas seminar, 15. 6. 2012 26  Reconstructed cosmic ray muons are used for calibration and commissioning.  Efficiency of cosmic tracker: >98%.

27. NDOS: Neutrino Candidate Jaroslav ZalesakFZU - Atlas seminar, 15. 6. 2012 27

28. Events in NDOS Jaroslav ZalesakFZU - Atlas seminar, 15. 6. 2012 28 Neutrino & cosmic ray @ NDOS  Develop commissioning, calibration, reconstruction, and analysis tools coincident cosmic ray NuMI neutrino interaction Neutrino events in beam direction

29. Neutrino event distributions Jaroslav ZalesakFZU - Atlas seminar, 15. 6. 2012 29 NuMI neutrino events at NDOS  Two example distributions: angle of primary track w.r.t. the neutrino beam, and total visible energy [in photoelectrons]  Monte Carlo simulation agrees well with observations

30. Estimated ν e Appearance Signal Jaroslav ZalesakFZU - Atlas seminar, 15. 6. 2012 30  The large θ 13 is extremely good for NOvA since it leads to large event rates in the far detector and enhancing early sensitivities. The following sensitivities use our earlier analysis approaches but include the latest knowledge of θ 13 :  Sin 2 2θ 13 =0.095  Optimized for ∼ 4% oscillation probability  10% uncertainty on backgrounds  41% (ν) and 48% (anti-ν) signal efficiency Estimated numbers based on: 15 kton, 18 x 10 20 POT (3 years each neutrino-mode running) No solar-atmospheric terms and no matter effects

31. Early Reach Jaroslav ZalesakFZU - Atlas seminar, 15. 6. 2012 31 Will start with running Can switch to ͞ any time, optimizing the run plan based on our or others’ results  5 observation of → e in first year if NH (even with partial detector and beam commissioning!) … and beyond  Nominal run plan: 3 yr () + 3 yr ( ͞ ) (with 6×10 20 p.o.t./year ) NC CC e CC tot. BG → e 19 5 8 32 68 10 <1 5 15 32 ͞ beam =

32. NOA measurement principle Jaroslav ZalesakFZU - Atlas seminar, 15. 6. 2012 32 NOA will measure: P( → e ) at 2 GeV P( ͞ →͞ e ) at 2 GeV & These depend in different ways on the CP phase and on sign(  m 2 ). Appearance probabilities are plotted as: P( ͞ e ) vs. P( e ) for all and both hierarchies [ assuming: sin2(213)=0.095, sin2(223)=1 ]

33. NOA measurement principle Jaroslav ZalesakFZU - Atlas seminar, 15. 6. 2012 33 Example NOA result… P( → e ) at 2 GeV P( ͞ →͞ e ) at 2 GeV & Data will yield allowed regions in P( ͞ e ) vs. P( e ) space (3 yr + 3 yr possibility shown) Here, all inverted hierarchy scenarios are excluded at >2

34. sin 2 (2 23 ) ≠ 1 ? (non maximal) Jaroslav ZalesakFZU - Atlas seminar, 15. 6. 2012 34 sin 2 (2) |  m 2 | (10 -3 eV 2 ) Example NOA contours for three test points sin 2 (2 23 ) = 1 sin 2 (2 23 ) = 0.94 4% energy resolution for the QE sample. Inclusive CC sample should be background-free

35. Jaroslav ZalesakFZU - Atlas seminar, 15. 6. 2012 35 23 octant sensitivity P( e ) ∝ sin 2 ( 23 )sin 2 (2 13 ) Expected NOA contours for one example scenario at 3 yr + 3 yr e e 3 ? 23 > 45 ° 23 < 45 ° Simultaneous hierarchy, CP phase & 23 octant information from NOA Θ 23 =45°

36. Mass Hierarchy resolution Jaroslav ZalesakFZU - Atlas seminar, 15. 6. 2012 36 Including T2K information  In T2K, P( → e ) has dependence but comparatively little hierarchy dependence (shorter baseline).  When CPv and matter effects cancel in NOA, the NOA + T2K combination helps. range included for given significance of hierarchy determination (  m 2 > 0 case) range included for given significance of hierarchy determination (  m 2 > 0 case)

37. Summary Jaroslav ZalesakFZU - Atlas seminar, 15. 6. 2012 37  NOA FD assembly underway at Ash River!  NuMI upgrades underway → 700 kW  First neutrino events in the partial FD next Spring  NDOS run: → commissioning, cosmic ray, and neutrino data → invaluable for assembly practice and analysis development  Actively developing analyses for 1 st FD data → aiming to surpass the sensitivities shown  The observed 13 is great for NOA program → mass hierarchy, CP, 23 → broad range of -sector measurements Far Detector Hall

38. Jaroslav ZalesakFZU - Atlas seminar, 15. 6. 2012 38 END

39. NOνA Measurements Jaroslav ZalesakFZU - Atlas seminar, 15. 6. 2012 39  The transition probability is dependent on θ 13,θ 23,δ CP and Δm 31  The reactor measurements do not have the these dependencies  NOvA measures P( → e ) & P( ͞ →͞ e ) over an 810 km baseline at a central energy of 2GeV.