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F Axis The NO A Experiment: Phase 2 of the Fermilab NuMI Program Workshop on Physics with Atmospheric Neutrinos and Neutrinos from Muon Storage Rings Maury.

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Presentation on theme: "F Axis The NO A Experiment: Phase 2 of the Fermilab NuMI Program Workshop on Physics with Atmospheric Neutrinos and Neutrinos from Muon Storage Rings Maury."— Presentation transcript:

1 f Axis The NO A Experiment: Phase 2 of the Fermilab NuMI Program Workshop on Physics with Atmospheric Neutrinos and Neutrinos from Muon Storage Rings Maury Goodman, Argonne National Lab (most slides courtesy of Gary Feldman, Harvard)

2 Maury Goodman IIT Mumbai 1-2 August 2005 2 The NO A Experiment (NuMI Off-Axis e Appearance Experiment) NO A is an approved Fermilab experiment optimized for measuring e appearance with the goal of improving the sensitivity to  13 from the current CHOOZ limit by more than a factor of 20. The NO A far detector will be l a 30 kT “totally active” liquid scintillator detector l located 15 mrad (12 km) off the NuMI beamline axis near Ash River, NM, 810 km from Fermilab The uniqueness of NO A is the long baseline, which is necessary for determining the mass ordering of the neutrino states.

3 Maury Goodman IIT Mumbai 1-2 August 2005 3 2004 APS  study  One of (two) high priority recommendations is for a concerted program to measure  13 including:  A reactor experiment  An accelerator experiment (with NO A in mind).

4 Maury Goodman IIT Mumbai 1-2 August 2005 4

5 Maury Goodman IIT Mumbai 1-2 August 2005 5 Ash River; 810 km 200 x 40 m labs shown

6 Maury Goodman IIT Mumbai 1-2 August 2005 6 P(   e ) (in Vacuum) P(   e ) = P 1 + P 2 + P 3 + P 4 P 1 = sin 2 (  23 ) sin 2 (2  13 ) sin 2 (1.27  m 13 2 L/E) “Atmospheric” P 2 = cos 2 (  23 ) sin 2 (2  12 ) sin 2 (1.27  m 12 2 L/E) “Solar” P 3 = J sin(  ) sin(1.27  m 13 2 L/E) P 4 = J cos(  ) cos(1.27  m 13 2 L/E) where J = cos(  13 ) sin (2  12 ) sin (2  13 ) sin (2  23 ) x sin (1.27  m 13 2 L/E) sin (1.27  m 12 2 L/E) Atmospheric- solar interference

7 Maury Goodman IIT Mumbai 1-2 August 2005 7 P(ν μ → ν e ) (in Matter) l In matter at oscillation maximum, P 1 will be approximately multiplied by (1 ± 2E/E R ) and P 3 and P 4 will be approximately multiplied by (1 ± E/E R ), where the top sign is for neutrinos with normal mass hierarchy and antineutrinos with inverted mass hierarchy l About ±30% effect for NuMI l About ±11% effect for T2K l The effect is reduced for energies above the oscillation maximum & increased for energies below

8 Maury Goodman IIT Mumbai 1-2 August 2005 8 Off-Axis Rationale Both Phase 2 experiments, NO A and T2K are sited off the neutrino beam axis. This yields a narrow band beam: More flux and less background ( e ’s from K decay and higher- energy NC events)

9 Maury Goodman IIT Mumbai 1-2 August 2005 9 NO A Far Detector “Totally Active” 30 kT: 24 kT liquid scintillator 6 kT PVC 32 cells/extrusion 12 extrusions/plane 1984 planes Cell dimensions: 3.9 cm x 6 cm x 15.7m (0.15 X 0 thickness) Extrusion walls: 3 mm outer 2 mm inner U-shaped 0.8 mm WLS fiber into APD 132 m 15.7m 32-plane block Admirer

10 Maury Goodman IIT Mumbai 1-2 August 2005 10 30 kton NO A detector

11 Maury Goodman IIT Mumbai 1-2 August 2005 11 Light collection

12 Maury Goodman IIT Mumbai 1-2 August 2005 12 Far Detector Assembly One 8-plane sub-block assembled per day Detector has 248 sub- blocks 8-plane sub-block 32-plane block 1-cm expan- sion gap 32-plane block

13 Maury Goodman IIT Mumbai 1-2 August 2005 13 Half-scale NO A Prototype in Bldg 366 l Unprecedented plastic structure of this scale l Measure mechanical properties l Compare to FEA calculations l Try out assembly procedures l Mounting/gluing tests

14 Maury Goodman IIT Mumbai 1-2 August 2005 14 Structural Analysis l Rigid PVC l ASTM D1784 “Standard Specification for Rigid PVC Compounds” Defines 6 grades with allowable design stresses from 1000 PSI to 2000 PSI l NOvA design working limit of 1500 PSI Well before creep onset l Good resistance to catastrophic failure Creep before crack l FEA model l Results baselined with bench tests l Maximum internal stress of 1400 PSI for vertical cell from hydrostatic pressure l Maximum transferred stress of 560 PSI for horizontal to vertical cells 70 PSI in sheer l Safety factor of 2.9 for buckling l 10C temperature change Force generated of 4.3 PSI Length of detector increased by 9cm Include expansion gaps between blocks

15 Maury Goodman IIT Mumbai 1-2 August 2005 15 Near Detector 5 m 3.5 m 9.6 m Veto region Target region Shower containment region Muon catcher 1 m iron 262 T 145 T totally active 20.4 T fiducial (central 2.5 x 3.25 m) 8-plane block 10.6 T full 1.6 T empty

16 Maury Goodman IIT Mumbai 1-2 August 2005 16 Near Detector in MINOS Surface Building 45,000   CC events2,200 e CC events 6.5 x 10 20 pot in 75 mrad off-axis beam Kaon peak

17 Maury Goodman IIT Mumbai 1-2 August 2005 17 1.87 GeV e N  ep  +  0 x-z View Accepted

18 Maury Goodman IIT Mumbai 1-2 August 2005 18 2.11 GeV  N   p  0 x-z View Accepted!

19 Maury Goodman IIT Mumbai 1-2 August 2005 19 1.86 GeV e N  ep  + x-z View Not accepted

20 Maury Goodman IIT Mumbai 1-2 August 2005 20 Electron ID & Energy Resolution Electrons Muons Electron resolution Also use RMS of pulse height per plane, gaps & energy cuts

21 Maury Goodman IIT Mumbai 1-2 August 2005 21 Post-Collider Proton Plan l Proton Plan with Collider l 9/11 Slip-stacked Booster batches at 5.5  10 12 p/batch l Repetition rate = 0.8 s (Booster) + 1.4 s (Ramp) = 2.2 s l 10% for Collider shot setup + 5% for antiproton transfer l  3.4  10 20 protons/yr l Post-Collider Proton Plan l 11 batches for neutrinos  11/9 = 1.22 factor l Hide Booster filling time in Recycler  0.8 s  0.067 s  2.2 s  1.467 s = 1.50 factor l Save 10% shot setup and 5% antiproton transfer = 1.17 factor l  (3.4  10 20 protons/yr)(1.22)(1.50)(1.17) = (7.3  10 20 protons/yr) l Negotiated rate is 90% of this: (6.5  10 20 protons/yr) l Proton Driver rate taken as 25  10 20 protons/yr

22 Maury Goodman IIT Mumbai 1-2 August 2005 22 Parameters Consistent with a 2%   e Oscillation

23 Maury Goodman IIT Mumbai 1-2 August 2005 23 Parameters Consistent with Other Oscillation Probabilities

24 Maury Goodman IIT Mumbai 1-2 August 2005 24 3  Sensitivity to  13  0 5 year only run

25 Maury Goodman IIT Mumbai 1-2 August 2005 25 3  Sensitivity to  13  0

26 Maury Goodman IIT Mumbai 1-2 August 2005 26 3  Sensitivity to  13  0  Comparison with Proton Driver

27 Maury Goodman IIT Mumbai 1-2 August 2005 27 Importance of the Mass Ordering l Window on very high energy scales: grand unified theories favor the normal mass ordering, but other approaches favor the inverted ordering. l If we establish the inverted ordering, then the next generation of neutrinoless double beta decay experiment can decide whether the neutrino is its own antiparticle. However, if the normal ordering is established, a negative result from these experiments will be inconclusive. l To measure CP violation, we need to resolve the mass ordering, since it contributes an apparent CP violation that we must correct for.

28 Maury Goodman IIT Mumbai 1-2 August 2005 28 Role of NO A in Resolving the Mass Ordering l The mass ordering can be resolved only by matter effects in the earth over long baselines. NO A is the only proposed experiment with a sufficiently long baseline to resolve the mass ordering. The siting of NO A is optimized for this measurement. NO A is the first step in a step-by-step program that can resolve the mass ordering in the region accessible to conventional neutrino beams.

29 Maury Goodman IIT Mumbai 1-2 August 2005 29 95% CL Resolution of the Mass Ordering

30 Maury Goodman IIT Mumbai 1-2 August 2005 30 95% CL Resolution of the Mass Ordering

31 Maury Goodman IIT Mumbai 1-2 August 2005 31 95% CL Resolution of the Mass Ordering Scenario: 2 years into the PD run, realize the need for the 2nd off-axis detector. Build in 4 years, run for 6 years. Thus, 12 years running of NO A with PD and 6 years of running the second detector. Several technologies possible for the 2nd detector. Use SK as a model for the calculation.

32 Maury Goodman IIT Mumbai 1-2 August 2005 32 Other Physics Better  m 2 31 & sin 2 2  23 l Study a possible MiniBooNE signal l Supernova

33 Maury Goodman IIT Mumbai 1-2 August 2005 33 Cost ContingencyTotal Cost M$ Far Detector Active detector30% 79.5 Electronics and DAQ55% 13.4 Shipping21% 7.0 Installation43% 13.5 Near Detector44% 3.1 Building and outfitting58% 29.3 Project management25% 4.7 Additional contingency 14.1 Total50%164.7

34 Maury Goodman IIT Mumbai 1-2 August 2005 34 Schedule (10 of 29 Milestones) Project startOct 2006 R&D prototype Near Detector completeMar 2007 Start Far Detector Building constructionJul 2007 Start receiving packaged APDsOct 2007 Start extrusion module factoriesOct 2007 Start construction of Near DetectorDec 2007 Start operation of Near DetectorJul 2008 Start Far Detector assemblyMay 2009 First kiloton operationalOct 2009 Full 30 kilotons operationalJul 2011

35 Maury Goodman IIT Mumbai 1-2 August 2005 35 NO A Status l Approved by Fermilab April 2005: Letter from Mike Witherell l “The Committee found that NO A …is the best approach to address the compelling neutrino physics questions ahead of us. They judged NO A to be well designed, fully competitive, and complementary to other efforts. They also consider it to be the right platform for further steps in the evolving neutrino program worldwide. The Committee recommended Stage I approval.” l “Organizing the best program of neutrino research with Fermilab’s accelerators is critical to the strength of the particle physics program in the US and worldwide. I agree with the Committee’s judgment that NO A is the right experiment to anchor this program, and I agree that now is the time to act. I therefore grant Stage I approval to the NO A experiment.”

36 Maury Goodman IIT Mumbai 1-2 August 2005 36 NO A Status l Approved by Fermilab April 2005 (see letter) l Ed Temple has set out a schedule of critical decisions and reviews that will allow a Oct 2006 construction start (see timeline)

37 Maury Goodman IIT Mumbai 1-2 August 2005 37 Sensitivity vs. Time

38 Maury Goodman IIT Mumbai 1-2 August 2005 38 Conclusion NO A provides a flexible approach to studying all of the parameters of neutrino oscillations l A long baseline approach is crucial in the context of the world program. NO A is the first stage of a flexible program where each stage can be planned according to what has been learned in previous stages. The NO A physics reach is greater than other experiments being contemplated for the next few years.

39 Maury Goodman IIT Mumbai 1-2 August 2005 39 Backup Slides

40 Maury Goodman IIT Mumbai 1-2 August 2005 40 3  Sensitivity to  13  0

41 Maury Goodman IIT Mumbai 1-2 August 2005 41 95% CL Resolution of the Mass Ordering: Summary

42 Maury Goodman IIT Mumbai 1-2 August 2005 42 3  Determination of CP Violation

43 Maury Goodman IIT Mumbai 1-2 August 2005 43 95% CL Resolution of the Mass Ordering NO A with T2K Phase 1 NO A/PD with T2K Phase 2

44 Maury Goodman IIT Mumbai 1-2 August 2005 44 95% CL Resolution of the Mass Ordering

45 Maury Goodman IIT Mumbai 1-2 August 2005 45 Ed Temple’s Timeline of Critical Decisions and Reviews 11 reviews in 22 months exclusive of NuSAG, P5, and the PAC

46 Maury Goodman IIT Mumbai 1-2 August 2005 46 Assumed T2K Beam Power vs. Time From S. Nagamiya, Feb 2005

47 Maury Goodman IIT Mumbai 1-2 August 2005 47 Sensitivity vs. Time Comparison to T2K

48 Maury Goodman IIT Mumbai 1-2 August 2005 48 Sensitivity vs. Time Comparison to a reactor experiment

49 Maury Goodman IIT Mumbai 1-2 August 2005 49 P(   e ) (in Matter) l In matter at oscillation maximum, P 1 will be approximately multiplied by (1 ± 2E/E R ) and P 3 and P 4 will be approximately multiplied by (1 ± E/E R ), where the top sign is for neutrinos with normal mass hierarchy and antineutrinos with inverted mass hierarchy. About a ±30% effect for NuMI, but only a ±11% effect for JPARC. However, the effect is reduced for energies above the oscillation maximum and increased for energies below.

50 Maury Goodman IIT Mumbai 1-2 August 2005 50 3  Sensitivity to  13  0 Comparison with Proton Driver 5 year only run

51 Maury Goodman IIT Mumbai 1-2 August 2005 51 3  Sensitivity to  13  0 Comparison with T2K 5 year only run

52 Maury Goodman IIT Mumbai 1-2 August 2005 52 3  Sensitivity to  13  0 Comparison with a reactor experiment 5 year only run

53 Maury Goodman IIT Mumbai 1-2 August 2005 53 95% CL Resolution of the Mass Ordering: with a Reactor Expt.

54 Maury Goodman IIT Mumbai 1-2 August 2005 54 3  Determination of CP Violation: with a Reactor Expt.

55 Maury Goodman IIT Mumbai 1-2 August 2005 55 95% CL Resolution of the  23 Ambiguity

56 Maury Goodman IIT Mumbai 1-2 August 2005 56 3  Determination of CP Violation

57 Maury Goodman IIT Mumbai 1-2 August 2005 57 3  Determination of CP Violation

58 Maury Goodman IIT Mumbai 1-2 August 2005 58 3  Determination of CP Violation

59 Maury Goodman IIT Mumbai 1-2 August 2005 59 3  Determination of CP Violation

60 Maury Goodman IIT Mumbai 1-2 August 2005 60 3  Determination of CP Violation

61 Maury Goodman IIT Mumbai 1-2 August 2005 61 95% CL Resolution of the Mass Ordering

62 Maury Goodman IIT Mumbai 1-2 August 2005 62 95% CL Resolution of the Mass Ordering

63 Maury Goodman IIT Mumbai 1-2 August 2005 63 Far Detector Assembly One 8-plane sub-block assembled per day Detector has 248 sub- blocks 8-plane sub-block 32-plane block 1-cm expan- sion gap 32-plane block

64 Maury Goodman IIT Mumbai 1-2 August 2005 64 Far Detector Building Proposal Design Bathtub for full containment

65 Maury Goodman IIT Mumbai 1-2 August 2005 65 Far Detector Building Design with Overburden

66 Maury Goodman IIT Mumbai 1-2 August 2005 66 Near Detector 5 m 3.5 m 9.6 m Veto region Target region Shower containment region Muon catcher 1 m iron 262 T 145 T totally active 20.4 T fiducial (central 2.5 x 3.25 m) 8-plane block 10.6 T full 1.6 T empty

67 Maury Goodman IIT Mumbai 1-2 August 2005 67 Near Detector: Modular and Mobile M Test MINOS Surface Building NuMI Access Tunnel

68 Maury Goodman IIT Mumbai 1-2 August 2005 68 Near Detector in MINOS Surface Building 45,000   CC events2,200 e CC events 6.5 x 10 20 pot in 75 mrad off-axis beam Kaon peak

69 Maury Goodman IIT Mumbai 1-2 August 2005 69 Near Detector in the Access Tunnel  CC events e CC events Far Detector x 800 Site 1.5 Site 2

70 Maury Goodman IIT Mumbai 1-2 August 2005 70 Sensitivity to   e Vs. Off-Axis Distance

71 Maury Goodman IIT Mumbai 1-2 August 2005 71 Sensitivity to   e Vs. Off-Axis Distance

72 Maury Goodman IIT Mumbai 1-2 August 2005 72 Sensitivity to the Mass Ordering Vs. Off-Axis Distance

73 Maury Goodman IIT Mumbai 1-2 August 2005 73 3  Sensitivity to  13  0

74 Maury Goodman IIT Mumbai 1-2 August 2005 74 3  Sensitivity to  13  0

75 Maury Goodman IIT Mumbai 1-2 August 2005 75 3  Sensitivity to  13  0

76 Maury Goodman IIT Mumbai 1-2 August 2005 76 3  Sensitivity to  13  0

77 Maury Goodman IIT Mumbai 1-2 August 2005 77 Measurement of  m 32 2 and sin 2 (2  23 ) 5-year run with Proton Driver

78 Maury Goodman IIT Mumbai 1-2 August 2005 78 Study MiniBooNE Signal Site 1.5Site 3 1-year run 1-year run

79 Maury Goodman IIT Mumbai 1-2 August 2005 79 Sensitivity to a Galactic Supernova Signal in 100 ms bins for a galactic supernova assuming a 3 m overburden 1500 signal events

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