1. Long Baseline Experiments at Fermilab Maury Goodman

2. Outline Fermilab Long-Baseline history (1987) NuMI MINOS results 2006 A tale of identical detectors NOvA Fermilab/BNL study

3. Some History of Long-Baseline at Fermilab

4. n I first heard a serious long-baseline talk from Al Mann The Fermilab beam pointed towads Sudbury First Physical Review paper with a map?

5. Fermilab pre-history

6. Long-Baseline History at Fermilab I started work in 1987 for a “GRANDE” workshop in Arkansas Calculations were done with what we now call the HE beam

7. NuMI - a combined short-baseline/long-baseline program

8. 1992 Workshop on long- baseline neutrino oscillations

9. 1991

10. Optimize Distance?

11. Optimize decay pipe

12. Optimize beam energy

13. NuMI

16. A tale of 3 beam configurations

17. MINOS results 2006

18. MINOS Experiment Far Detector, Soudan, MNNear Detector at Fermilab, IL 980 tons, 105 m underground 282 steel and 153 scintillator planes 5400 tons, 710 m underground 486 steel and 484 scintillator planes 735 km 1 2 Monte Carlo 1 2

20. Stability of the energy spectrum & reconstruction June July August September October November Energy spectrum (ND) by month Energy spectrum by batch

22. Far Detector Unoscillated Energy spectrum Different methods are robust against different kinds of systematics

23. Observed & Expected events There is a large energy dependent deficit Below 10 GeV the significance of the deficit is 5.8  (stat+syst) MINOS Preliminary result based on 1.27 E20 protons Data sampleData Expected (Fit Method; Unoscillated) Expected (Matrix Method; Unoscillated) Data/MC (Matrix) ν μ only (<30 GeV)215332.8335.80.64 ν μ only (<10 GeV)122237.7238.90.51 ν μ only (< 5 GeV)67168.6168.30.45

24. nc/cc Variables

25. MINOS result

26. MINOS ratio

27. Allowed region (Preliminary)  m 2 32 = (2.72 +0.38 - 0.25) (stat) x 10 -3 eV 2 Sin 2 2  23 = 1.00 - 0.13 (stat)  m 2 32 = (2.72  0.25) (stat) x 10 -3 eV 2 Constrained to sin 2  23 = 1.00 Systematics are about 1/3 of statistical error

28. A tale of identical detectors

33. Energy Calibration

34. Calibration Light Injection

35. Drift

36. Linearity

37. Strip to Strip Variation

38. Attenuation

42. NO A

43. The Far Detector The cells are made from 32-cell extrusions. 12 extrusion modules make up a plane. The planes alternate horizontal and vertical. For structural reasons, the planes are arranged in 31-plane blocks, beginning and ending in a vertical plane. There are 54 blocks = 1654 planes. The detector can start taking data as soon as blocks are filled and the electronics connected.

44. The Near Detector 4.1 m 2.9 m 14.4 m Veto region Target region Shower containment region Muon catcher 1 m iron 209 T 126 T totally active 23 T fiducial The Near Detector will be placed off-axis in the MINOS access tunnel and will be moveable along the tunnel to measure the different components of the backgrounds.

45. The Integration Prototype Near Detector We plan to have a prototype version of the Near Detector running in the MINOS surface building by the end of 2007. It will detect a 75 mr off-axis NuMI beam, dominated by K decays. 3 GeV  2 GeV e

46. Event Quality Longitudinal sampling is 0.15 X0, which gives excellent  -e separation. A 2-GeV muon is 60 planes long.

47. Cost & schedule $200M cap(?) Just combined with beam efforts ~$100M to get to 1.2 MW

48. Fermilab/BNL study

49. More long-baseline neutrino issues Physics goals (  space) DUSEL (Homestake/Henderson, if, when, who pays) Detectors (Water-UNO, liquid Argon,…) Transverse-2 nd maximum? Proton intensity upgrades (proton plan, proton driver, Super-NuMI,…) Detector depth (for other physics) Concerns: event rate, NC background, resolution, parameter sensitivity, total cost and timeliness. http://nwg.phy.bnl.gov/~diwan/nwg/fnal-bnl/

50. CP-2540 km

51. BNL Wide band Single Ring Events only Example- 500 kton water detector (UNO) See CP effects with one measurement

52. For  13 Two Approaches Off axis: Use existing NUMI beam. NOvA(25kT) will be built ~10mrad offaxis for the first maximum. NOvA2(50kT LAR) will be built at 40 mrad for second maximum. Both detectors will be on the surface. Combine the results to extract  13, mass hierarchy, & CP. Low energy wide band: Couple the long baseline program to DUSEL. Site a large detector (~200kT if water Cherenkov) at approximately 5000 mwe. Build a new wide beam with a spectrum shaped to be optimum (0.5-6 GeV). Use detector resolution to extract multiple nodes. Report to NuSAG in progress

53. FNAL/BNL long-baseline study

54. Two Approaches Off axis: Use existing NUMI beam. NOvA(25kT) will be built ~10mrad offaxis for the first maximum. NOvA2(50kT LAR) will be built at 40 mrad for second maximum. Both detectors will be on the surface. Combine the results to extract  13, mass hierarchy, & CP. Low energy wide band: Couple the long baseline program to DUSEL. Site a large detector (~200kT if water Cherenkov) at approximately 5000 mwe. Build a new wide beam with a spectrum shaped to be optimum (0.5-6 GeV). Use detector resolution to extract multiple nodes. Concerns: event rate, NC background, resolution, parameter sensitivity, total cost and timeliness. Report to NuSAG in progress

55. An opinion on Our neutrino future

56. Graphs like this are necessary They are very difficult to interpret & believe

57. Backup

58. Predicting the unoscillated FD spectrum ND and FD spectra are similar but not identical For each MC  in ND with energy E i, we know the kinematics of its parent from MC That allows us to calculate probability of this parent giving with E j in FD Thus one can calculate matrix M ij (MC is tuned to ND energy spectrum) FD Decay Pipe π+π+ Target ND p