MINOS/NO A Deborah Harris Fermilab NuFact’04 Osaka University July 28, 2004

MINOS/NOvA2 Outline of Talk MINOS –Beamline Progress –Detector Progress –Not covered: Cosmic ray analyses at Far Detector –Accelerator Physics Expectations NO A –Overview –Beamline Progress—see above –Detector Progress—see P.Strolin (mostly) –Physics Reach now and in the future

MINOS/NOvA3 Acknowlegements The majority of the slides I will show come from the excellent talks given by –Sacha Kopp, Fermilab User’s Meeting, 6/2004 –Mark Messier, Neutrino 2004, 6/2004 –Mark Thomson, Neutrino 2004, 6/2004 Since probably no one here was at all of these talks, I hope at least a few slides will be new for everyone in the audience

MINOS/NOvA4 Det km Det. 2 Near detector predicts energy spectrum at far detector (in absence of oscillations) Multiply near spectrum by scaling factor to predict far. Must believe that beam at two detectors is (1) the same, or (2) difference calculable. Near Detector: 980 tons Far Detector: 5400 tons Two Detector Experiment Idea dates back to CERN, FNAL mid-1980’s

MINOS/NOvA5 The NuMI Beam “Neutrinos at the Main Injector” NuMI has 400kW primary proton beam 120 GeV 8.67  sec spill 1.9 sec rep rate 5 Booster batches (2.5  prot/spill) p beam Pion beam

MINOS/NOvA6 Extracted Proton Beam Line Carrier Tunnel Angling down Pre-Target Foil Profile Monitor

MINOS/NOvA7 Progress on Target and Horns Horns assembled and pulsed Horn 1 & power supply installed underground >>5.4+1kton of shielding installed “Crosshairs” for alignment checks in situ Beam’s eye view of horn in chase

MINOS/NOvA8 Progress on Decay Pipe and Absorber 675m long decay pipe pumped down to 1.4Torr on first try! Water-cooled Aluminum core installed Hadron Monitor Support Installed Almost all of 2.2kTons there

MINOS/NOvA9    p      Bypass Tunnel  Monitors to Study Beam BeamTests Expected  profiles in Alcove 1 Alcove 2 Alcove 3 New levels of radiation hardness Required for muon monitors!

MINOS/NOvA10 MINOS Near Detector Installation 1. Down the shaft 2. Across the hall 3. Installed Less than 30 out of 282 planes to go!

MINOS/NOvA11 MINOS Far Detector magnetized Fe-scintillator calorimeter segmented scint for X, Y tracking 485 planes, 8m diam, 5400 tons

MINOS/NOvA12 MINOS Schedule Far Detector completed in 2003 NuMI Tunnel –Excavation complete in 2002 –Outfitting (electrical, air, water, etc) complete in fall 2003 and March 2004 (two phases) Primary beamline and target hall installation –Begun in fall 2003 –Finish in November 2004 Near detector installation to finish early fall ‘04 READY FOR BEAM November, 2004

MINOS/NOvA13 Oscillated/unoscillated ratio of number of   CC events in far detector vs E observed 90% and 99% CL allowed oscillation parameter space for the Super-K best fit point. For  m 2 = eV 2, sin 2 2   = 1.0 Measurement of  Disappearance in MINOS Figures from MINOS 5yr plan submitted to Fermilab PAC 2003

MINOS/NOvA14 MINOS Measurement of  m 2 Current way of quoting  m 2 range: Full width at sin 2 2  23 =1, at 90%CL K2K now has 90%CL range of 1.7<  m 2 <3.3 x10 -3 eV 2, or a fractional error of 0.66 with a  m 2 of 2.73x10 -3 eV 2 (NuFact04) When MINOS has 7x10 20 POT, this Should result in a factor Of 4 increase in precision Can we please start quoting 1  error bars like precision experiments? (plot on left is in “current way”) Or, Time for a Change of Terminology 90%CL

MINOS/NOvA15 Region where sin 2 2  can be resolved as <1.0 at 90% CL. Resolve Non-Maximal Mixing?  m 2 (eV 2 ) sin 2 (2   ) SK allowed (90%C.L.)

MINOS/NOvA16 Beam e backgrounds For  m 2 = eV 2, sin 2 2  13 = Osc. Max for this  m 2 Search for   e Appearance Observed e CC 25x10 20 POT With e oscillations 90% CL Exclusion Limits (5 years, 3kt)  m 2 (eV 2 ) sin 2 (2   ) Protons on Target (  ) JHF (2009+5yrs) MINOS (  m 2 = eV 2 ) sin 2 (2  13 ) Discoverable at 3  CHOOZ (  m 2 = eV 2 ) Or 3  Discovery!!

MINOS/NOvA17 Next Steps in Oscillation Physics Once MINOS provides stringent test of oscillation framework Once MINOS improves precision on  m 2 by factor of 4 or more… Want to focus on  → e transitions –Seeing it in the first place –Getting the most physics out of what you see

MINOS/NOvA18 Goals and Beams MINOS: pin down  m 2 NO A look for e /  transitions at  m 2 atm –First hint of  13 being non-zero? –CP violation in absence of matter effects –Matter effects in absence of  m sol 2

MINOS/NOvA19 NO A Collaboration 160 Authors, 34 Institutions, Gary Feldman and John Cooper Co-spokespersons US UK Greece Brazil Canada

MINOS/NOvA20 How will NO A Improve on MINOS? Increase Detector Mass by 5 or more Increase Flux/POT at Oscillation Max by ~2 by going off axis Reduce the backgrounds to e appearance –Lower e at the peak by going off axis –Lower NC contamination by going off axis Build detector optimized for e appearance –Segmented X 0 /3 instead of 1.5X 0 ! Low Z instead of High Z –more kton/X 0 –Events are big—need fewer channels per transverse dimension Go to Higher L, Lower E, more matter effects –810km, 2GeV peak, instead of 735km, 3.5GeV peak Goal: factor of 10 past MINOS reach on sin 2 2  13

MINOS/NOvA21 How the Off Axis Strategy Works

MINOS/NOvA22 What Can we expect at NO A?

MINOS/NOvA23 Detector Strategy Baseline Design –Particle Board (20cm) w/ Liq. Scintillator (3cm thick) in Extrusions, 750 planes –Segmentation X 0 /3 –6.9kton active/50.7kton total (14%) –Active Veto Shield Planned Totally active Design –Liquid Scintillator (4.9cm thick) in Extrusions, 1845 planes –Segmentation X 0 /7 –21kton active/25kton total (85%) Both Designs –Looped Wavelength Shifting Fiber to Avalance PhotoDiode Readout (see P. Strolin’s talk) Scintillator modules 1.3m 20cm

MINOS/NOvA24 Event Displays from Baseline Detector Design e CC signal: >3 hits/track >1.5 hits/plane Cos(  beam )>.8 Likelihood Analysis on “event shape”

MINOS/NOvA25 Totally Active Scintillator Detector Events (2GeV) One unit is 4.9 cm (horizontal), 4.0 cm (vertical) + A -> p + 3  ± +  0 + e +A→p  +  - e -  + A -> p +  - Signal Efficiency 32%(18% baseline) Signal/Background 7.7(4.6 baseline) Signal/sqrt(bg.) 26(24.5 basline) Because of larger Efficiency and better Background rejection, Can make ½ the mass

MINOS/NOvA26 Where should NO A put the detector? Largest asymmetry for normal vs inverted Mass hierarchy at larger angles Site that maximizes matter effects is Not optimal for  13 but Mass Hierarchy Determination is unique to NO A Duty cycle is tiny (10  sec/1.8sec) So detector can be at surface of Earth

MINOS/NOvA27 NO A Near Detector

MINOS/NOvA28 Measurement Suite NO A will use

MINOS/NOvA29 NO A Physics Results  Disappearance e Disappearance –Seeing evidence for sin 2 2  13 ≠0 –Mass Hierarchy –CP Violation –What about adding another detector? Make more of same detector in same place? Add another detector farther off axis? Lesson we’ve seen before: 2 different E or L (or both) are better than twice as much at same E and L!

MINOS/NOvA30  Disappearance in NO A

MINOS/NOvA31 NO A’s Reach in sin 2 2  13 : Depends on ,mass hierarchy!

MINOS/NOvA32 NO A’s reach in sin 2 2  13 Smaller angle off axis has slightly better reach in sin 2 2  13 How it compares to T2K depends on sign(  m 2 )! 12mrad Off axis 15mrad Off axis

MINOS/NOvA33 Determination of the Mass Hierarchy Different ways of getting there: –Compare NO A and T2K –Compare 15mrad NO A to 42mrad NO A (matter effects tiny at that energy-- 0.7GeV ) –Add More protons and stir… –Add more detector mass and stir…

MINOS/NOvA34 Search for CP Violation No matter what, T2K and NO A need proton driver upgrades to get to CP violation (need the ’s) Second Oscillation Max strategy: CP violation 3x bigger! ( energy at 42mrad 1/3 of energy at 15mrad) NO A+T2K + 2 p driver upgrades NO A+2 nd Osc. Max NO A + 1 p driver upgrade NO A+T2HyperK + 2 p driver upgrades

MINOS/NOvA35 Technically Driven Schedule Need Stage I approval, don’t have it yet… With Final approval in 2005, Construction starting 2006, data taking starting with half the detector in 2008 Will pass up reach of MINOS quickly…or make precision measurement of a signal they (or OPERA or ICARUS) see first!

MINOS/NOvA36 Conclusions NuMI Beamline is a long time coming, but is almost here: ready to commission end of 2004! MINOS is right around the corner –Near Detector commissioning as we speak! –Physics running in 2005 –Improve  m 2 measurement over what we have now by factor of 4 or better! NO A –10x sensitivity of MINOS to  → e –Even more precise disappearance measurements –Optimize for physics reach (matter effects!) –Precision P(  → e ) measurements the goal Both experiments benefit greatly from measurements at –MIPP (hadron production on NuMI target) –MINER A (neutrino cross sections & interactions)