Today: Part I: Neutrino oscillations: beam experiments. Part II: Next tutorials: making distributions with histograms and ntuples

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Arthur Neal
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1 Today: Part I: Neutrino oscillations: beam experiments Part II: Next tutorials: making distributions with histograms and ntuples

2 Super-Kamiokande Physics II: Long Baseline Beams

3 Neutrino Oscillations Assume FLAVOR STATES nf > weakly interacting are superpositions of MASS STATES nm > unitary mixing matrix N f >= Ufi i > i=1 If mixing matrix is not diagonal, get flavor oscillations as neutrinos propagate

4 Simple two-flavor case f >= cos 1 > sin > g >= sin 1 > cos > Propagate a distance L: iei t i ( t ) >=e imi L/ p i ( 0) >~e i ( 0) > Probability of detecting flavor g at L: 1.7 m L P ( f g )=sin sin E E in GeV L in km Dm in ev P( )=sin Parameters of nature to measure: q, Dm=m1-

5 The Experimental Game Start with some neutrinos (natural or artificial) Measure (or calculate) flavor composition and energy spectrum Let them propagate Measure flavor and energies again Have the flavors and energies changed? If so, does the 1.7 m L change follow P( f g )=sin sin E? Disappearance: n's oscillate into 'invisible' flavor e.g. ne nm at ~MeV energies Appearance: directly see new flavor e.g. nm nt at ~GeV energies

6 Oscillation Parameter Space 1.7 m L P( f g )=sin sin E fast wiggle Twiddle L/E allowed region Frequency DmL/E slow wiggle Amplitude sinq Experimental statistics

7 Zenith angle distribution FC 1489 days of SK data (SKI) FC+PC e-like m-like up-going down-going Deficit of nm from below (long pathlength)

8 Next: INDEPENDENT TEST of atmospheric neutrino oscillations using a well-understood n beam En~ GeV, L~ 100's of km for same L/E 1.7 m L P ( f g )=sin sin E LONG BASELINE EXPERIMENTS Compare flux, flavor and energy spectrum at near and far detectors

9 KK (KEK to Kamioka) Long Baseline Experiment ~ 1 GeV muon neutrinos 1 GeV protons on Al target + p focusing horn + decay pipe for pions Events matched w/gps

10 The Neutrino Beamline at KEK

11 The Near Detector (300 m away) (scibar) Characterize the n beam for extrapolation to SK

12 Results from KK Single-ring m-like events Total 107 beam events observed; expect Suppression observed, spectral distortion consistent with oscillations

13 KK Allowed Oscillation Parameters Best Fit Results: Dm =.8 x 10-3 ev sin(q) = 1.0 (constrained to physical region) Consistent with SK atmospheric

14 Future Long Baseline Experiments start 005-6, 730 km distance MINOS: Fermilab to Soudan CNGS: CERN to Gran Sasso

15 NuMI Beamline at Fermilab MINOS Detector at the Soudan mine iron plates + scintillating fibers w/ magnetic field

16 CNGS CERN Neutrinos to Gran Sasso Look for t neutrinos explicitly

17 ICARUS Liquid Argon Time Projection Chamber "Digital Bubble Chamber"

18 OPERA lead/emulsion sandwich + scintillator planes Extract bricks for scanning if electronic detector indicates t-like event

19 TK: "Tokai to Kamioka" Existing detector: Super-K 95 km, about 30 times KK flux.5 deg. off axis

20 TK ("Tokai to Kamioka") o off-axis Near + km detectors, Super-K refurbished by 006 Start 009 Beam neutrino energy tuned to oscillation minimum

21 J-PARC beamline under construction now n beam-line decay volume J-PARC Beamline Construction, Jan 004

22 TK Detectors p p n off-axis on-axis 0m 140m 80m km 95 km 1. Near detector at 80 m: fine-grained tracker. Intermediate detector at km Water Cherenkov + fine-grain tracker (LAr) + muon ranger Beam spectrum looks more like beam at SK cancel systematics 3. Super-K III at 95 km, fully refurbished

23 Summary Atmospheric muon neutrinos are changing flavor ('disappearing') as they travel through the Earth: This measurement in SK was the first clear indication of neutrino mass and oscillation 1.7 m L P( f g )=sin sin E This oscillation disappearance has now been confirmed with a long-baseline beam of neutrinos: KK results are consistent Next generation: MINOS, CNGS, TK

24 SK Data Tutorial Today 1. Run superscan to eyeball data files.1 Set up and run sample program to look at charges and times for events. Make and view histograms TODAY (distributions) - Histograms made directly in program - Ntuples made using PAW

25 Histogram: a distribution of some variable(s) 1D D density of dots number of events in bin Cernlib/PAW: software package that allows manipulation of histogram structures - create histogram - 'fill' with data - output histo to file

26 Ntuple: list of 'events' and their variables e.g. run no., event no., total charge, mean t 000, 1, 4., ,, 13., , 3,.,984. Note: an 'event' need not be an SK event (trigger); you can make an ntuple of tube hits, or any kinds of items ('event' an item in the list) PAW will allow you to plot distributions of any chosen variable, or any variable vs any other, with 'cuts' (conditions) e.g. nt/plot 1.q%t t>800&&t<1000 means plot charge vs time for times between 800 and 1000 very powerful!

27 Making a histogram in the program: - Open data file (skopenf) - Loop over events - Read one event (skread) (information stashed locally) - Loop over PMT hits - For each hit, fill charge and time histograms - Close data file (skclosef) - Output histogram to file Later, view histogram with PAW (or Root)

28 Making simple ntuples: - Open data file (skopenf) - Loop over events - Read one event (skread) (information stashed locally) - Loop over PMT hits - For each hit, output list of variables to a text file - Close data file (skclosef) Later, use PAW to make ntuples from text file, and plot desired variables

29 Next weeks: I will be in Japan, but other HEP profs (who would like to recruit students for research) will speak

AN EXPERIMENTAL OVERVIEW OF NEUTRINO PHYSICS. Kate Scholberg, Duke University TASI 2008, Boulder, CO

AN EXPERIMENTAL OVERVIEW OF NEUTRINO PHYSICS Kate Scholberg, Duke University TASI 008, Boulder, CO Alexei Smirnov, Neutrino 008, Christchurch NZ These lectures: experiment How do we know what we know?