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First long dist<strong>an</strong>ce data in 2007G. Rosa, Nu200838 intarget(nontau)events
Expectations for 5 years <strong>of</strong> OPERA runningG. Rosa, Nu2008totalexpectedsignal in targettotalexpectedbackground
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AN EXPERIMENTAL OVERVIEWOF NEUTRINO
Page 3 and 4:
These lectures:experimentHow do we
Page 5 and 6:
Lecture 1Overview of neutrino sourc
Page 7 and 8:
Why Do Neutrinos Matter?They are a
Page 9 and 10:
Sources of 'tame' neutrinosNuclearr
Page 11 and 12:
Neutrino detectors: in general want
Page 13 and 14:
Simple twoflavor case| f>= cos| 1
Page 15 and 16: Probabilityof changingflavorP( f f
Page 17 and 18: Experimental statisticsOscillationP
Page 19 and 20: The Three SignalsSOLAR NEUTRINOS e
Page 21 and 22: First, zoom in to atmospheric ν pa
Page 23 and 24: Detecting Neutrinos with Cherenkov
Page 25: SuperKamiokandeOuterdetector:1889
Page 28 and 29: SuperK Accident November 12, 2001
Page 30 and 31: SuperK Full Reconstruction Photo
Page 32: Get differentpatternsin Cherenkovli
Page 35 and 36: Getting more from the data set:pare
Page 37 and 38: What flavors are involved in thisν
Page 39 and 40: For ν µ→ ν sterilewould expect
Page 43 and 44: Tau Appearancein SuperKTypical MC
Page 47 and 48: Select events for which resolution
Page 49 and 50: Improves ∆m 2 resolution a little
Page 51 and 52: K2K (KEK to Kamioka)Long BaselineEx
Page 53 and 54: The Near Detector (300 m away)(scib
Page 55 and 56: K2K Allowed Oscillation ParametersC
Page 57 and 58: NuMI Beamline at FermilabH. Gallagh
Page 59 and 60: Event flavors selected based on top
Page 61 and 62: Allowed oscillation parameters from
Page 63 and 64: The CNGS beamlineDesignedto searchf
Page 65: OPERAlead/emulsion sandwich +active
Page 69 and 70: 600 ton detector at LNGS awaiting f
Page 71: Lecture 2Current status of oscillat
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