Future Outlook: Experiment Future Outlook: Experiment Future Outlook: - PowerPoint PPT Presentation

Future Outlook: Experiment Future Outlook: Experiment Future Outlook: Experiment Future Outlook: Experiment Yoichiro SUZUKI Yoichiro Yoichiro SUZUKI Yoichiro SUZUKI SUZUKI Kamioka Observatory, Institute for Cosmic Ray Research, Kamioka Observatory, Institute for Cosmic Ray Research, and and and and Institute for the Physics and Mathematics of the Universe, Institute for the Physics and Mathematics of the Universe, The University of Tokyo The University of Tokyo The XXIII International Conference on Neutrino Physics and Astrophysics, Neutrino2008, N t i Ph i d A t h i N t i 2008 May ‐ 31 Christchurch, New Zealand Christchurch, New Zealand 1 2008/5/30 Y. Suzuki @NEUTRINO2008, Christchurch, New Zealand

Preface Preface • My talk is neither y neither a summary talk nor y nor general g view in future. • This is a quite biased and personal view biased and personal view of a direction of the future future large scale neutrino experiments � ‘Ultimate’ Experiments beyond � ‘ ’ beyond the next the next generation experiments: • more than 20 years from now (or more) • more than 20 years from now (or more) • Please relax and have a dream together Note for the audience Note for the audience This talk may contain hazardous opinion and may spoil you (PG40). It is your own responsibility to listen me. 2 2008/5/30 Y. Suzuki @NEUTRINO2008, Christchurch, New Zealand

10 th anniversary of the Discovery of the Neutrino Oscillation • It started as an Atmospheric Neutrino Anomaly It t t d At h i N t i A l ( ν μ deficits in 1988, by Kamiokande) – Background of the Proton Decay Search Background of the Proton Decay Search ν µ - ν τ ν µ - ν τ ν µ - ν τ 200 200 200 number of events number of events number of events Super Kamiokande Preliminary Super Kamiokande Preliminary Super Kamiokande Preliminary μ ‐ like 180 180 180 e ‐ like like like 160 160 160 140 140 140 120 120 120 100 100 100 80 80 80 60 60 60 40 40 40 ( 1.0, 2.2 × 10 -3 ) ( 1.0, 2.2 × 10 -3 ) ( 1.0, 2.2 × 10 -3 ) 20 20 20 Momentum (MeV Momentum ( MeV/c) /c) 0 0 0 -1 -1 -1 -0.8 -0.8 -0.8 -0.6 -0.6 -0.6 -0.4 -0.4 -0.4 -0.2 -0.2 -0.2 0 0 0 0.2 0.2 0.2 0.4 0.4 0.4 0.6 0.6 0.6 0.8 0.8 0.8 1 1 1 cos θ cos θ cos θ Multi-GeV µ -like+P.C. Multi-GeV µ -like+P.C. Multi-GeV µ -like+P.C. Multi-GeV µ -like+P.C. Multi-GeV µ -like+P.C. Multi-GeV µ -like+P.C. Multi-GeV µ -like+P.C. Multi-GeV µ -like+P.C. Multi-GeV µ -like+P.C. • It took 10 years to establish as an Real Effect • It took 10 years to establish as an Real Effect – Convincing Evidence came from Super ‐ K (1998) • High Statistical Measurement High Statistical Measurement High Statistical Measurement High Statistical Measurement • Independent of the Flux calculation Independent of the Flux calculation 3 2008/5/30 Y. Suzuki @NEUTRINO2008, Christchurch, New Zealand

More than 30 years More than 30 years • Solar neutrino problem: S l t i bl – Started in late 60 – Solved in 2001 (SNO +SK) • High statistical experiments High statistical experiments High statistical experiments High statistical experiments • Flux independent evidence (SNO+SK, SNO Flux independent evidence (SNO+SK, SNO NC+CC) NC+CC) NC+CC) NC+CC) � Discovery of Neutrino Oscillation has really changed the world has really changed the world 4 2008/5/30 Y. Suzuki @NEUTRINO2008, Christchurch, New Zealand

Number of Talks @N98 & N08 @ 18 16 14 12 ? ? 10 8 Neutrino98 6 6 Neutrino2008 4 2 0 0

After the establishment of the neutrino oscillation • We now have well motivated ‘standard’ menu ‘standard’ menu to do. – Physics parameters to be measured! – Questions to be answered ? b d – θ 13 ! – CPV ?, CP phase ! – Majorana or Dirac ?, Majorana mass ! – Mass hierarchy ? – Absolute mass ! – ……… • Though the above list are significant and important, there are no big puzzles or problems puzzles or problems like solar neutrino problem or atmospheric anomaly. • In any way we are guided to the fruitful and promising future !? ? ? ? ? future !? ? ? ? ? 6 2008/5/30 Y. Suzuki @NEUTRINO2008, Christchurch, New Zealand

Ultimate experiment after the next Since we will build a huge detector and spend big amount of money with large d bi f i h l number of scientists 1) Cover the standard list standard list as much as possible 2) Include other 2) Include other other scientific possibility or new opportunity other scientific possibility, or new opportunity new opportunity new opportunity as much as possible θ 13 may not be determined positively! θ 13 may not be determined positively! 13 may not be determined positively! 13 may not be determined positively! DB decay may not be accessible! DB decay may not be accessible! 3) Need bread and butter ) bread and butter science need ‘measurements’ as well as searches need ‘measurements’ as well as searches � Build � Build Build GOOD Versatile detectors Build GOOD Versatile detectors GOOD Versatile detectors GOOD Versatile detectors 7 2008/5/30 Y. Suzuki @NEUTRINO2008, Christchurch, New Zealand

Limit myself to discuss two example, because of the limitation of the time the limitation of the time 1) Neutrino Oscillation Experiments, and 2) Double Beta Decay Experiments 8 2008/5/30 Y. Suzuki @NEUTRINO2008, Christchurch, New Zealand

‘Standard’ ‘Standard’ Next Next Neutrino Oscillation Experiments Neutrino Oscillation Experiments • Aim to study CPV, Mass hierarchy • Megaton Scale Detector + Upgraded Accelerator Megaton Scale Detector + Upgraded Accelerator • Typical � Detector 0.5 Mton (fiducial Volume) UNO 440kton Hyper-K 540kton • Other Subjects – Proton Decay (10 35 years for e π 0 ) – SN neutrinos SN i 9 2008/5/30 Y. Suzuki @NEUTRINO2008, Christchurch, New Zealand

Is the Proton Decay sensitivity of 10 35 years for e π 0 (10 years of running) strong enough? running) strong enough? 10 2008/5/30 Y. Suzuki @NEUTRINO2008, Christchurch, New Zealand

What is the best goal for the proton decay search • ν K, , μ K : strong model dependence d l d d • Prediction of Dimension 6 in SUSY GUT – Less model dependent for e π for e π 0 35 ～ 10 10 35 10 36 36 yr – Reasonable range: 10 Reasonable range: 10 10 10 10 yr yr for e yr for e � From coupling unification From coupling unification 36 yr � Search up to � Search up to Search up to ～ 10 Search up to ～ 10 10 36 10 36 36 yr yr is quite important and yr is quite important and is quite important and is quite important and add significant value to the neutrino oscillation exp. add significant value to the neutrino oscillation exp. Sensitivity for e π 0 � S � Sensitivity for 0 0 will guide the size of the S i i i i i i f f will guide the size of the ill ill id id h h i i f h f h experiment experiment 11 2008/5/30 Y. Suzuki @NEUTRINO2008, Christchurch, New Zealand