Three flavor effects and Synergy between atmospheric and other - PowerPoint PPT Presentation

Three flavor effects and Synergy between atmospheric and other experiments Srubabati Goswami Physical Research Laboratory Ahmedabad, India PANE 2018, ICTP Srubabati Goswami 1

Synergy between atmospheric and LBL experiments 2 PANE 2018, ICTP Srubabati Goswami

Synergies Between Experiments S. Raut. Talk @NUFACT 2017 PANE 2018,ICTP 3 Srubabati Goswami

Synergies Between Experiments S. Raut. Talk @ NUFACT 2017 PANE 2018, ICTP 4 Srubabati Goswami

Synergy between channels  2 Total greater than individual Contribution PANE 2018, ICTP 5 Srubabati Goswami

Three neutrino oscillation parameters 3 masses, 3 mixing angles, 1 phase Interplay among different sectors  because of 13 PANE 2018, ICTP 6 Srubabati Goswami

Global Analysis (2018) Best-fit in second octant Preference for NO     90 disfavored at CP 3  more than irrespective of mass ordering Talk by E. Lisi PANE 2018, ICTP 7 Srubabati Goswami

Immediate Goals Mass Hierarchy Non-zero   Matter effects in atmospheric and long-baseline experiments ( ) 13  m ,  13 2 Interference effects in reactor experiments ( ) 21 13 Non-zero   2 m Octant of 23 21  Matter effects in atmospheric and long baseline experiments ( ) 13  2 m Matter effects in atmospheric neutrino experiments ( ) 21 CP Violation Long baseline experiments , needs to disentangle matter CP , atmospheric neutrino experiments (Talk by S. Razzaque)  m ,  2 Genuine three flavor effect ( ) 21 13 PANE 2018, ICTP 8 Srubabati Goswami

Current and Future Experiments Current Future Atmospheric Atmospheric INO, Hyper Kamiokande, Super Kamiokande PINGU, ORCA Long-baseline Long-baseline T2K, NOVA DUNE,T2HK,T2HKK, ESSnuSB Reactor Reactor Daya-Bay, Double CHOOZ JUNO  --Decay  Dar MOMENT PANE 2018 , ICTP 9 Srubabati Goswami

Long-baseline Experiments: Salient features E Details Expt Baseline (GeV) Energy 295 km, 0.6 0.76 MW T2K Tokai to Kamioka Super Kamiokande 810 km, 1.7 0.7 MW NOVA FNAL to ASH River 14 kt TASD 1300 km 0.5-8 1.2 MW DUNE FNAL to South Dakota Liquid Argon 10kt/40 kt 295 km 0.6 1.3 MW , 187 kt X2 T2HK JPARC to Kamioka Hyper Kamiokande 295km, 1100 km 0.6 HK, Water Cherenkov in T2HKK Korea 540 km , Lund to 2 500 kt ESSnuSB Gapenberg Water Cerenkov , PANE 2018, ICTP Srubabati Goswami L 10

Atmospheric Neutrino Detectors: Salient features Prototype Salient features Magnetized IRON ICAL@INO 50 kt, muon energy and direction measurement, charge id, neutrino energy reconstruction Water Cherenkov Hyper Megaton, no charge id, both electron Kamiokande and muon energy and direction Water Cherenkov ORCA Multi- Megaton, tracks and showers, (Mediteranian) no charge id ICE Cherenkov PINGU Multi megaton, tracks and showers , (Southpole) no charge id Liquid Argon DUNE Liquid Argon, both muon and electron events Charge id for both ?? PANE 2018, ICTP Srubabati Goswami L 11

Salient Features of Atmospheric & LBL experiment Atmospheric Neutrinos Long-baseline Neutrinos Fixed Path Length < 1500 km Path length 10 – 10,000 km Narrow band and wide band Broad range of energy compared to beams, smaller range for latter other natural or artificial sources Can’t probe resonant matter effect Can probe resonant matter effects       , Source of or Source of , ,     e e 0  N  ~ P N 0 0 Disappearance channel N ~ N P N P       e e 0 Appearance Channel 0 0 N ~ P N N ~ N P + N P     e e e ee e e Can probe disappearance and Cannot disentangle disappearance appearance channels separately and appearance channels The same experiment can also run Both neutrinos and antineutrinos in antineutrino mode and only detectors with chargeID can probe these separately Srubabati Goswami L PANE 2018 ,ICTP 12

Matter Effects : Three flavors The propagation equation in matter       2 2 m / m Double Expansion in small parameters s 21 31 13 Suitable for studying the current and proposed long-baseline experiments      2 2 One Mass Scale Dominance (OMSD) Limit ( ), 2 m m m 0 21 31 21   2  Also m L / E 1 21  Satisfied by atmospheric neutrinos of energy O (GeV) sin       Valid for sin 0.03 13 13 Resonance in the 1-3 sector PANE 2018, ICTP 13 Srubabati Goswami

  s The survival and oscillation probabilities ( ) 13 In matter of      2 2 1 sin 2 sin subleading terms P  23 constant density    2 / 4 m L E 31 ˆ  Hierarchy    2 2 s gn( ) m 2 2 / A G n E m Changes sign with 31 sensitivity F e 31  + for neutrinos Depends on CP - for antineutrinos PANE 2018, ICTP Srubabati Goswami L 14

The survival and oscillation probabilities (OMSD)  No dependence on CP Hierarchy Detectors with sensitivity charge Id suitable PANE 2018, ICTP Srubabati Goswami L 15

Matter Effect at large baselines Atmospheric neutrinos can encounter resonance Matter effect opposite for and P  P  e PANE 2018, ICTP Srubabati Goswami L 16

Degeneracy Menace The main problem in determination of hierarchy, octant and CP in long- baseline experiments is due to the presence of degeneracies. Minakata, NunoKawa, 2001 Gandhi, Ghosal, Goswami, Shankar 2005 Fogli and Lisi, 1996 Comprehensive Approach Coloma, Minakata, Parke, 2014 Ghosh,Ghoshal, Goswami, Nath, Raut, 2015 PANE 2018, ICTP 17 Srubabati Goswami

 Hierarchy -- Degeneracy CP Antineutrino Neutrino Favourable No degeneracy No degeneracy LHP UHP LHP UHP            0 180 LHP 180 0 UHP CP CP No degeneracy for NH-LHP and IH-UHP IH-LHP degenerate with NH-UHP Combining neutrino and antineutrino does not help in lifting degeneracy PANE 2018, ICTP 18 Srubabati Goswami

Hierarchy Sensitivity : T2K and NOVA 3  T2K + NOVA can give up to sensitivity in favorable zone ( Praksh, Raut, Sankar, 2012 ) Hierarchy sensitivity less in the degenerate region 3  Shaded region currently allowed at from global analysis PANE 2018 , ICTP 19 Srubabati Goswami

Impact of Matter effect Resonant matter effect NH +90 and IH -90 Degeneracy for  No degeneracy separated ~ 2-4 GeV CP NH +90 & IH -90 20 PANE 2018, ICTP Srubabati Goswami

Can atmospheric Neutrinos help ? W. Winter, 2013 Devi, Thakore, Agarwalla, Dighe, 2014  For atmospheric neutrinos hierarchy- degeneracy is not present CP Addition of atmospheric data raises sensitivity in the degenerate region PANE 2018, ICTP Srubabati Goswami L 21

Next generation LBL experiments : DUNE Using atmospheric neutrinos @DUN E Ghosh, Goswami, Raut, 2014 Barger et al, 2014  5  DUNE (10kt, 5+5 years) has close to hierarchy sensitivity over most CP  2 Adding other experiments results in slight increase in overall 22 PANE 2018, ICTP Srubabati Goswami L

Next generation LBL: ESSnuSB and T2HK 4  ESSnuSB + INO : upto Enhanced sensitivity in T2HK 5  ESSnuSB+T2K+NOVA+INO : upto by adding HK atmospheric data Chakraborty, Goswami, Gupta, Thakore, (2018) Fukasawa, Ghosh, Yasuda (2017) Srubabati Goswami L 23 PANE 2018, ICTP

Octant sensitivity in long-baseline experiments Synergy between appearance and disappearance channel Huber,Lindner,Winter ,2002 Octant Sensitivity Hiraide et al., 2006 Coloma,Minakata, Parke, 2014 PANE 2018, ICTP 24 Srubabati Goswami

Marginalization and synergy   2 2 Marginalization over leads to a higher than the appearance value m 31 PANE 2018, ICTP 25 Srubabati Goswami

 Octant- degeneracy CP  CP Flips sign UHP LHP LHP UHP LO-UHP and HO-LHP no degeneracy LO-LHP and HO-UHP degeneracy Combination of neutrino and antineutrino data can help in lifting octant degeneracy Agarwalla, Prakash, Umasankar 2013 Machado et al. 2013 PANE 2018, ICTP 26 Srubabati Goswami

Octant Sensitivity: Atmospheric Neutrinos 5000km Choubey , Roy, 2005   2 m (    Near resonance sin 2 1 No 13 ) degeneracy 13 23  5000km effects subdominant CP  dependence of 23 survival and conversion probabilities opposite Chaterjee,Ghoshal, Goswami, Raut, 2013 PANE 2018 , ICTP 27 Srubabati Goswami

Octant sensitivity: Atmospheric neutrinos Chaterjee,Ghoshal, Goswami, Raut, 2013 For Liquid Argon detector 50 kton Both Muon and Electron Events Barger et al., 2012 Matter effect breaks octant degeneracy in the muon channel Resultant octant sensitivity is due to both channels PANE 2018, ICTP 28 Srubabati Goswami

Muon vs Electron events Liquid Argon (500 kty) Atmospheric muon flux > electron flux P  P and opposite octant sensitivity  e  P has no dependence on ee 23  Dependence on stronger for muons 23 45  Away from muon contribution is more Chatterjee,Ghoshal, Goswami, Raut, 2013 PANE 2018, ICTP 29 Srubabati Goswami