GLOBAL ANALYSIS OF NEUTRINO DATA

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1 GLOBAL ANALYSIS OF NEUTRINO DATA Stony Brook & IFIC-Valencia) Nobel Syposiu, August 4 Introduction: The Paraeters of the New Minial Standard Model Orthodox Global Fits Solar and Reactor Neutrinos Atospheric and LBL Neutrinos Mixing Unorthodox Fits: Constraints on Extensions of the NMSM: LSND+Karen and Sterile neutrinos: 4 Mixing Tests of Fundaental Syetries: CPT, LI, WEP Suary In collaboration with J Bahcall, M Maltoni, CPeña-Garay and A Sirnov

2 = EM ED <; / % ' ) % $! # $! * + & ' #, & in the SM The SM is a gauge theory based on the syetry group There is no Accidental global syetry: strictly assless When SM was built upper bounds on K T) ν Q T 6 7 J K< L; 6 7? BA C = N FHG DG I O ) > > Neutrinos are conjured to be assless and left-handed ) 6 7 8:9 ; = >

3 - - & We have learned: Atospheric disappear ) ost likely to KK: accelerator disappear at K with -distortion ) Solar convert to or & ) KaLAND: reactor disappear at K with -distortion CL) LSND found evidence for

4 - - & We have learned: Atospheric disappear ) ost likely to KK: accelerator disappear at K with -distortion ) Solar convert to or & ) KaLAND: reactor disappear at K with -distortion CL) LSND found evidence for All this iplies that neutrinos are assive

5 Effects of Mass Neutrino asses ust have kineatic effects at soe level Also if neutrinos have a ass the charged current interactions of leptons are not diagonal sae as quarks)? J? # J νj u j W + W + _ l i _ d i SM gauge invariance does not iply syetry Total lepton nuber can be or cannot be still a syetry depending on whether neutrinos are Dirac or Majorana

6 Mass Questions # To fully deterine the lepton flavour sector we want to know: * How any,, assive and their asses * Their ixing: angles * Their CP properties: Dirac neutrino lepton nuber is conserved Majorana neutrino antineutrino lepton nuber is violated antineutrino phases extra phases

7 extra phases antineutrino angles phases # Mass Questions To fully deterine the lepton flavour sector we want to know: * How any,, assive * Their ixing: * Their CP properties: Dirac neutrino lepton nuber is conserved Majorana neutrino antineutrino lepton nuber is violated For exaple for s : Mixing angles + 1 Dirac Phase + +Majorana Phases and their asses

8 Effects of Mass: Oscillations If neutrinos have ass, a weak eigenstate produced in is a linear cobination of the ass eigenstates ) : After a distance -it can be detected with flavour ; with probability ; Re ' &! # I! $#! ev K/GeV % depends on Theoretical Paraeters The ass differences and Dirac phases) The ixing angles and on Two Experiental Paraeters: The neutrino energy -Distance source to detector No inforation on ass scale nor Majorana versus Dirac *nature

9 Counts/day/5 MeV Global Fits: Solar Neutrinos SNU) SNO Ph-I D-N Spectru 4 Points) SNU) SK Zenith spectru 44 Data points) Night Day Kinetic energy MeV) Counts/day/5 MeV a) b) Kinetic energy MeV) SNOII spectru unconstrained fluxes stat) stat) stat) syst) syst) syst)

10 Solar Neutrinos: Oscillation Solutions RATES ONLY SK and SNO E and t dependence GLOBAL LMA LMA SMA -7 1 LOW SMA, LOW, VAC at VAC ev 1 )

11 / ) 4 Terrestrial Test of LMA: KaLAND Search on at L 18 k reactors, few MeV: In : Deficit Observed In 4: Significant Energy Distortion MeV) delayed E Nobs/Nexp ILL Savannah River Bugey Rovno Goesgen Krasnoyarsk Palo Verde Chooz KaLAND Distance to Reactor ) Events / 45 MeV 6 4 no-oscillation best-fit oscillation accidentals KaLAND data E MeV) Fri Jun 11 11:4: 4 propt

12 ev ) ev ) Test of LMA: KaLAND Oscillation Analysis Our binned analysis 1): tan θ tan θ ev

13 - CHOOZ Negative search with source: Nuclear Reactor at k

14 Cobined Solar and KaLAND Analysis 1-5 ev ) All free + Lu constraint Before Nu4 tan θ All free + Lu constraint After Nu4 4 6 tan θ ev

15 Atospheric Neutrinos Coplete SKI data: down-going [not to scale] p, He L ~ 1- k + π +, K µ + e + atosphere zenith angle detector ν µ ν µ ν e L 5 k L 1 4 k EARTH L k up-going

16 & Atospheric Neutrinos: Oscillation Solutions : best channel 1-1-di [ev ] ev 1 - -di tan θ

17 & Matter effects Atospheric Neutrinos: Oscillation Solutions : best channel 1-1-di [ev ] ev 1 - -di : Excluded at tan θ 5Bad fit to observed SM like distributions) Strongly liited subdoinant contribution in ixing because of CHOOZ : Disfavoured at Flatter upgoing-! distribution ) Liited subdoinant contribution in 4 ixing

18 I G I G I G ATM Test at Long Baseline Experients: KK KK MINOS Opera/Icarus at KEK Kaiokande L=5 k at Ferilab Soundan L=7 k at CERN Gran Sasso L=74 k KK 4: spectral distortion Confiration of ATM oscillations

19 Solar+Atospheric+Reactor+LBL Oscillations : angles, 1 CP-phase + Majorana phases) Two ass schees M solar solar atos 1 1 NORMAL INVERTED oscillation analysis

20 Solar+Atospheric+Reactor+LBL Oscillations : angles, 1 CP-phase + Majorana phases) Two ass schees M NORMAL atos 1 INVERTED solar solar 1 oscillation analysis Generic ixing effects: Interference of two wavelength oscillations Effects due to Difference between Inverted and Noral CP violation due to phase

21 # # solar and atospheric oscillations decouple # In the Hierarchical approxiation For Noral Inverted Solar and KaLAND Atospheric and KK

22 @ # # In the Hierarchical approxiation For Solar and KaLAND Atospheric and KK # solar and atospheric oscillations decouple Noral Inverted For Solar and KaLAND: Liit on Atos + KK: Independent of soe, Liit on Dependence on schee but too sall CHOOZ: For 6 K B@ ev liit on All data prefers sall

23 @ # # In the Hierarchical approxiation For Solar and KaLAND Atospheric and KK # solar and atospheric oscillations decouple Noral Inverted For Solar and KaLAND: Liit on Atos + KK: Independent of soe, Liit on Dependence on schee but too sall CHOOZ: For 6 K B@ ev liit on,, very siilar to analysis All data prefers sall

24 : Three Neutrino Oscillations Projected allowed regions dof) Best Fit: ev ev

25 B < B; B < K B B B < K ; B < K 9 B < B; # # B B < B < B < B < A B < ; B < ; B < < < A K B < B : Three Neutrino Oscillations 1-paraeter allowed ranges ranges: The leptonic ixing atrix:

26 4 # 8? 4 Beyond Hierarchical: effects in ATM Data Best at electron saples 1 Noral 1 Inverted 1 1 N e / N e For and : N e / N e 9 9 SK sub-gev e) SK sub-gev e) Noral SK ulti-gev e) cos θ cos θ Inverted SK ulti-gev e) Sensitivity to Octant of!!! Most iportant for Sub-GeV e For and $ Most iportant for Muli-GeV e the opposite:

27 effects in ATM Data: Present 1 - Sub-GeV e+µ) Contained µ) 1 [ev ] 1-1 = ev 1 = 1-4 ev 1 [ev ] χ SK+CHOOZ [ev ] Multi-GeV e+µ) Upgoing µ) sin θ sin θ sin θ sin θ

28 ' ; ' 1 1 Neutrino Mass Scale Oscillation analysis lower bound on heaviest ass Upper bounds fro: : for both Dirac or Majorana s at 95 % CL) -less Double- decay: E ' theor uncert 9% CL) only for Majorana s Sensitive to Majorana CP phases COSMO:WMAP+LSS

29 ' ' ' Neutrino Mass Scale Global oscillation analysis Correlated ranges for, and Fogli et al hep-ph/4845) Noral Mass Schee ) Inverted Mass Schee )

30 & / - LSND The only short distance signal for oscillation: Observed with probability with MeV )searched for the sae signal and did not observe oscillations [ev /c 4 ] LSND+Karen Cobined Analysis % CL 1 9% CL 68% CL sin Θ

31 # Sterile Neutrinos and 4 Models Motivation: To explain LSND To fit solar, atospheric and LSND 4th sterile : 6 ixing angles and CP Dirac phases and Majorana phases 6 ass spectra of two type: atos solar solar atos atos solar LSND LSND LSND LSND LSND LSND atos solar solar atos solar atos + 1 +

32 ! 6 7 Sterile Neutrinos and 4 Models Maltoni et al hep-ph/1715 LSND [ev ] constrained by Bugey constrained by CDHSW+ATM NEV + at + KK LSND global LSND DAR % CL 99% CL sin θ LSND Only tiny regions at 99%CL Also constrained by coso bound on

33 ! Sterile Neutrinos and 4 Models Maltoni et al hep-ph/1715 LSND [ev ] constrained by Bugey constrained by CDHSW+ATM NEV + at + KK LSND global LSND DAR Mixed active-sterile oscillations Naively: Solar: At: % CL 99% CL sin θ LSND Only tiny regions at 99%CL Also constrained by coso bound on Disagreeent at ore than 4

34 Tests of Syetries: CPT CPT violation: sand scan have different asses Possibility of accoodating LSND? Atospheric Solar 1 Neutrinos 1 Atospheric, LSND KaLAND Antineutrinos

35 Tests of Syetries: CPT CPT violation: sand scan have different asses Possibility of accoodating LSND? But Data does not support this: ATM and s siilar wavelength Solar and KaLAND siilar Atospheric Solar 1 Neutrinos 1 Atospheric, LSND KaLAND Antineutrinos [ev ] 1 - sin θ sin θ [ev ] sin θ Best fit near CPT conservation sin θ 1

36 Tests of Syetries: CPT CPT violation: sand scan have different asses Possibility of accoodating LSND? But Data does not support this: ATM and s siilar wavelength Solar 1 1 and KaLAND siilar Atospheric Solar Neutrinos 1 1 Atospheric, LSND KaLAND All-But-LSND and LSND regions incopatible at 1 Antineutrinos 1 [ev ] sin θ LSND sin θ [ev ] sin θ Best fit near CPT conservation All-but-LSND sin θ LSND sin θ 1

37 Tests of Syetries: LI, WEP These New Physics Effects can also lead to -Oscillations But in general oscillation wavelegth has different dependence

38 Tests of Syetries: LI, WEP These New Physics Effects can also lead to -Oscillations But in general oscillation wavelegth has different Violation of Lorentz Invariance: dependence Non universal asyptotic velocity of neutrinos 9% CL Liit fro ATM data

39 Tests of Syetries: LI, WEP These New Physics Effects can also lead to -Oscillations But in general oscillation wavelegth has different Violation of Lorentz Invariance: dependence Non universal asyptotic velocity of neutrinos 9% CL Liit fro ATM data Violation of Weak Equivalence Principle: Non universal coupling of neutrinos to graviational potential 9% CL Liit fro ATM data

40 Suary Solar, Reactor, Atospheric and LBL data: Perfect in -oscillations ranges) ev and leptonic ixing atrix: Accoodating LSND: A proble +1 still arginally at 99%CL with ev + sterile liits fro Solar and ATM incopatible CTP violation incopatible at ore than Neutrino data provides interesting liits on fundaental syetries CPT, LI, WEP

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