Long baseline experiments

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1 Mauro Mezzetto, Istituto Nazionale Fisica Nucleare, Padova Long baseline experiments Present Status Concepts, strategies, challenges The two players: Dune and Hyper-Kamiokande Conclusions M. Mezzetto, INFN Padova, TAUP 2015, Torino 1

2 We are talking of Long Baselines because Super-Kamiokande discovered neutrino oscillations with m ev 2 The discovery of neutrino oscillations had been made by Super-Kamiokande in 1998 by measuring atmospheric neutrinos. Concluding slide of the original talk of T. Kajita at Neutrino 98 Long baseline: 1 GeV neutrinos have max of oscillations at about 500 Km. Very much reduced fluxes: need of gigantic detectors deep underground: ideal detector SK (it s approaching 20 years of leading edge operations).

3 The progress on atmospheric parameters Atmospherics 99% CL 1999 SuperK 2002 K2K Along time changed variables, fitting methods, conventions, assumptions Results also from Opera, Antares, IceCube. M. Mezzetto, INFN Padova, TAUP 2015, Torino 3

4 We now have a ν τ gallery by the Opera experiment See N. Di Marco talk in Neutrinos A M. Mezzetto, INFN Padova, TAUP 2015, Torino 4

5 And recently LBL surpassed atmospherics in precision T2K: Phys.Rev.Lett. 112 (2014) 18, Antineutrinos M. Mezzetto, INFN Padova, TAUP 2015, Torino 5

6 The progress on Solar parameters Solars 3σ 1999 SAGE Homestake 2002 Gallex/GNO Along time changed variables, fitting methods, conventions, assumptions. And also some important cross section both at the source and the detector, not to mention the new evaluation of reactor antineutrino rates M. Mezzetto, INFN Padova, TAUP 2015, Torino 6 SNO

7 θ 13 The progress on θ 13 90%CL At Neutel 2010 Fogli et al. Start claiming that global fits Favour sin 2 2θ 13 =0.1 at 1.5σ 12 years to improve Chooz and θ 13 was just behind the corner M. Mezzetto, INFN Padova, TAUP 2015, Torino 7

8 Present situation See A. Marrone in Neutrinos A Precision era started Can precision constrain new physics? What about unitarity? (It s assumed in all these plots) M. Mezzetto, INFN Padova, TAUP 2015, Torino 8

9 What s missing Neutrino mass ordering ν e can be the heaviest or the lightest of neutrinos Impacts on prospects of double beta decay detection Leptonic CP violation The last parameter of the Standard Model to be measured Intringuing correlations with matter/antimatter asymmetry in the Universe Phys. Rev. D75 (2007) atmosperic: atmospheric: atmospheric: M. Mezzetto, INFN Padova, TAUP 2015, Torino 9

10 Short term: short baselines (sterile neutrinos) The 3 ν model is matched by 4 anomalies conspiring to the same oscillation parameters LSND: a 3.5 σ excess of ν e events in a neutrino beam created by pion decays at rest. First paper on 1995, the experiment has never been repeated. MiniBoone: a 10 years effort at Fermilab to check the LSND result at different energies (but same L/E), the final result had been inconclusive. Reactor anomaly: recent recalculation of neutrino fluxes at reactors showed an enhancement of about 3.5% of absolute fluxes with respect to previous calculations: all the reactor experiments at very short baselines could be reinterpreted as evidence of ν e disappearance (about 2.5 σ). Recent results on reactor experiments seriously match the reliability of these recent calculations. Source calibration of Gallex and SAGE: the source calibration of these experiments showed a 15% deficit of ν e events. To be noted that the calibration had been designed and funded to check the efficiency of the detectors, while the sterile evidence is there assuming 100% efficiency of the detectors. Overall fit: the 4 anomalies can accommodated in the same oscillation model by adding a 4 th, sterile, neutrino, with a mass of about 1 ev, nevertheless tensions exist in the global fit Cosmology: severely constraints total number of neutrinos to 3 and their mass below 1 ev Most economical way to falsify steriles: a convincing null result from the source experiments at Borex (SOX) would falsify the sterile n interpretation of anomalies Most complete way to explore the phenomenology if steriles exist: the new short baseline project at Fermilab, with 3 liquid argon detectors, has the potential of fully exploit the several manifestations of sterile neutrinos.

Medium term: ν mass ordering Pure oscillation effects in ν e disappearance: Juno Matter effects in ν µ disappearance: INO, Pingu, Orca, HyperKamiokande Matter effects in ν e appearance: NOνA, Dune,

11 Medium term: ν mass ordering Pure oscillation effects in ν e disappearance: Juno Matter effects in ν µ disappearance: INO, Pingu, Orca, HyperKamiokande Matter effects in ν e appearance: NOνA, Dune, T2HK (Very) long baseline ν experiments have the best potential for this measurement but are also the most expensive and probably the last to come into play No needs of precision, the experiment has just to decide between +1 and -1. M. Mezzetto, INFN Padova, TAUP 2015, Torino 11

12 We are talking of measuring δcp because of a very favorable combination of parameters M. Mezzetto, INFN Padova, TAUP 2015, Torino 12

13 We are talking of measuring δcp because of a very favorable combination of parameters Also m 2 12 matters: m 2 12 < ev2 would prevent any CP sensitivity From CERN Yellow Report arxiv:hep-ph/ M. Mezzetto, INFN Padova, TAUP 2015, Torino 13

14 The value of θ 13 decides the strategy SMALL VALUES: ν µ ν e transitions are tiny Need large statistics and small background rates Transition asymmetry is large Little effect of systematic errors LARGE VALUES: ν µ ν e transitions are large Relaxed constraints on statistics and background rates Transition asymmetry is small Large effects of systematic errors Conventional neutrino beams are not enough Conventional neutrino beams maybe enough M. Mezzetto, INFN Padova, TAUP 2015, Torino 14

The value of θ 13 decides the strategy SMALL VALUES: LARGE VALUES: ν µ ν e transitions are tiny ν µ ν e transitions are large Need large statistics and small Relaxed constraints on statistics

15 The value of θ 13 decides the strategy SMALL VALUES: LARGE VALUES: ν µ ν e transitions are tiny ν µ ν e transitions are large Need large statistics and small Relaxed constraints on statistics background rates and background rates Transition asymmetry is New large concepts for neutrino beams, for the Transition asymmetry is small Little effect of systematic moment, errors have been abandoned Large effects of systematic errors CP violation searches are designed to use Conventional neutrino beams «brute force» upgrades on conventional Conventional neutrino beams are not enough neutrino beams maybe enough M. Mezzetto, INFN Padova, TAUP 2015, Torino 15

16 New concepts: Neutrino Factories S. Geer, Phys. Rev. D57 (1998) IDS-NF, arxiv: M. Mezzetto, INFN Padova, TAUP 2015, Torino 16

17 New concepts: Beta Beams P. Zucchelli, Phys.Lett. B532 (2002) Lindroos, MM, Imperial College Pr. (2010) M. Mezzetto, INFN Padova, TAUP 2015, Torino 17

18 What we know today about δ CP T2K (Phys.Rev. D88 (2013) 3, ) measures a combination of θ 13 and δ CP while reactors (PDG 2012) measure pure θ 13 effects. Their combination favours δ CP =-π/2 M. Mezzetto, INFN Padova, TAUP 2015, Torino 18

19 Hint of CP violation? See A. Marrone in Neutrinos A M. Mezzetto, INFN Padova, TAUP 2015, Torino 19

20 Hint of CP violation? See A. Marrone in Neutrinos A Adding information the «evidence» increases Only 8% of T2K stats and 0% of Noνa No antineutrino run Predictions of future sensitivities of T2K+Noνa don t include solars and atmosn t M. Mezzetto, INFN Padova, TAUP 2015, Torino 20

21 Two very recent results Antineutrinos at T2K (EPS 2015) Noνa, 7.6% of full statistics (LP2015) See B. Rebel in Neutrinos A Exposure: pot 3 events detected Excludes that ν e excess is due to unknown backgrounds 3 times more statistics next year M. Mezzetto, INFN Padova, TAUP 2015, Torino 21

22 Projection of T2K+Noνa at full statistics From T2K collaboration: PTEP 2015 (2015) 4, 043C01 CP MH Full statistics of the running experiments: T2K and Noνa, equal ν and ν runs, dashed lines: including systematics M. Mezzetto, INFN Padova, TAUP 2015, Torino 22

23 Good CP coverage requires order of 1 Mton x Mwatt x year M. Mezzetto, INFN Padova, TAUP 2015, Torino 23

experimental sensitivity) Varying θ13 at fixed luminosity Huber, MM, Schwetz, JHEP

24 Effects of systematic errors on CP sensitivity Since a long time they are known to be the real bottleneck (or in positive the only convincing way of enhancing the experimental sensitivity) Varying θ13 at fixed luminosity Huber, MM, Schwetz, JHEP 0803 (2008) 021 Varying luminosity at fixed θ13. M. Mezzetto, INFN Padova, TAUP 2015, Torino 24

25 Systematic errors The experience of T2K A sophisticated close detector station: ND280 + Ingrid The best quality hadroproduction data ever produced (NA61) already included A huge, qualified, effort by the largest collaboration ever seen in neutrino physics At present limited by statistics M. Mezzetto, INFN Padova, TAUP 2015, Torino 25

26 Two players: Dune and Hyper-Kamiokande

27 See G. De Rosa in Neutrinos A M. Mezzetto, INFN Padova, TAUP 2015, Torino 27

28 See M. Bishai in Neutrinos A M. Mezzetto, INFN Padova, TAUP 2015, Torino 28

29 CP violation: general considerations HK: short baseline no matter effects: pure CP but reduced MH Off axis reduced intrinsic ν e contamination, reduced NC backgrounds DUNE: Long baseline sensitive to matter effects: excellent performances in MH On axis: second oscillation maximum and sensitive to ν τ appearance (tiny effects at 1300 km) On axis: Extended lever of arm for measurement of oscillation parameters M. Mezzetto, INFN Padova, TAUP 2015, Torino 29

30 CP violation: just event numbers Which of the two has the best S/N? 10 years 6 years M. Mezzetto, INFN Padova, TAUP 2015, Torino 30

estimation extrapolating from Minos (no LAr close

31 CP violation: systematic errors HK estimation assuming identical close detector as T2K Dune estimation extrapolating from Minos (no LAr close detector data so far) M. Mezzetto, INFN Padova, TAUP 2015, Torino 31

32 M. Mezzetto, INFN Padova, TAUP 2015, Torino 32

33 Borrowed from M. Bishai talk M. Mezzetto, INFN Padova, TAUP 2015, Torino 33

34 Proton Decay HK DUNE Will improve Super-Kamiokande limits in very few channels, notably in the p K + ν channel M. Mezzetto, INFN Padova, TAUP 2015, Torino 34

Supernova Neutrinos HK Mainly ν e from ν e p e + p Burst from galactic center (10 kpc) 170,000 260,000 ν s Burst from Andromeda Galaxy 30 50 ν s Supernova relic ν 200

35 Supernova Neutrinos HK Mainly ν e from ν e p e + p Burst from galactic center (10 kpc) 170, ,000 ν s Burst from Andromeda Galaxy ν s Supernova relic ν 200 in 10 years DUNE Mainly ne from ν e + 40 Ar e + 40 K* Burst from galactic center (10 kpc) ~ 900 ν s in 10 kton detector M. Mezzetto, INFN Padova, TAUP 2015, Torino 35

far the best Spin Dependent (SD) and very competitive in the

36 WIMP annihilation at Sun SK updated results recently presented by Nakahata-san at Neutel 2015 HK sensitivity by far the best Spin Dependent (SD) and very competitive in the SI low WIMP mass region M. Mezzetto, INFN Padova, TAUP 2015, Torino 36

37 M. Mezzetto, INFN Padova, TAUP 2015, Torino 37

38 M. Mezzetto, INFN Padova, TAUP 2015, Torino 39

39 Conclusions Bright future for accelerator neutrino physics, unfortunately not in Europe. Main goal: CP violation in the leptonic sector But also unitarity tests of the 3ν mixing matrix The gigantic far detectors have an excellent non-accelerator physics program in their own The sophisticated close detectors will have their hard job in measuring neutrino cross sections in all their tricky manifestations M. Mezzetto, INFN Padova, TAUP 2015, Torino 40

The future of neutrino physics (at accelerators)

Mauro Mezzetto, Istituto Nazionale Fisica Nucleare, Padova The future of neutrino physics (at accelerators) Present Status Concepts, strategies, challenges The two players: Dune and Hyper-Kamiokande Conclusions