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MEASUREMENT OF THE NEUTRINO MASS HIERARCHY IN THE DEEP SEA J. Brunner.

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Presentation on theme: "MEASUREMENT OF THE NEUTRINO MASS HIERARCHY IN THE DEEP SEA J. Brunner."— Presentation transcript:

1 MEASUREMENT OF THE NEUTRINO MASS HIERARCHY IN THE DEEP SEA J. Brunner

2 Matter effects & Mass Hierarchy Solar Neutrinos : Matter effects inside sun  m 2 > m 1 Matter effects in Earth (not yet measured !)  m 3 >< m 1,m 2 Normal Hierarchy Inverted Hierarchy

3 Matter effects & Mass Hierarchy e see additional potential due to W-exchange in +e  +e scattering Illustration for constant electron density n e At resonant energy  13 maximal A changes sign with n e via / A changes sign with  m 2  mass hierarchy !

4 Example Earth Matter Effect : P( µ  e ) cos  = 0.6 Baseline = 7645 km Inclination = 36.9˚ Resonance energy Earth mantle : 6-7 GeV NH IH GLOBES

5 Example Earth Matter Effect : P( µ  µ ) cos  = 0.6 Baseline = 7645 km Inclination = 36.9˚ Resonance energy Earth mantle : 6-7 GeV NH IH GLOBES

6 Sensitivity Calculation Fit of event count in Energy-Zenith space Color code : bin-by-bin significance of hierarchy difference W. Winter : arXiv:1305.5539 Oscillation parameter fixedOscillation parameter fitted

7 ORCA Dense Mton detector with KM3Net design Oscillation Research with Cosmics in the Abyss Less than 20 MEuro with current KM3Net technology

8 Effective Mass From ORCA simulations (preliminary) Same function used for all CC interaction Same light output for µ and e  ok Conservative for  due to escaping neutrinos NC evaluated at E/2 A. Trovato (LNS)

9 PINGU – ORCA : Energy Energy reconstruction from total light yield Ice is a better calorimeter due to scattering Energy reconstruction from fitted track length PINGU ORCA ICRC 2013 : Contribution 164 ICRC 2013 : Contribution 555

10 PINGU – ORCA : Zenith angle Resolution close to kinematical limit Water is a better tracker due to absence of scattering PINGU ORCA ICRC 2013 : Contribution 555 ICRC 2013 : Contribution 164

11 Sensitivity Calculation A. Heijboer

12 PINGU : Sensitivity combined

13 ORCA Sensitivity  Comparable or Better ! Muons only 6 years Cascades Muons No particle ID Cascades better than Muons Combination improves sensitivity by about a factor 2

14 Huber : Sensitivity over time ArXiv:1311.1822

15 A NEUTRINO BEAM TOWARDS ORCA

16 Why consider Beams ? PINGU / ORCA Motivations Fast : Construction within few years Significant measurement after few years Stay within low budget Neutrino Beams Expensive & long(er) Timescale  counter intuitive Matter effects with Atmospheric Nu’s More challenging than originally hoped for Beam allows for complementary measurement Neutrino Beams Easier to motivate if pointing towards an existing detector Maybe possible in “parasitic mode”

17 Why consider Beams ? Recently : change of paradigm for European LBL program Opens new, so far neglected options

18 Optimal Baseline ? For L>2000km the oscillation probabilities are always well separated for both MH hypotheses To find optimal baseline calculate event rates N ~ 1/L 2 N ~ E (cross section) Fixed beam profile ORCA detector response NH IH

19 Optimal Baseline L=2600km maximizes the difference in event rates between two MH hypotheses Event rate difference NH - IH

20 Oscillation Probabilities All relevant oscillation probabilities taken into account Full 3-flavour treatment CP-phase variations included

21 Optimal Energy Range ? Cross section weighted sum of oscillation probabilities Allows to find optimal energy range for MH determination No flavour tagging or CC/NC separation used Kinematical suppression of  exploited NH / IHRatio of Integrals IH/NH (2.5 GeV - E max )

22 Optimal Energy Range “Event counting”, no flavour ID : 2-6 GeV 11-14% suppression of IH w.r.t. NH Ratio of Integrals IH/NH (2.5 GeV - E max )

23 Proton Accelerator Complex Protvino Presentation S. Ivanov (IHEP) on 22/11/2012 @ CERN  Talk Wednesday

24 Proton Accelerator Complex Protvino Presentation S. Ivanov (IHEP) on 22/11/2012 @ CERN

25

26 Protvino – ORCA Baseline 2588km ; beam inclination : 11.7˚ (cos  = 0.2) Deepest point 134km : 3.3 g/cm 3

27 SKAT bubble chamber Courtesy: R. Nahnhauer p target focus Decay pipe 55m Shielding SKAT 140m 270m 245m

28 Beam parametrisation (1988) Neutrino Focus Anti-Neutrino Focus Scaling to ANTARES site (0.245/2600) 2 Z. Phys. C 40 (1988) 487

29 Beam parametrisation (1988) Very clean µ beam Less than 1% contaminations from other flavours Most neutrinos between 2-8 GeV Z. Phys. C 40 (1988) 487

30 Off-Axis Beam : suppress HE tail Beam optimisation still to be done Off-axis or combination on-axis/off-axis might be favorable

31 Event rates - Signal Event numbers for 1.5 10 21 p.o.t.s (3 years NOVA beam) 20  statistical separation of both Mass Hierarchy hypotheses from signal 10000 muon events for beam normalisation 3.5% separation between MH hypotheses Other contributions:  : 1316 +/- 13 ; 1416 +/- 8 ; NC : 4732 µ CC e CC NH 1621 +/- 255 IH 497 +/- 100 NH 10927 +/- 24 IH 10548 +/- 43

32 Event rates – All Flavours & Mis-ID Event numbers for 1.5 10 21 pots 9-18% difference for NH/IH 7  statistical separation of MH hypotheses Can allow for 3-4 % syst. uncertainty No requirement of energy reconstruction trackscascades NH 7300 +/- 200 IH 6420 +/- 80 NH 10690 +/- 45 IH 10244 +/- 15

33 Flavour identification & Neutrino Energy Need to separate “tracks” from “cascades” 2004 @ Villars : C2GT project (F. Dydak) CERN to Gulf of Taranto

34 Flavour identification 2004 @ Villars : C2GT project (F. Dydak) Clean separation of µ CC and e CC at 0.8 GeV OM spacing 3m

35

36 Dense detector 3x3 with cone display Electron-Neutrino Event, C-Cone clearly visible E = 5 GeV ; E e = 4 GeV 50nsec 100 nsec

37 Synergies between potential Sites Modane 2393km Antares 2588km Gran Sasso 2189km Nemo 2574km Protvino 4.1˚ 11.0˚ 13.6˚

38 Conclusion Preliminary Performance Figures of ORCA encouraging Mass hierarchy measurement in the deep sea possible Upgraded proton accelerator at Protvino well suited for LBL towards Mediterranean Sea Needed : 10 21 p.o.t. within few years Perfect subject for Russian Mega-Science program Synergy with Underground Labs in the same beam Complementary to measurement with atmospheric Complementary between ORCA / PINGU  High Significance determination of Mass Hierarchy

39 Possible Timescale 2014-2015 : Finalize optimization work for both options Currently active groups : CPPM, APC, ECAP (Erlangen)  Publish comprehensive document ~2016 : Planning “Phase II” of KM3Net Parallel : Contact with Russian partners, LoI ? First encouraging contact 08/2013 (Y. Kudenko, INR) Start contact with Modane project(s) (ex LBNO) First discussion 08/2013

40 Backup

41 Neutrinos from Beams Eliminate ambiguities Improve mass hierarchy sensitivity arXiv:1301.4577 Narrow band beam 6-9 GeV 10 20 p.o.t.

42 P( µ  µ ) cos  = 0.1 Baseline = 1274 km Inclination = 5.7˚ GLOBES NH IH

43 P( µ  µ ) cos  = 0.2 Baseline = 2548 km Inclination = 11.5˚ GLOBES NH IH

44 P( µ  µ ) cos  = 0.3 Baseline = 3823 km Inclination = 17.4˚ GLOBES NH IH

45 P( µ  µ ) cos  = 0.4 Baseline = 5097 km Inclination = 23.6˚ GLOBES NH IH

46 P( µ  µ ) cos  = 0.5 Baseline = 6371 km Inclination = 30.0˚ GLOBES NH IH

47 P( µ  µ ) cos  = 0.6 Baseline = 7645 km Inclination = 36.9˚ GLOBES NH IH

48 P( µ  µ ) cos  = 0.7 Baseline = 8919 km Inclination = 44.4˚ GLOBES NH IH

49 P( µ  µ ) cos  = 0.8 Baseline = 10194 km Inclination = 53.1˚ GLOBES NH IH

50 P( µ  µ ) cos  = 0.9 Baseline = 11468 km Inclination = 64.2˚ GLOBES NH IH Beam to IceCube

51 P( µ  µ ) cos  = 1.0 Baseline = 12742 km Inclination = 90.0˚ GLOBES NH IH

52 Counting Muons from Beam Neutrinos Optimal Beamline : 7000-8000 km Favoured Option: FermiLab – KM3Net site in Mediterranean Sea 1300 versus 950 events for both mass hierarchy hypotheses in Mton underwater detector (ORCA)  Inverse approach : Counting “Electrons” arXiv:1301.4577

53 P( µ  e ) cos  = 0.1 Baseline = 1274 km Inclination = 5.7˚ GLOBES (CP-phase varied in steps of 30˚) NH IH

54 P( µ  e ) cos  = 0.2 Baseline = 2548 km Inclination = 11.5˚ GLOBES NH IH

55 P( µ  e ) cos  = 0.3 Baseline = 3823 km Inclination = 17.4˚ GLOBES NH IH

56 P( µ  e ) cos  = 0.4 Baseline = 5097 km Inclination = 23.6˚ GLOBES NH IH

57 P( µ  e ) cos  = 0.5 Baseline = 6371 km Inclination = 30.0˚ GLOBES NH IH

58 P( µ  e ) cos  = 0.6 Baseline = 7645 km Inclination = 36.9˚ GLOBES NH IH

59 P( µ  e ) cos  = 0.7 Baseline = 8919 km Inclination = 44.4˚ GLOBES NH IH

60 P( µ  e ) cos  = 0.8 Baseline = 10194 km Inclination = 53.1˚ GLOBES NH IH

61 P( µ  e ) cos  = 0.9 Baseline = 11468 km Inclination = 64.2˚ GLOBES NH IH Beam to IceCube

62 P( µ  e ) cos  = 1.0 Baseline = 12742 km Inclination = 90.0˚ GLOBES NH IH

63 Oscillation parameters Taken from Global Fit (Fogli et al.) for both hierarchy options CP phase left free

64 Neutrino Cross sections Simple parton scaling assumed (QE, Res. ignored) Flavour universality m  threshold NC approximation

65 Neutrino Cross sections Simple parton scaling assumed (QE, Res. ignored) Flavour universality m  threshold NC approximation NC, CC: e µ  Solid : neutrino, dashed : antineutrino

66 Event rates Here : no flavour misidentification CC Rates NC Rates

67 Event rates Include Background and Flavour tagging Total Background : Total Event Rate :

68 Flavour identification Misidentification probability : assume same for both directions 50% at 2 GeV  random ; 20% at 5 GeV ; 10% at GeV

69 V. Ludwig (ECAP)

70 Systematic Uncertainties Detector Response Water parameters – Extensively studied in ANTARES Neutrino flux – Can be monitored with muon events Neutrino Cross Section – Ongoing and planned short baseline Experiments Oscillation parameters – ORCA with atmospheric neutrinos

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