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31 October 2008 Group seminar 1 Hong Kong

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Page 1: 31 October 2008Group seminar1 Hong Kong. 31 October 2008Group seminar2 Christchurch Home to the Canterbury Crusaders rugby team

31 October 2008 Group seminar 1

Hong Kong

Page 2: 31 October 2008Group seminar1 Hong Kong. 31 October 2008Group seminar2 Christchurch Home to the Canterbury Crusaders rugby team

31 October 2008 Group seminar 2

Christchurch

Home to the Canterbury Crusaders rugby team

Page 3: 31 October 2008Group seminar1 Hong Kong. 31 October 2008Group seminar2 Christchurch Home to the Canterbury Crusaders rugby team

31 October 2008 Group seminar 3

Maori welcome

Page 4: 31 October 2008Group seminar1 Hong Kong. 31 October 2008Group seminar2 Christchurch Home to the Canterbury Crusaders rugby team

31 October 2008 Group seminar 4

What do you mean where are the cubicles?

This the NU-LAB not the NEW LAV!

Page 5: 31 October 2008Group seminar1 Hong Kong. 31 October 2008Group seminar2 Christchurch Home to the Canterbury Crusaders rugby team

31 October 2008 Group seminar 5

Summary of Neutrino08

Robert L. Flack

Thanks to the group and the graduate school for jointly funding my attendance at the conference.

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31 October 2008 Group seminar 6

The conference was hosted by the University of Canterbury, Christchurch, NZ.

http://www2.phys.canterbury.ac.nz/~jaa53/index.htm

50 plenary and >100 “beer and pizza” talks.

This talk comes with a “health warning”; the words are a mixture of mine and the author and I apologise if I misrepresent or misinterpret any of the speakers.

Therefore this is highly personal review of the plenary talks.

Page 7: 31 October 2008Group seminar1 Hong Kong. 31 October 2008Group seminar2 Christchurch Home to the Canterbury Crusaders rugby team

31 October 2008 Group seminar 7

Ernest Rutherford (Cecilia Jarlskog)

He was born in Spring Grove, Nelson, New Zealand in 1871. He attended Canterbury University and his laboratory still exists and can be visited to this day.

Cecilia pointed out that although he was working in England at the time he was not proposed by any English physicists.

It is the 100th anniversary of the award of the 1908 Nobel Prize for chemistry to Ernest Rutherford for his work on radioactivity.

Page 8: 31 October 2008Group seminar1 Hong Kong. 31 October 2008Group seminar2 Christchurch Home to the Canterbury Crusaders rugby team

31 October 2008 Group seminar 8

Properties of neutrinos

(Boris Kayser)

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31 October 2008 Group seminar 9

Oscillation data

What is the absolute mass scale?How far above zero is the pattern?

Cosmological data

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31 October 2008 Group seminar 10

If neutrinos do have Majorana masses then they must have a very different origin to quark and charged lepton masses.

Do neutrinos have Majorana masses?

Majorana masses for quarks and charged leptons are forbidden due to charge conservation.

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31 October 2008 Group seminar 11

What are the neutrino dipole moments?

In the SM loop diagrams like this produce a dipole moment for a Dirac neutrino:

A Majorana neutrino cannot have a dipole moment.

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31 October 2008 Group seminar 12

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31 October 2008 Group seminar 13

Double beta decay

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31 October 2008 Group seminar 14

NEMO 3 - New result: 48Ca

Cut at 0

Cut at 1.5 MeV

E1 + E2 (MeV)

High bkgs here due to contamination with 90Sr.

Preliminary results: T1/2 (2 = [4.4 +0.5-0.4 (stat) ± 0.4 (syst)] x 1019

y

T1/2 (0) >1.3 x1022 y (90% C.L) <m> < 29.6 eV (90%CL), Eff. 22% Refs: E Caurrier et al., Phys.

Rev. Lett. 100 (2008) 052503 (NME)

133 eventsS/B 6.76

948 days7g

NEMO-3 NEMO-3

(Shiva King)

Page 15: 31 October 2008Group seminar1 Hong Kong. 31 October 2008Group seminar2 Christchurch Home to the Canterbury Crusaders rugby team

31 October 2008 Group seminar 15

NEMO 3 - New result: 96Zr

Preliminary result:96Zr: T1/2 (2νββ) = [2.3 ± 0.2(stat) ± 0.3(syst) ] 1019 y

T1/2 (0νββ) = 8.6 1021 y (90% C.L) <m> < 7.4 - 20.1 eV (90%CL), Eff. 19% Refs for NME : Simkovic, et al., Phys. Rev. C 77 (2008) 045503 Kortelainen and Suhonen, Phys. Rev. C 76 (2007) 024315

925 days S/B 1.019.41g

NEMO-3 NEMO-3

(Matt Kauer)

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31 October 2008 Group seminar 16

Recent result: 150Nd Moriond

Mass = 37g

Preliminary results: T1/2 (2νββ) = [9.20 +0.25-0.22 (stat) ± 0.072 (syst)] x 1018 y

Expected T1/2 (0νββ) = 1.45 x 1022 y Observed T1/2 (0νββ) = 1.8 x 1022 y (90% C.L.) Eff. 19% <m> < 1.7 – 2.4 eV (90%CL), QRPA (2007, corrected paper compared to 2006)deformation not taken into account<m> < 4.8-7.6 eV: pseudo-SU(3) Hirsh (95) deformation taken into account Ref for NME : V. Rodin et al., Nucl. Phys. A 793 (2007) 213. J.H. Hirsch et al., Nucl. Phys. A 582 (1995) 124.

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31 October 2008 Group seminar 17

From NEMO 3 to SuperNEMO

7 kg 100-200 kg isotope mass M

18 % ~ 30 %

isotope 100Mo

82Se - baseline

(150Nd if it can be enriched)

T1/2 () > ln 2 M Tobs

N90

NA

A

NEMO-3 SuperNEMO

internal contaminations 208Tl and 214Bi in the foil

208Tl: < 20 Bq/kg214Bi: < 300 Bq/kg

208Tl Bq/kg

if 82Se: 214Bi 10 Bq/kg

T1/2() > 2 x 1024 y<m> < 0.3 – 0.9 eV

T1/2() > 1026 y<m> < 0.04 - 0.11 eV

energy resolution (FWHM) 8% @ 3MeV 4% @ 3 MeV

efficiency

Page 18: 31 October 2008Group seminar1 Hong Kong. 31 October 2008Group seminar2 Christchurch Home to the Canterbury Crusaders rugby team

31 October 2008 Group seminar 18

Scintillators used as a source in double beta decay experiments (M. Chen)

Q-values:48Ca, 4.27MeV150Nd, 3.37MeV100Mo, 3.03MeV82Se, 3.00MeV136Xe, 2.48MeV76Ge, 2.04MeV

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31 October 2008 Group seminar 19

SNO+

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31 October 2008 Group seminar 20

Neutrino mass = 0.15eV

Neutrino mass = 0.1eV

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31 October 2008 Group seminar 21

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31 October 2008 Group seminar 22

Neutrino oscillation

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31 October 2008 Group seminar 23

Latest MINOS results (H. Gallagher)

Preliminary result: arXiv:hep-ex/0806.2237

Charged current

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31 October 2008 Group seminar 24

Preliminary results

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31 October 2008 Group seminar 25

Neutral current analysisA search for evidence of oscillations to sterile neutrinos

Oscillation parameters are fixed

Reconstructed energy of NC-like events in the far detector

Page 26: 31 October 2008Group seminar1 Hong Kong. 31 October 2008Group seminar2 Christchurch Home to the Canterbury Crusaders rugby team

31 October 2008 Group seminar 26

Preliminary results

Preliminary result: arXiv:hep-ex/0807.2424

Page 27: 31 October 2008Group seminar1 Hong Kong. 31 October 2008Group seminar2 Christchurch Home to the Canterbury Crusaders rugby team

31 October 2008 Group seminar 27

Super-K (J. Raaf)

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31 October 2008 Group seminar 28

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31 October 2008 Group seminar 29

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31 October 2008 Group seminar 30

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31 October 2008 Group seminar 31

3rd and final phase of SNO (R. Robertson)

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31 October 2008 Group seminar 32

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31 October 2008 Group seminar 33

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31 October 2008 Group seminar 34

Borexino (C. Galbiati)

Matter dominatedoscillations due to high density of electrons in the core of the sunMSW-effect.

Low energy vacuum oscillations.

Vacuum – matter transition region, 1 – 2 MeV

Page 35: 31 October 2008Group seminar1 Hong Kong. 31 October 2008Group seminar2 Christchurch Home to the Canterbury Crusaders rugby team

31 October 2008 Group seminar 35

Borexino (C. Galbiati)

Page 36: 31 October 2008Group seminar1 Hong Kong. 31 October 2008Group seminar2 Christchurch Home to the Canterbury Crusaders rugby team

31 October 2008 Group seminar 36

192 days of data taking

Page 37: 31 October 2008Group seminar1 Hong Kong. 31 October 2008Group seminar2 Christchurch Home to the Canterbury Crusaders rugby team

31 October 2008 Group seminar 37

Borexino (C. Galbiati)

Page 38: 31 October 2008Group seminar1 Hong Kong. 31 October 2008Group seminar2 Christchurch Home to the Canterbury Crusaders rugby team

31 October 2008 Group seminar 38

New detector developments

Page 39: 31 October 2008Group seminar1 Hong Kong. 31 October 2008Group seminar2 Christchurch Home to the Canterbury Crusaders rugby team

31 October 2008 Group seminar 39

Coherent neutrino scattering (J. Collar)

This is a SM process but has yet to be observed.

The cross-section is enhanced if the energy of the neutrino is less than a few tens of MeV.

Cross-section is proportional to N2.

Small detectors~1 kg.

Page 40: 31 October 2008Group seminar1 Hong Kong. 31 October 2008Group seminar2 Christchurch Home to the Canterbury Crusaders rugby team

31 October 2008 Group seminar 40

Coherent neutrino scattering (J. Collar)

So far this effect has not been observed

Page 41: 31 October 2008Group seminar1 Hong Kong. 31 October 2008Group seminar2 Christchurch Home to the Canterbury Crusaders rugby team

31 October 2008 Group seminar 41

Megaton Detectors(Andre Rubbia)

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31 October 2008 Group seminar 42

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31 October 2008 Group seminar 43

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31 October 2008 Group seminar 44

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31 October 2008 Group seminar 45

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31 October 2008 Group seminar 46

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31 October 2008 Group seminar 47

Implications of results from cosmic rays including the Pierre Auger

observatory.(Subir Sakar and Estaban Roulet)

Page 48: 31 October 2008Group seminar1 Hong Kong. 31 October 2008Group seminar2 Christchurch Home to the Canterbury Crusaders rugby team

31 October 2008 Group seminar 48

The Pierre Auger Observatory

Page 49: 31 October 2008Group seminar1 Hong Kong. 31 October 2008Group seminar2 Christchurch Home to the Canterbury Crusaders rugby team

31 October 2008 Group seminar 49

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31 October 2008 Group seminar 50

Cosmic ray flux is suppressedat the GZK (> 6 sigma).

20 out of 27 of the most energetic CRs (~10^18eV) point back to within 3 degrees of an AGN. Expected 6.Also the sources must be nearby (GZK horizon).

There must be cosmic neutrinos with similar energies.None found to-date.

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31 October 2008 Group seminar 51

The primary particles in the CRs are not photons

The data from Auger indicates that the main primary maybe heavy nucleii.

These are more easily accelerated to these extremely high energies.

Auger found that the

Page 52: 31 October 2008Group seminar1 Hong Kong. 31 October 2008Group seminar2 Christchurch Home to the Canterbury Crusaders rugby team

31 October 2008 Group seminar 52

Heavy neutrinos and geo-neutrinos.

Page 53: 31 October 2008Group seminar1 Hong Kong. 31 October 2008Group seminar2 Christchurch Home to the Canterbury Crusaders rugby team

31 October 2008 Group seminar 53

Search for heavy neutrinos(Vanucci)

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31 October 2008 Group seminar 54

PS 191 was used to search for heavy neutrinos.

Not excluded by the MINIBOONE excess

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31 October 2008 Group seminar 55

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31 October 2008 Group seminar 56

Geo-Neutrinos (Learned + McDonough)

Measuring the electron antineutrino flux of the Earth will improve our models of its structure. The questions geologists want our help with are:

Page 57: 31 October 2008Group seminar1 Hong Kong. 31 October 2008Group seminar2 Christchurch Home to the Canterbury Crusaders rugby team

31 October 2008 Group seminar 57

The energy spectrum of electron antineutrinos from the Earth

The region KamLAND can detect

Page 58: 31 October 2008Group seminar1 Hong Kong. 31 October 2008Group seminar2 Christchurch Home to the Canterbury Crusaders rugby team

31 October 2008 Group seminar 58

Large scintillator detectors used to detect antineutrinos from the Earth

Page 59: 31 October 2008Group seminar1 Hong Kong. 31 October 2008Group seminar2 Christchurch Home to the Canterbury Crusaders rugby team

31 October 2008 Group seminar 59

I have made a contribution to the proceedings - arXiv:0810.5497

Being relatively new to the neutrino field I found the conference educational, well organised and the people in NZ are friendly and welcoming.

I certainly would like to go to the next one in Athens 2010.

Travel tips:Never go via Hong kong because the women in my family expected me to buy too many “girly” gifts for them; handbags, etc!

Don’t put bottles of orange juice in your rucksack because it doesn’t go well with travel documents. The check in staff were not impressed!

I can recommend the rucksack shop at Christchurch airport. The lady who runs it is very helpful to dumb travellers.

Conclusion