31 october 2008group seminar1 hong kong. 31 october 2008group seminar2 christchurch home to the...
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31 October 2008 Group seminar 1
Hong Kong
31 October 2008 Group seminar 2
Christchurch
Home to the Canterbury Crusaders rugby team
31 October 2008 Group seminar 3
Maori welcome
31 October 2008 Group seminar 4
What do you mean where are the cubicles?
This the NU-LAB not the NEW LAV!
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.
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.
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.
31 October 2008 Group seminar 8
Properties of neutrinos
(Boris Kayser)
31 October 2008 Group seminar 9
Oscillation data
What is the absolute mass scale?How far above zero is the pattern?
Cosmological data
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.
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 13
Double beta decay
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)
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)
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.
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
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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SNO+
31 October 2008 Group seminar 20
Neutrino mass = 0.15eV
Neutrino mass = 0.1eV
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31 October 2008 Group seminar 22
Neutrino oscillation
31 October 2008 Group seminar 23
Latest MINOS results (H. Gallagher)
Preliminary result: arXiv:hep-ex/0806.2237
Charged current
31 October 2008 Group seminar 24
Preliminary results
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
31 October 2008 Group seminar 26
Preliminary results
Preliminary result: arXiv:hep-ex/0807.2424
31 October 2008 Group seminar 27
Super-K (J. Raaf)
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31 October 2008 Group seminar 30
31 October 2008 Group seminar 31
3rd and final phase of SNO (R. Robertson)
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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
31 October 2008 Group seminar 35
Borexino (C. Galbiati)
31 October 2008 Group seminar 36
192 days of data taking
31 October 2008 Group seminar 37
Borexino (C. Galbiati)
31 October 2008 Group seminar 38
New detector developments
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.
31 October 2008 Group seminar 40
Coherent neutrino scattering (J. Collar)
So far this effect has not been observed
31 October 2008 Group seminar 41
Megaton Detectors(Andre Rubbia)
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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)
31 October 2008 Group seminar 48
The Pierre Auger Observatory
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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.
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
31 October 2008 Group seminar 52
Heavy neutrinos and geo-neutrinos.
31 October 2008 Group seminar 53
Search for heavy neutrinos(Vanucci)
31 October 2008 Group seminar 54
PS 191 was used to search for heavy neutrinos.
Not excluded by the MINIBOONE excess
31 October 2008 Group seminar 55
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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:
31 October 2008 Group seminar 57
The energy spectrum of electron antineutrinos from the Earth
The region KamLAND can detect
31 October 2008 Group seminar 58
Large scintillator detectors used to detect antineutrinos from the Earth
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.
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