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Z.Djurcic, D.Leonard, A.Piepke Physics Dept, University of Alabama, Tuscaloosa AL
P.Vogel Physics Dept Caltech, Pasadena CA
A. Bellerive, M. Dixit, C. Hargrove, D. Sinclair Carleton University, Ottawa, CanadaW.Fairbank Jr., S.Jeng, K.Hall
Colorado State University, Fort Collins COM.Moe
Physics Dept UC Irvine, Irvine CAD.Akimov, A.Burenkov, M.Danilov, A.Dolgolenko, A.Kovalenko, D.Kovalenko, G.Smirnov, V.Stekhanov
ITEP Moscow, RussiaJ. Farine, D. Hallman, C. Virtue
Laurentian University, CanadaM.Hauger, F.Juget, L.Ounalli, D.Schenker, J-L.Vuilleumier, J-M.Vuilleumier, P.Weber
Physics Dept University of Neuchatel, Neuchatel SwitzerlandM.Breidenbach, R.Conley, C.Hall, A.Odian, C.Prescott, P.Rowson, J.Sevilla, K.Skarpaas, K.Wamba,
SLAC, Menlo Park CAE.Conti, R.DeVoe, G.Gratta, M.Green, T.Koffas, R.Leon, F.LePort, R.Neilson, S.Waldman, J.Wodin
Physics Dept Stanford University, Stanford CA
EEnriched nriched XXenon enon OObservatorybservatoryfor double beta decayfor double beta decay
Last decade: the age of ν physics
Discovery of ν flavor change:
• Solar neutrinos (MSW effect)• Reactor neutrinos (vacuum oscillation)• Atmospheric neutrinos (vacuum oscillation)• Loose ends: LSND results
So assuming that MiniBoone sees no oscillations,we know that:
•ν masses are non-zero,•There are 2.981±0.008 v (Z lineshape),•3 ν flavors were active in Big bang Nucleosynthesis
Drastically different mass scenarios are still allowed by the data
~2.8 eV From
tritium
en
dpoin
t(M
ain
tz an
d T
roitsk
)
~0.3 eVFrom
0νβ
β if ν is M
ajo
rana
~1 eVFro
m W
MA
P
Tim
e o
f flig
ht fro
m S
N198
7A
(PD
G 2
002)
23 eV
No real understanding why M so smallDirac vs Majorana neutrinos?Need a lepton number violating process…
decay can occur in two modes
a)Via the emission of 2’s:
A typical 2nd order nuclear process
b) A neutrinoless mode:Requires bothM0 and
decay a standard but small2nd order correction to regular decay
BUT in some cases is the onlyenergetically allowed
2 has beenobserved
experimentally
0 has neverbeen
observedexperimentall
y
0 sensitive to allneutrino masses
For 0 decay due to light Majorana ν masses:
where,
the effective Majorana neutrino mass,
FM and GTM nuclear matrix elements that canbe calculated,
0G a known phase-space factor,
02/1T the half-life time to be measured
12
0
2
0002/1
2,
FV
AGTee M
g
gMZEGTm
3
1
2
,i
iiieee mUm
2 spectrum(normalized to 1)
0 peak (5% FWHM)(normalized to 10-2)
0 peak (5% FWHM)(normalized to 10-6)
Summed electron energy in units of the kinematic endpoint (Q)
Detection of 0νββ DecayThe two e- energy sum is the primary tool
from S.R. Elliott and P. Vogel, Ann.Rev.Nucl.Part.Sci. 52 (2002) 115.
For further substantial progress we need tons of anappropriate isotope exposed for a long time
BUT there are problems
•In a bkgnd free environment mass sensitivity scales as
NtTm /1/1 02/1
•If bkgnd scales like Nt mass sensitivity scales as
4/102/1 /1/1 NtTm
Qualitatively new means are needed to suppressbkgnds and fully utilize the large fiducial mass
Xe is ideal for such a measurement• It is one of the easiest isotopes to enrich;
• Like argon, it represents a good ionization detecting medium;
• It exhibits substantial scintillation that can be used to complement the ionization detection;
• Can be re-purified during the experiment;
• No long lived Xe isotopes to activate;
• Its decay results in 136Ba that can be identified in its atomic form via techniques of high resolution optical spectroscopy.
22PP1/21/2
44DD3/23/2
22SS1/21/2
493nm493nm
650nm650nm
metastable 47smetastable 47s
Optical detection of a 136Ba+ atom (M. Moe PRC44(1991)931)
Resonant laser detection is:
•Highly sensitive, yielding >107
photons per atom;•Highly selective;•Extensively used in the atomic physics community.
Provides additionalconstraint
Huge bkgnd reductionpump probe
Detector R&D Program
• Single ion Ba+ tagging at different Xe pressures;
• LXe energy resolution;• LXe purification for long e- lifetime and
radioimpurities;
• Ba ion lifetime and grabbing from LXe;
• 136Xe Isotopic enrichment;
• Procurement and characterization of low radioactivity
materials;
• Construction/operation of a 200kg enriched 136Xe prototype detector;
Zero ion backgroundZero ion background
All above in UHV;Perform the sameexperiment in noblegas atmosphere
Millikan type experiment with the ion trap
1Lt Test Chamber
PMT
Ionization ReadoutPreamplifier
Energy Resolution Measurement Setup
Reconstruct energy as linearcombination of ionization andscintillation signals
There are indications thatcorrelations between the twovariables help improve energyresolution; J.Seguinot et al. NIM A354 (1995) 280
Clear anti-correlation on event-to-event basis is seen…
A linear combination of ionization and scintillation WILL optimize resolution
First E
XO published result i
n Phys.Rev.B
Resolution is optimized by a ~100-150 ‘mixing angle’
Ionization onlyIonization only
Ionization combinedIonization combinedwith scintillationwith scintillation
E.Conti et al Phys. Rev. B 68 (2003) 054201E.Conti et al Phys. Rev. B 68 (2003) 054201
3.3%@570keV3.3%@570keVor 1.6%@2.5MeVor 1.6%@2.5MeV
This is already the This is already the largest non-fissile largest non-fissile
isotope enrichment isotope enrichment program ever program ever entertained!entertained!
First 200 kg pilot production started in the Summer of 2001 First 200 kg pilot production started in the Summer of 2001 and was successfully completed in May 2003 and was successfully completed in May 2003
Xe leak monitoringXe leak monitoringstationstation
200kg 136Xe Prototype is an important step
• Need to test the detector technology, particularly the LXe option;
• Essential to understand backgrounds from radioactivity;
• Necessary to measure the 2 “background” mode;
• Test the production logistics and quality of 136Xe;
• 2000kg of natural Xe are already available by our collaborators at ITEP;
• Already a respectable (20x) decay experiment (no Ba-ion tagging at this stage);
Detector
• ~60 liters enriched liquid 136Xe,
– In low background teflon vessel– Surrounded and shielded by ~50 cm radially low
background thermal transfer fluid– Contained in a low background Cu double walled
vacuum insulated cryostat– Shielded by ~ 5 cm very low background Pb– Further shielded by ~20 cm low background Pb– Located ~800 m below ground in NaCl deposit – WIPP in
Carlsbad, New Mexico.
• Detector is a liquid TPC with photo-detectors to provide start time and improve energy resolution of the β’s.
Cryostat Cross Section
Condenser
Xenon Heater
should be
on this area
Xenon
Chamber
Support
Outer Copper Vessel
Inner Copper Vessel
FC-87
FC-87
1” thick Thermal Insulation (MLI-vacuum), not shown to scale
Outer Door
Inner Door
Xenon
Chamber
Refrigerant feedthroughsHeat Transfer Fluid In/Out
•Enriched Xe in hand.
•Clean rooms in commercial production.
•WIPP agreement, including Environmental Impact, complete.
•Swiss collaborators building cryostat.
•Xe purification and refrigeration issues through R&D, purchasing of components.
•Detector vessel, readout, and electronics being engineered.
•EXO could be in WIPP by Summer 2005, if technically limited.
Status
Assumptions: Assumptions: 1)1) 200kg of Xe enriched to 80% in 136200kg of Xe enriched to 80% in 1362)2) σσ(E)/E = 1.6% obtained in EXO R&D, Conti et al Phys Rev B 68 (2003) 054201(E)/E = 1.6% obtained in EXO R&D, Conti et al Phys Rev B 68 (2003) 0542013)3) Low but finite radioactive background: Low but finite radioactive background: 20 events/year in the ±220 events/year in the ±2σσ interval centered around the 2.481MeV endpoint interval centered around the 2.481MeV endpoint4)4) Negligible background from 2Negligible background from 2νββνββ (T (T1/21/2>1·10>1·102222yr R.Bernabei et al. measurement)yr R.Bernabei et al. measurement)
EXO 200kg prototype mass sensitivityEXO 200kg prototype mass sensitivity
Case Mass(ton)
Eff.(%)
Run Time(yr)
σE/E @ 2.5MeV
(%)
Radioactive
Background
(events)
T1/20ν
(yr, 90%CL)
Majorana mass(eV)
QRPA (NSM)
Prototype 0.2 70 2 1.6* 40 6.4*1025 0.18 (0.53)
Assumptions: Assumptions: 1)1) 80% enrichment in 13680% enrichment in 1362)2) Intrinsic low background + Ba tagging eliminate all radioactive backgroundIntrinsic low background + Ba tagging eliminate all radioactive background3)3) Energy res only used to separate the 0Energy res only used to separate the 0νν from 2 from 2νν modes: modes: Select 0Select 0νν events in a ±2 events in a ±2σσ interval centered around the 2.481MeV endpoint interval centered around the 2.481MeV endpoint4)4) Use for 2Use for 2νββνββ T T1/21/2>1·10>1·102222yr (Bernabei et al. measurement)yr (Bernabei et al. measurement)
** (E)/E = 1.6% obtained in EXO R&D, Conti et al Phys Rev B (E)/E = 1.6% obtained in EXO R&D, Conti et al Phys Rev B 68 (2003) 05420168 (2003) 054201†† (E)/E = 1.0% considered as an aggressive but realistic guess with large light(E)/E = 1.0% considered as an aggressive but realistic guess with large light collection areacollection area‡‡ QRPA: A.Staudt et al. Europhys. Lett.13 (1990) 31; Phys. Lett. B268 (1991) 312QRPA: A.Staudt et al. Europhys. Lett.13 (1990) 31; Phys. Lett. B268 (1991) 312## NSM: E.Caurier et al. Phys Rev Lett 77 (1996) 1954 NSM: E.Caurier et al. Phys Rev Lett 77 (1996) 1954
EXO neutrino effective mass sensitivityEXO neutrino effective mass sensitivity
Case Mass(ton)
Eff.(%)
Run Time(yr)
σE/E @ 2.5MeV
(%)
2νββBackgroun
d(events)
T1/20ν
(yr, 90%CL)
Majorana mass(meV)
QRPA‡ (NSM)#
Conservative 1 70 5 1.6* 0.5 (use 1) 2*1027 33 (95)Aggres
sive 10 70 10 1† 0.7 (use 1) 4.1*1028 7.3 (21)