Pauli. Davis Fermi. Majorana. Dirac. Koshiba. Reines. Pontecorvo. Goeppert-Mayer. Steve Elliott
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1 Davis Fermi Pauli Dirac Majorana Pontecorvo Reines Koshiba Goeppert-Mayer
2 Experimental Double Beta Decay Outline Experimental issues Upcoming experiments Conclusion
3 Example Decay Scheme 2-76 As Ge Endpoint Energy ββ Se In many even-even nuclei, β decay is energetically forbidden. This leaves ββ as the allowed decay mode.
4 Energy Spectrum for the 2e - Two Neutrino Spectrum Zero Neutrino Spectrum 1% resolution Γ (2 ν) = 100 * Γ (0 ν) Sum Energy for the Two Electrons (MeV) Endpoint Energy
5 ββ Decay Rates Γ 2 ν = G 2ν M 2 ν 2 Γ 0 ν = G 0ν M 0 ν 2 m ν 2 G are calculable phase space factors. G 0ν ~ Q 5 M are nuclear physics matrix elements. Hard to calculate. M ν is where the interesting physics lies.
6 What about mixing, m ν & ββ(0ν)? No mixing: m ββ = m νe = m 1 3 m ββ = U 2 ei m i ε virtual ν i i=1 ε= ±1, CP cons. exchange Compare to β decay result: 3 real ν m β = U 2 2 ei m i i=1 emission
7 An exciting time for ββ! For at least one neutrino: m i > δm 2 atmos 50meV For the next experiments: m ββ 50meV < m ββ > in the range of mev is very interesting.
8 The First Observation
9 Present Experimental Limits m ββ 1 M G 0ν τ 1/2 Half L ife <m ββ > Ge (IGEX ) N P of R A S 63, 1299 (2000) G e (H ei d -Mo sc) Dar k Mat ter 2000 Mo (ELEG A NTS ) N P A 611, 85 (1996) Te-130 (Cuoricino) P L B486, 13 (2000) Te-128 (Geochem) P R C 47, 806 (1993) Xe (Gotthard) PL B 434, 407 (1998 ) 160 x y ~ 3 30 m ev 190 x y ~ 3 00 m ev 0.52 x y ~6600 mev 1.44 x y ~1700 mev 6.9 x y ~1100 mev 4.4 x y ~2500 mev
10 Peak Hunting Mod. Phys. Lett. A16, 2409 (2001) Looking for a rare peak on a continuum background Counts Energy (kev)
11 A recent 20 claim Counts (/kev) The feature at 2038 kev is arguably present. This will probably require experimental testing Energy (KeV) 2050 Background level depends on intensity fit to other peaks. Counts (/kev) Energy (KeV)
12 Found Peaks PR D45, 2548 (1992) Need more than one experiment A 2527-keV Ge-det. peak that was an electronic artifact. A ~2528-keV Te-det. peak that was a 2σ Statisticalflucuation. NP B35 (Proc. Supp.), 366 (1994).
13 An Ideal Experiment Maximize Rate/Minimize Background m ββ b E Mt live 1 4 Large Mass (~ 1 ton) Good source radiopurity Demonstrated technology Natural isotope Small volume, source = detector Good energy resolution Ease of operation Large Q value, fast ββ(0ν) Slow ββ(2ν) rate Identify daughter Event reconstruction Nuclear theory
14 An Ideal ββ Program Several experiments Several isotopes Better interpretation of neutrino mass Possible identification of underlying mechanism > kg Precision measurement at quasi-degenerate scale Scalable to 1000 kg Discovery sensitivity at inverted hierarchy scale
15 ββ(2ν) tail Classes of Background for ββ(0ν) Need good energy resolution. Natural U, Th in source and shielding Pure materials, segmentation, pulse shape. Cosmic ray activation Store and prepare materials underground.
16 ββ(2ν) as a Background. 30 dn/d(k e /Q) x K e /Q 1.10 Need good energy resolution K e /Q
17 The Problem: Natural Activity τ(u, Th) ~ years Goal: τ(ββ(0ν)) ~ years Source, Detector, Shielding must all be very free of radioactivity.
18 Cosmic Ray Induced Activity Material dependent. Lots of experience with Ge. Need for depth to avoid activation. Need for storage to allow activation to decay.
19 A Great Number of Proposed Experiments COBRA Te kg CdTe semiconductors DCBA Nd kg Nd layers between tracking chambers NEMO Mo-100, Various 10 kg of ββ isotopes (7 kg of Mo) CAMEO Cd t CdWO 4 crystals CANDLES Ca-48 Several tons CaF 2 crystals in liquid scint. CUORE Te kg TeO 2 bolometers EXO Xe ton Xe TPC (gas or liquid) GEM Ge-76 1 ton Ge diodes in liquid nitrogen GENIUS Ge-76 1 ton Ge diodes in liquid nitrogen GSO Gd t Gd 2 SiO 5 :Ce crystal scint. in liquid scint. Majorana Ge kg Ge diodes MOON Mo-100 Mo sheets between plastic scint., or liq. scint. Xe Xe t of Xe in liq. Scint. XMASS Xe t of liquid Xe
20 Major US Activities US contribution Status CUORE Significant Operating prototype EXO Mostly US Building prototype Majorana Mostly US Proposal MOON Significant Building prototype
21 Summary of Proposals Kilomoles Background Counts/year CUORE 1.4 ~60 EXO 4.2 <1 Exposure (kilomole-years) Majorana 3.5 ~1 10 KDHK MOON 2.5 ~ Background (counts) These background projections depend on various assumptions and the arithmetic of myself. The kilomole estimate includes efficiency. Discovery sensitivity for a half life (10 25 y). 45 mev ~ few y.
22 The Majorana Project Duke U. North Carolina State U. TUNL Lawrence Livermore Nat. Lab. JINR, Dubna ITEP, Moscow Lawrence Berkeley Nat. Lab. Pacific Northwest Nat. Lab. U. of Washington Los Alamos Nat. Lab. U. of South Carolina Brown University Univ. of Chicago RCNP, Osaka Univ. Univ. of Tenn. Oak Ridge Nat. Lab. Queen s University
23 Majorana Overview 0.5 ton of 86% enriched 76 Ge Segmented detectors using pulse shape discrimination to improve background rejection. Prototypes are being assembled. (18 crystal array, 1 enriched segmented detector) Highly efficient Long history with Ge detectors - No proofof-principle R&D required
24 Majorana Layout
25 x Ge + fast n -> 68 Ge + X β+ 90% EC 10 % 68 m EC 68 Ga 288d 271 d 68 Ge 68 Zn 2.9 MeV 68 Ge is the dominate background. For 500-kg enriched detector, initially expect ~ Ge decays/day. τ 1\2 = 288 d The naturally occurring 40 K in the human body decays at a rate of decays/second.
26 Why Segmentation and Pulse Shape Analysis? ββ β + ββ is pointlike. β + or Compton scattered γ rays deposit energy in multiple locations. Segmentation and PSD help reduce these Backgrounds.
27 Significant Milestone Segmentation R&D We now have data to confirm our hypothesis that the PSD and segmentation cuts are orthogonal. Clover Data The 228 Ac γ will typically produce multiple energy deposits. The DEP (like ββ) will produce a single-site energy deposit. 228 Ac 208 Tl DEP
28 Bare-Crystal Option Max Planck Institute
29 Cryogenic Underground Observatory for Rare Events - CUORE Berkeley Firenze Gran Sasso Insubria (COMO) Leiden Milano Neuchatel U. of South Carolina Zaragoza Spokesperson Ettore Fiorini Milano
30 CUORE Overview 0.21 ton, 34% natural abundance 130 Te TeO 2 bolometers, 750 g crystals Doesn t require enriched material x5x5 cm 3 crystals 25 towers of 10 layers of 4 crystals Gran Sasso Laboratory CUORICINO is an approved prototype (1 tower). CUORICINO began operation in Feb. 2003
31 CUORE Detector Detector Damping Suspension Dilution Unit Thermal Shields
32 CUORICINO IS OPERATING FIRST PULSE. Data runs began In Feb Initial Results 5.46 kg-y τ 1/2 > 7.2 x y
33 Enriched Xenon Observatory - EXO U. of Alabama Caltech IBM Almaden ITEP Moscow U. of Neuchatel INFN Padova SLAC Stanford U. U. of Torino U. of Trieste WIPP Carlsbad Spokesperson Giorgio Gratta Stanford
34 EXO Overview 10 ton, ~70% enriched 136 Xe 70% effic., LXe chamber Optical identification of Ba ion. Extract ion on cold probe to optical trap. Has achieved ~2% energy resolution Measure ionization and scintillation TPC performance similar to that at Gottard. ~200-kg enr Xe prototype (no Ba ID) Isotope in hand
35 Stanford Optics Lab with Ba Trap Ba Trap 136 Xe -> 136 Ba ++ e - e - -> 136 Ba + Optically observe final state. (Moe, PRC44 (1991) 931
36 EXO lone Ion/Resolution Single Ba ion Measure ionization and scintillation
37 Conclusion Due to the minimum neutrino mass scale implied by the neutrino oscillation experiments: The next generation ββ experiments have a good possibility of reaching an exciting <m ββ > region.
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