Strategies for Next Generation Neutrinoless Double-Beta Decay Experiments

Frank AvignoneUniversity of South Carolina

Neutrino-2004College de France, ParisJune 2004

General Theme

I will not discuss the details of individual experiments.

I will discuss the important parameters and how they impact the experimental techniques.

The Parameters of interest are: , ,G0ν M0ν

b ≡

δE ≡

! ≡ detection efficiency, Mass, Isotopic abundance, background rate, and energy resolution.

Parameters of Sensitivity

€

T1/20ν

T 0ν1/2 !

ln2Nt!

γ√

bMt δE

T 0ν1/2 !

ln2(A0/W ) × 103(Mat!)γ√

bMt δE

T0ν1/2 ∝

a!

W

√Mt

b δE

a ≡ isotopic abundance

b ≡ background rate in c/(keV · kg · y)

M ≡ source mass

δE ∝ energy resolution

! ≡ detection efficiency

W ≡ molecular weight

Detection with a 4 CL

€

σ

C

€

C −B = 4 C

B

€

δE

a ≡ isotopic abundance

b ≡ background rate in c/(keV · kg · y)

M ≡ source mass

δE ∝ energy resolution

! ≡ detection efficiency

W ≡ molecular weight

T 0ν1/2 ! 4.74 × 10

25a!

W

√Mt

b δEy

Neutrinoless Double-Beta Decay Experimental Figure of Merit

f ≡ηa"

W

√M

bδE

η ≡ G0ν |M0ν |2 × 1013 = FN × 1013

η ≡ 〈η〉nuclear models

Available Experimental Techniques

Cryogenic Bolometry

Ionization Detectors

Scintillation Detectors

Time Projection Chambers

Tracking Chambers

Available Enriched Isotopes 48Ca - AVLIS† (USA)

76Ge - Centrifuge (Russia)

82Se - Centrifuge (Russia)

100Mo - Centrifuge (Russia) & AVLIS† (USA)

116Cd - Centrifuge (Russia) & AVLIS† (USA)

130Te - Centrifuge (Russia)

136Xe - Centrifuge (Russia)

150Nd - AVLIS† (USA) † Technology available at LLNL. No known production program.

Average TheoreticalNuclear Structure Factors

Parent Isotope

!

FN " G0#M

0#2

y$1

48Ca

!

(5.4"1.4+3.0) #10

"14

76Ge

!

(7.3± 0.6) "10#14

82Se

!

(1.7"0.3+0.4) #10

"13

100Mo

!

(1.0 ± 0.3) "10#12

116Cd

!

(1.3"0.3+0.7) #10

"13

130Te

!

(4.2 ± 0.5) "10#13

136Xe

!

(2.8 ± 0.4) "10#14

150Nd

!

(5.7"0.7+1.0) #10

"12

Table of Values of

η ≡ 〈G0ν |M0ν |2〉 × 1013

Isotope

!

" 48Ca 0.5476Ge 0.7382Se 1.70

100Mo 10.0116Cd 1.30130Te 4.20136Xe 0.28150Nd 57.0

€

η

Cryogenic Detector

CUORE/CUORICINO (Gran Sasso)

760 kg of (nat. abundance = 33.8%)

1000 bolometers at ~ 8 mK

25 Towers of 40 bolometers per tower

CUORICINO ~ 1 tower, operated 03/04

€

TeO2

€

T1/20ν ≥ 7.5x1023 y

!"#"$#%&'()#*" "+","-#.&/ ,%01+"

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!9),.2.0)

!9),.2.0)&!"#$%6&@A&B,CA&2!>)3$-)

!!!!

!DEF'2-

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$2/+*',.+3'-4).,3+*3'-5-6.*-)2*

728.9'62-):)2*)*;'-1-:./

CUORICINO

Ionization Detectors

COBRA - CdTe

GEM - (Ge Crystals in LN)

GENIUS - (Ge Crystals in LN)

Majorana - (Ge Crystals in Cryostat)

MPI - (Ge Crystals in LN)

€

76Ge

€

76Ge

€

76Ge

€

76Ge

COBRA

10 kg of CdTe (CdZnTe) Detectors

Measure 7(9) double-beta isotopes at once

Systematic studies of Cd and Te isotopes

Rare beta decays of 113Cd and 123Te

Dark matter search

Slide adapted from presentation of K. Zuberat DESY Zeuthen, 19-21 June 2001

NaI

Veto system

Pb

Cu

Fig. 1. Schematic layout of the proposed COBRA experiment. An array of CdTedetectors is installed within two NaI detectors, serving as active veto and part ofcoincidence measurements. This will be installed inside an OFHC copper shield,surrounded by low level lead. As a veto the complete setup will be surrounded by amuon veto consisting of high efficiency plastic scintillators.

11

CdTe - Array

Slide adapted from presentation of K. Zuberat DESY Zeuthen, 19-21 June 2001

COBRA

1 ccm crystals

Option:

Pixel Detectors

Tracking

Majorana Proposal

500 kg of Ge (86% 76Ge)

Conventional Cryostat Technology

Could use GENIUS direct immersion in LN if feasible; cooperation with MPI

Digital Electronics

Pulse-Shape Discrimination

Majorana

Majorana

MPI 76Ge Proposal for Gran Sasso

Bare Ge detectors in pure LN/LAr

Phase 1: ~ 20 kg, HM/IGEX; 86% 76Ge

Phase 2: Add 20 kg new enriched detectors

Physics Reach

Phase 1: refute claim at 99.6% or confirm at

Phase 2: 10% measurement if KKDK correct. Push limit to 2×1026 years if not.

Start construction early 2005

Begin data acquisition 2006

€

5σ

Ge

water

insulation

LN/LAr

cleanroom

lock

lead

MPI 76Ge Proposal

Scintillation Detectors

CAMEO - 116Cd (CdWO4 crystals in liq. scint.)

CANDLES - 48Cd (CaF2 crystals in liq. scint.)

CARVEL - 48Cd (CaWO4 scintillators)

GSO - 160Gd (Gd2SiO4 crystals in liq. scint.)

Xe - 136Xe (Xe dissolved in liq. scint.)

1

10

102

103

104

1000 2000 3000 4000 5000

210Bi, Q

! = 1.16 MeV

214Pb, Q

! = 1.02 MeV

211Pb, Q

! = 1.37 MeV

234mPa, Q

! = 2.27 MeV

214Bi, Q

! = 3.27 MeV

2! of 48

Ca

Energy (keV)

Co

un

ts/1

0 k

eV

210Pb,

! = 64 keVQ

Energy, keV

Counts

/10 k

eV

0

2000

4000

6000

8000

50 100 150

0

100

200

300

400

1000 2000 3000 4000 5000

E219

Rn, ! = 6.82 MeV

!/" = 0.27

E214

Po, ! = 7.69 MeV

!/" = 0.27

Q", 214

Bi, " = 3.27 MeV

Energy in # scale (keV)

Co

un

ts/1

0 k

eV

T1/2

= 120+30

-50 µs

Time interval (µs)

Co

un

ts/1

0 µ

s

0

50

100

150

200

250

100 200 300 400 500

Carvel

tr 50

o

.= 45o

r-

a40

35

30

.,<

20

154000 5000

Energy (keV)

Carvel

Time Projection, Tracking , & Drift Chambers

DCBA - 150Nd (Nd foils in a drift chamber)

MOON - 100Mo (Mo foils in plastic scint. - tracking chamber)

NEMO/Super NEMO - 82Se (Se foils in a magnetic tracking chamber)

EXO - 136Xe (Gas or liquid Xe TPC with +Ba identification)

DCBA

DCBA-T (Test apparatus for technical development)

DCBA-I (4xDCBA-T - Standard Module (SM) with natural Nd source)

DCBA-II(1) (100-SM with natural Nd - 7.7 mol 150Nd)

DCBA-II(2) (100-SM with 124 mol 150Nd enriched source)

Sensitivity to effective neutrino mass ~0.05eV

Drift Chamber Beta-ray Analyzer

Slide adapted from presentation of N. Ishihara at NDM03 Nara, 9-14 June 2003

Slide from presentation of N. Ishihara at APPI 2004 Iwate, 16-20 February 2004

DCBA

!""#$$$%&'($)*+$,--. /($#0121343 5

678β)

β,

8

9 678

β,

β)

:

9

β)

678

β,

8

:

B

9

8:

ee mmpT

rBp

!"#

#

,;),, (-?@0$

p =A&6;?

Molybdenum Observatory Of Neutrinos (MOON)

Molybdenum foils between plastic scintillators for energy readout optical fibers for position readout

MOON-I: 1 kg, 3 y, T1/2~6x1025 y (mee~0.1 eV)

MOON-II: 250 kg, 3 y, T1/2~8x1026 y (mee~0.03 eV)

MOON III: 750 kg, 7 y, T1/2~3x1027 y (mee~0.02 eV)

Tracking with angular resolution

Size ; Plastic Scintillator ~ 50cm X 50cm

100Mo foil ~ 30cm X 30cm

100Mo

Plastic Scintillator

SciFi (X axis)

SciFi (Y axis)

Plastic Scintillator

6mm

0.4mm

0.8mm

Light Guide

NaI active shield

4 ~ 10 layers

MOON

PlasticScintillator

PlasticScintillator

50cm

100Mo

2”PMT

MA-PMT

SciFi flax (X axis)

SciFi flax(Y axis)

SciFi(X axis)

SciFi(Y axis)

50cm

50cm Light guide

MOON

Beginning of data taking: February 2003 NEMO

The Super-NEMO Double-Beta Decay Expression of Interest

At least 10 times the capacity of NEMO-3

~ 100 kg of enriched isotopes

Sensitivity

€

mν ~ 30 meV

€

82Se, 100 Mo, 116Cd, 130Te, 136Xe

Super-NEMO Proposed Schedule

Phase 1. (2004 - 2006) Feasibility Studies

Phase 2. (mid 2006 - 2007) Engineering, Design, and Acceptance

Phase 3. (2008 - end 2010) Construction

Phase 4. (2011- ) Operation

Enriched Xenon Observatory

136Xe - 40 m3 at 10 Atm. (2000 kg)

80% 136Xe (Xe is a good scintillator.)

Energy resolution ~2% at 2.5 MeV

Possible Liquid Version

R&D on tagging +Ba daughter ion

200 kg Prototype (no tagging) was approved and is funded. It will be located in the DOE WIPP site in Carlsbad, New Mexico.

March 14-16, 2002 Sendai Neutrino Conference 21

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EXO

Sample Figures of Merit

500 kg of Ge enriched to 86% 76Ge

760 kg of TeO2 nat. ab. 33.8% 130Te

122 kg of TeO2 enriched to 85% 130Te

f =(0.73)(0.86)(0.8)

76

√500

(0.005)(4)! 1.05

! = 0.8 b = 0.005

! = 0.84 b ! 0.01 f = 0.89

f = 0.90! = 0.84 b ! 0.01

Large Tracking Detector(Super NEMO?)

M = 100 kg a = 0.9 ! = 0.3 b = 0.003 δE = 125 keV

f =ηa"

W

√M

b δE=

η

W(4.4)

η

W=

1.7

82= 0.002 f ! 0.09

€

82Se:

η

W=

57

150= 0.38 f ! 1.7

€

150Nd:

Target Half-Lives for

€

mν = 0.04 eV

Isotope

!

T1/ 20"

48Ca 3.0!1027

76Ge 2.3!1027

82Se 9.4!1026

100Mo 1.6!1026

116Cd 1.3!1027

130Te 3.9!1026

136Xe 5.8!1027

150Nd 2.9!1025

ConclusionsLarge value of

High Efficiency

High Isotopic Abundance

Large Source Mass

Good Energy Resolution

Low Background

Cost Feasibility

G0ν |M0ν |2

€

η (linear)

(linear) !

√M

(linear) a

√δE

√b

$

f ≡ηa"

W

√M

b δE