cryogenic detectors for double beta decay and dark matter searches 1 -past and present of thermal...

Cryogenic Detectors for Double Beta Decay and Dark Matter Searches

1

- Past and present of thermal detectors- Their role in searches of rare events- Hybrid techniques- Present situation of searches on direct interactions of

WIMPS and the role of thermal detectors- The impact of the discovery of neutrino oscillation The

second mystery of Ettore Majorana- Present situation on experiments of neutrinoless double

beta decay and the possible impact of thermal detectors in this field

- Conclusions

August 31,2009 Ettore Fiorini, Madison

First ideas

1880 => Langley => resistive bolometers for infrrared rays from SUN

1903 => Curie et Laborde => calorimetric measurement of radioactivity

1927 => Ellis and Wuster => heat less then expected => the neutrino

1949 => D. Andrews, R. Fowler, M. Williams => a particle detection

1983 => T.Niinikoski =>observe pulses in resistors due to cosmic rays

1984 => S.H.Moseley et LT detectors for astrophysics and n mass

=> Fiorini and Niinikoski Low temperature detectors for rare events

=> A. Drukier, L. Stodolsky, => neutrino physics and astronomy

2August 31,2009 Ettore Fiorini, Madison

The cryogenic or thermal detectors


Incident particle

absorber

crystal

Thermal sensor

Excellent resolution <1 eV ~ 2eV @ 6 keV

~10 eV ~keV @ 2 MeV

VC

Q T

J/K )( v

v 1944 C 3

m V

T

4

Equilibrium detectors


5

-

- Various types of thermometers

=> a thermistor

=> a transition edge sensor (TES)

=> an Equilibrium Absorber weakly coupled to a heat bath

superconducting tunnel junction (STJ) Cooper pair

breaking

=> a magnetic thermometer . The temperature information is

obtained from the change of a paramagnetic sensor

placed in a small magnetic field

Caveat => possibility that the heat capacity of the thermometer be comparable or larger than the absorber one:


The first mini-meeting on thermal detectors(Ringberg castle 1986)


Energy resolution of a TeO2 crystal of 5x5x5 cm3

(~ 760 g )

:

0.8 keV FWHM @ 46 keV

1.4 keV FWHM @ 0.351 MeV




(the best a spectrometer so far

210Po a line


Non equilibrium detectors

Þ STJ Superconducting tunnel junctionsÞ SSG Superheated superconducting granules . The field does not

enter more in the granule. Often SQUID pickup Suggested for In solar neutrino detection. Considered for Dark Matter Experiments

=> Superfluid 3He and 4He detectors (rotons) . Also considered for Solar neutrinos

Comparison with conventional detectors:

=> They measure the total energy delivered (example MARE)

=> Slow propagation of the vibration inside the absorber

Kapitza resistence detector => heat sink (slow rise and decay times)

ÞPossible localizazion of the event (TES)

Þ Excellent detection of nuclear recoil

Þ Possibility of hybrid techniques (heat + ionization and/or scintillation? Crucial in searches for rare events


12

Possible “thermometers”

Superheated Superconducting Granules


13

Orpheus 0.45 kg of granules 70 m.w.e for Dark Matter detection Bern

Considered also for double beta decay (A.Morales)


14

Q inner

Q outer

A

B

D

C

Rbias

I bias

SQUID array Phonon D

Rfeedback

Vqbias

Hybrid techniques

heat + ionization or heat + scintillation


15

209Bi considered the only stable isotope of Bi and the stable nucleus with higher Z

A very interesting application of thermal detectors => decay of 209

Bi

Scintillation and heat experiment in Paris by P.de Marcillac et al with a BGO of 47 g

= 3137 DE ± 1stat ± 2syst => 1,9 ± 0.2 x 1019

a


16

Present status on direct interaction of WIMPS

Indeed a challenge as also shown by many reports to this Workshop


17

Interactions of WIMPS produce rare low energy events


18

Need signals with evidence of interaction of WIMPS

- seasonal modulation => general motion of the Sun toward Cygnus - directionality- different nuclei- elimination of the dominant electromagnetic background => electron versus nucleon recoils => the quenching factor

e.g. 25% in Ge detectors, In thermal detectors could be > 1 ! => need calibration with neutron sources or radioactive sources


August 31,2009 Ettore Fiorini, Madison 19

ELEGANT, XMASSCDMS

ZEPLIN-II

XENON

MAJORANA

GEODM

EDELWEISS

CRESST, WARP, XENON, HDMS/GENIUS

DAMA/LIBRA

CUORICINO/CUORE

ZEPLIN-III, NaIAD, DRIFT

IGEX

ROSEBUD

ANAIS

• CDMS-II @ Soudan Mine

• EDELWEISS-II (cryo Ge @ Fréjus)

• CRESST-II (cryo CaWO4, ZnW04) @ Gran Sasso

• ROSEBUD (cryo Al203, CaWO4) @ Canfranc

• XENON-10, XENON-100, ZEPLIN-III, DRIFT, NaIAD

• WARP, ArDM, DEAP/CLEAN (liquid argon, neon)

• DAMA/LIBRA (NaI, Xe @ Gran Sasso)

• IGEX @ Canfranc, HDMS/GENIUS-TF (Ge) @ Gran Sasso

• CUORICINO/ CUORE (Te02) @ Gran Sasso

• COUPP (Chicago), SIMPLE, MACHe3, ORPHEUS (Bern)

• ELEGANT, LiF @Japan

• + Future experiments: SuperCDMS/GEODM, EURECA , XENON-1ton, XMASS,

…

Wimps direct detection experiments

20

Possible evidence (DAMA/LIBRA)

Je ni laue ni blame pas. je report seulement Tallerand

I do not praise, nor blame. I only report.


Close relationship => Dark Matter and double beta decayFirst searches on direct interations of WIMPS with Ge detectors for bb decayCould this relationship start again?Why not! Answer g by Ezio Previtali to Richard Geiskell who asked if CUORE could give results on Dark MatterA personal note => Dark Matter experiments search the low energy region, the neutrinoless double beta decay ones a region at higher energy !Problems => kitchen multipurpose tools”!

Massive thermal detector s => seasonal modulation ( higher QF)

Hybrid techniquesScintillation or ionization => electromagnetic background (dominant) + + heat (nuclear reecoil) => in anticoincidence

.

21

Thermal detectors to search for WIMPS



After experiment in a shallow site with Ge bolometers and NTD thermistors => Soudan Laboratory also with Si

bolometers with TES

CDMS@Soudan

CDMS II results

25

In terra infidelium (in the land of infideles)


27

•Test of first two supertowers

•Detectors 1 inch thick

(640 g/detector unit)

•Improved phonon collection scheme

•Study of interdigitized electrodes

•Much larger detectors considered (6 inch diameter,

2 inch thick):

nearly 5 kg !

SuperCDMS developments


Future plans of CDMS


29

Ge bolometers => ionization+heat

EDELWEISS II

Inter Digit detectors

E-field modified near surface

with interleaved electrodes

EDELWEISS I

Ge bolometers with ND sensors

Guard rings

Problems with surface events


EDELWEISS@Frejus

30

23 detectors installed

11 detectors with <30 keV threshold.:

93.6 kgd / 4 mo.

3 events in nuclear recoil band

Bkg reduced wrt

EDELWEISS-I, but not

sufficient to reach 10-8

pb: need ID


D 08 DATA:

2 x 400g 86 live days /. 18.3 kgd with <15 keV 50% eff. @ 10 keV

No events in (or around) nucl. recoil band

More ID detectors later (10 in 2009)

August 31,2009 31Ettore Fiorini, Madison

32

W

β+γ

α

O

Works with many absorber materials

CaWO4, PbWO4, BaF, BGO

(other tungstates and molybdates)

300g scintillating

CaWO4 crstal

Light detector W thermometer

Light reflector

W thermometer

CRESST@LNGS

scintillation + heat


33

17 x 300 g modules installed in Gran Sasso

W films: Superconducting Transition Edge temperature sensors + SQUID read-out

Absorber: CaWO4 crystal (Wimps = W recoils, neutrons = O, Ca recoils)


34

ROSENBUD@Canfranc

Scintillation + heat


35

A large European project involving EDELWEISS, CRESST,

ROSEBUD, CERN et al

>> 100 kg multitarget experiment => 10-9 pb

Possible location (no responsability on my side)

=> a new 60,000 m cavity in the Frejus tunnel


36

What about the nature of the neutrino and its mass?

The second mystery of Ettore Majorana


Strongly supported by the discovery of n oscillations


→ →

<= =>

Majorana =>1937

Neutrinoless double beta decay and Majorana neutrinos

RIGHT

LEFT

:

:


1. (A,Z) => (A,Z+2) + 2 e-

+ 2 ne¯

2. (A,Z) => (A,Z+2) + 2 e-

+ c ( …2,3 c)

3. (A,Z) => (A,Z+2) + 2 e-

(A,Z+1) (A,Z) (A,Z+2)


u e -

d

d

e -W

u

ne

ne

2n - bb decay

W

0n - bb decay

e -

e -

d

du

u

W

Wen

en

Neutrinoless bb decay


Predictions from oscillations

42

• disfavoured by -0

•disfavoured by cosm

ology

• m 2atm

< 0

• m 2atm

> 0

• next generation -0 exp

• degeneration: m1 ≈ m

2 ≈ m

3

• inverse hierarchy: m3 « m

1 ≈ m

2

• normal hierarchy: m1 ≈ m

2 » m

3

•⟨m

⟩

[eV

]

• lightest neutrino mass [eV]

• A.Strumia and F.Vissani.: hep-ph/0503246

• <mn> = f( m

low,U

ek )


43

Claim of Evidence for 0 in 76

Ge

Single-site events in detectors 2, 3, 4, 5 (56.6 kg-y).

H.V. Klapdor-Kleingrothaus, Int. J. Mod. Phys. E17, 505 (2008)

<m> ~ 0.2 to 0.3 eV

Looks good to me…not to me (E.F.)


Experiment Nucleus Detector

NEMO III 100Mo et al 10 kg of enrich. Isotopes -tracking

Cuoricino 130Te + etc. 40 kg of TeO2 bolometers (nat)

CUORE 130Te + etc. 750 kg of TeO2 bolometers (nat)

EXO 136Xe 200kg - 1 t Xe TPC

GERDA 76Ge 30 Š 40 kg Š 1t Ge diodes in LN

Majorana 76Ge 180 kg - 1t Ge diodes

MOON 100Mo nat.Mo sheets in plastic sc.

DCBA 150Nd 20 kg Nd-tracking

CAMEO 116Cd 1 t CdWO4 in liquid scintillator

COBRA 116Cd , 130Te 10 kg of CdTe semiconductors

Candles 48Ca Tons of CaF2 in liquid scintillators

GSO 116Cd 2 t Gd2SiO5:Ce scintill.in liquid sc.

Xe 136Xe 1.56 Xenon in liquid scintillator.

Xmass 136Xe 1 t of liquid Xe

MOON

GERDA

EXO

CUORICINO

2P1/2

4D3/2

2S1/2

493 nm

650 nm

metastable

47s

Experimental situation

44

CUORE

SNO++

MOON

NEMO - SuperNEMO


Double beta decay with thermal detectors

45

Searches for the 2b decay in 130

Te (Q=2529 keV and 34% i.a.)

A series of experiments carried out first by the Milano group and later by the CUORICINO and CUORE collaboration

Mibeta (Milano only) an array of 20 TeO2 bolometers of 320 g

=> total mass 6.8 kg

CUORICINO (CUORICINO Coll.) 44 crystals of 150 g and 18 of 320

(4 enriched)n => total mass 40.7 kg

CUORE (CUORE coll) 988 crystals of 750 g

=> total mass 741 kg


Searches in the LNGS

Cuoricino (Hall A)

CUORE (Hall A)

CUORE R&D (Hall C)


year

tota

l ma

ss [

kg]


Mass increase of bolometers

11 modules, 4 detector each,

crystal dimension 5x5x5 cm3

crystal mass 790 g

4 x 11 x 0.79 = 34.76 kg of TeO2

2 modules, 9 detector each,

crystal dimension 3x3x6 cm3

crystal mass 330 g

9 x 2 x 0.33 = 5.94 kg of TeO2

48

At Hall A in the Laboratori Nazionali del Gran Sasso (LNGS)

18 crystals 3x3x6 cm3 + 44 crystals 5x5x5 cm3 = 40.7 kg of TeO2

Operation started in the beginning of 2003

Background .18±.01 c /kev/ kg/ a

CUORICINO



CUORICINO

Change of the measured value of DE

2523

2524

2525

2526

2527

2528

2529

2530

2531

2532

2533

With ~ 18 kg x a 130Te e DE ~ 2527 keV

=> t1/2 < 2.94 x 1030

2527.01 ± 0.32 keV

2527.518 ± 0.013 keV

With 15.53 kg x a of 130

Te and DE = 2530.30 +/- 1.99 keV => t1/2 < 3.1 x 1030


51

Klapdor .1-.9


Cosmological disfavoured

region (WMAP)

Direct hierarchy

m2

12= m2

sol

Inverse hierarchy

m2

12= m2

atm

“quasi” degeneracy

m1 m2 m3

With the same matrix elements the

Cuoricino limit is 0.53 eV

Possible evidence (best value 0.39

eV)

52

Present Cuoricino region


The CUORE collaboration


55

The calibration system


57

The crystals


58

Growing and lapping at SICCAS

ÞOrder for 63 cristals 4 crystals by flight => OK

ÞOrder for 500 crystals INFN 26 (2 being tested) + 32+36

ÞAgreement prepared for 500 crystals DOE

ÞCrystals are arriving at a rate of 30 crystals per month

ÞIn a year all INFN crystals produced. => Validation of the DOE ones

PackagingAugust 31,2009 Ettore Fiorini, Madison

SICCAS/INFN Clean Room


disfa

vou

red

by co

smo

log

y

11-576.5 × 1026510-3

19-1002.1 × 1026510-2

<m> [meV]T1/2 [y]

[keV]b (counts/keV/kg/y)

11-576.5 × 1026510-3

19-1002.1 × 1026510-2

<m> [meV]T1/2 [y]


11-576.5 × 1026510-3

19-1002.1 × 1026510-2

<m> [meV]T1/2 [y]


11-576.5 × 1026510-3

19-1002.1 × 1026510-2

<m> [meV]T1/2 [y]


Strumia A. and Vissani F. hep-ph/0503246

In 5 years:In 5 years:


CUORE expected sensitivity


The earthquake

0.64 g =>center of L’Aquila

0.29g =>outside laboratory

0.03 g inside

Compound Isotopic abundance Transiton energy

48CaF2 .0187 % 4272keV

76Ge 7.44 " 2038.7 "

100MoPbO4 9.63 " 3034 "

116CdWO4 7.49 " 2804 "

130TeO2 34 " 2528 "

150NdF3 150NdGaO3

5.64 " 3368“

Other possible candidates for neutrinoless DBD

63

The future


64

*Maybe Cherenkov light T.Tabarelli de Fatis – Milano-Bicocca

Scintillation* + heat

(in coincidence)



First scintillating bolometer (1991)

CaF2


Already tested different scintillating crystals

(CdWO4, CaF2, CaMoO4, SrMoO4, PbMoO4, ZnSe, …).

With some of them we have obtained excellent results (for

example CdWO4, CaMoO4 and ZnSe).

CdWO4: 508g

ZnSe:337 gCaMoO4: 157g

Four and one CDWO4 with Ge light detectors



724 hours

Background CdWO4 3x3x6 (426 g) – Scatter Plot (724 hours)

180W

238U

234U

210Po

230Th

228Th

224Ra

220Ra

216Po

232Th

212Bi

212- Bi212

Po


Background CdWO4 3x3x6 (426 g) – Beta Spectrum

113Cd

(i.a.= 12.2 %)

Qβ = 318 keV

Thermal detectors operating at low temperature (10-10 mK) had a great development in the last twenty years

In many fields of physics (e.g.low energy nuclear physics, X-ray spectroscopy, material sciences , even environmental physics etc)

they have not yet sufficiently exploited

Their long rise and decay time not a problem for searches on rare events

in non accelerator physics (see however their role in accelerator like DESY)

They offer a wide choice of source or target nuclei.

The possibility of hybrid employ association with detector of ionization

and/or scintillation => formidable tool in searches for direct interaction of WIMPS

In experiments on bb decay especially in its neutrinoless channel they are

already competitive with other detector. This property will be further

enhanced by the use of scintillation and /or ionization in coincidence

Their multidisciplinary nature => exiting and exellent for learning

CONCLUSIONS


cryogenic detectors for double beta decay and dark matter searches 1 -past and present of thermal...

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