Searches on neutrino physics with cryogenic detectors

Ettore Fiorini, Columbia, May 16, 2008

The birth of the neutrino

=> Named Neutrino by Enrico Fermi first properties of weakinteractrions

e

n p

GF ( )Fermi constant

The cryogenic or thermal detectors

First ideas

1884 => Langley => resistive bolometers for infrrared from SUN

1905 => Curie et Laborde => calorimetric measurement of radioactivity

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

1935 => Simon => sensitivity enhanced by lowering the temperature

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

=> McCammon et al (NASA-Wisconsin) Low temperature detectors for astrophysics and neutrino mass measurements1984 => Fiorini and Niinikoski Low temperature detectors for rare events

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

Absorber + various types of thermometer:

=> thermistor

=> transition edge sensor (TES)

=> superconducting tunnel junctions (STJ)

=> magnetic sensor

Other thermal detectors:

STJ’s => Grains superconducting grains kept in metastable state when

heated by an incoming particle they become “normal” with a consequente change of magnetic field , detectable by squid

=> liquid 3He or 4He

Energy resolution of a TeO2 crystal of 5x5x5 cm3

(~ 760 g )

0.8 keV FWHM @ 46 keV

1.4 keV FWHM @ 0.351 MeV

2.1 keV FWHM @ 0.911 MeV

2.6 keV FWHM @ 2.615 MeV

3.2 keV FWHM @ 5.407 MeV

(the best a spectrometer so far

Energy [keV]

Cou

nts

210Po line

Orpheus 0.45 kg of granules 70 m.w.e for Dark Matter detection BernConsidered also for double beta decay (A.Morales)

Q inner

Q outer

A

B

D

C

Rbias

I bias

SQUID array Phonon D

Rfeedback

Vqbias

Hybrid detectors (so far only for Dark Matter ) => heat + ionization or heat + scintillation

The scintillating bolometer Proved for CaF2 and CdWO4 being studied for TeO2

Tiny effect ->

Measurement (or limit ) on neutrino mass by single beta decay

For Neutrino Physics

Katrin

3H => 3He + e- + e

m < 2.2 eV => KATRIN < 2.2 eV

With thermal detectors187Re => 187Os + e- +-e

Manu (Genova) with metallic Rhenium Mibeta (Milano) con AgReO4 => MARE

A new fact in Nuclear Physics => Beta Environmenthal Fine Structure (BEFS) 187 Re => 187 Os + e- + ˉe E = 2.5 keV

Metallic Rhenium

AgReO4

Determination of the P/S ratio

e- + 163 Ho => 163 Os + e also for the study of neutrino mass

113 Cd => 113 I + e- + ˉ e 1/2 = (9+1) x 1015 y

e- + 123 Te => 123 Sb + e 1/2 > 1015 y

e- + 7 Be => 7Li + e => for solar neutrino

e- + 71Ga => 71 Ge + e => for solar neutrino

Discovery for the first time of 209 Bi => 204 Tl +

Other applications in Neutrino Physics

Double beta decay

Dirac Majorana =>1937

RIGHT

LEFT:

:

1. (A,Z) => (A,Z+2) + 2 e- + 2 e¯

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

Experimental approach

Direct experiments

Source detector Source = detector

(calorimetric)

Geochemical experiments82Se = > 82Kr, 96Zr = > 96Mo, 128Te = > 128Xe (non confirmed), 130Te

= > 130TeRadiochemical experiments

238U = > 238Pu (non confirmed)

e-

e-

Nucleus Experiment % Q Enr Technique 0 y <m)

48Ca Elegant IV 0.19 4271 scintillator >1.4x1022 7-45

76Ge Heidelberg-Moscow

7.8 2039 87 ionization >1.9x1025 .12 - 1

76Ge IGEX 7.8 2039 87 Ionization >1.6x1025 .14 – 1.2

76Ge Klapdor et al

7.8 2039 87 ionization 1.2x1025 .44

82Se NEMO 3 9.2 2995 97 tracking >1.x1023 1.8-4.9

100Mo NEMO 3 9.6 3034 95-99

tracking >4.6x1023 .7-2.8

116Cd Solotvina 7.5 3034 83 scintillator >1.7x1023 1.7 - ?

128Te Bernatovitz 34 2529 geochem >7.7 1024

.1-4

130Te Cuoricino 33.8 2529 bolometric >3.1x1024 .16-.84

136Xe DAMA 8.9 2476 69 scintillator >1.2x1024 1.1 -2.9

150Nd Irvine 5.6 3367 91 tracking >1.2x1021 3 - ?

Present situation Present situation

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

CUORE

NEMO

MAJORANA

GERDA

EXO

CUORICINO

22PP1/21/2

44DD3/23/2

22SS1/21/2

493 nm493 nm650 nm650 nm

metastable metastable 47s47s

SNO++

CUORE

Increase of the bolometer mass

CUORICINOCUORICINO

Operations carried out In a clean room

Operations carried out In a clean room

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

Search for the 2|o in 130Te (Q=2529 keV) and other rare events

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 => ~ 4 months

Background .18±.01 c /kev/ kg/ a

T 1/2 0 (130Te) > 3.1 x 1024 y <m> .16 -.84 eV

Klapdor 0.1 – 0.9

Without indetermination on E 11.83 kg 130Te x year => ½ lower than 3 x 1024 years at 90% c.l. 15.53 kg 130Te x year => ½ lower than 3.1 x 1024 years at 90% c.l.With indetermination on DE 11.83 kg 130Te x year => ½ lower than 2.9 x 1024 years at 90% c.l. 15.53 kg 130Te x year => ½ lower than 3.1 x 1024 years at 90% c.l.

m < 200-680 meV (V.A Rodin et al ( after the Erratum) and O.Civitarese and J.Suhonen ) Klapdor et al 200-1000 meV

Cosmological disfavoured region (WMAP)

Direct hierarchym2

12=

m2sol

Inverse hierarchym2

12= m2atm

“quasi” degeneracym1 m2 m3

With the same matrix elements the Cuoricino limit is 0.53 eV

Present Cuoricino region

Possible evidence (best value 0.39 eV)

Feruglio F. , Strumia A. , Vissani F. hep-ph/0201291

Arnaboldi et al., submitted to PRL, hep-ex/0501034 (2005).

CUORICINOPresently running , but its destiny connected with radioactivity measurements and

CUORE0

Data up to September 2007 => 11.83 to 15.53kg 130Te x year

New analysis taking into account the error on the transition energy

2 national laboratories and 7 Universities

2 universities in Europe

2 national laboratories and 5 Universities in USA

SICCAS and SINAP in Cina Plan approved by DOE

CUORICINO and CUORE

The Hut

• Design completed of the structure to house CUORE

• Construction began end of 2007

• In 2008 funds available for the Hut

• To be completed end of 2008

• External shield and polyetylene ready end of 2008

The cryostat

• CUORE cryostat design completed

• Shield by > 30 cm Pb everywhere

• External shield and polyetylene ready end of 2008

• Only radiofree materials inside

• Cryogen-free => pulse tube . Now tested in Milan

Carlo Bucci CUORE Meeting, LNGS, 4-6 February 2008

EvolutionEvolution

Step 8: Steel Work Completion31 March 2008Step 8: Steel Work Completion31 March 2008

• 12 source wires shown by white dots

• In the simulation, the sources are wires inside a teflon coating, inside a copper guide tube (’s do not escape)

• Previous study showed external sources should have twice the strength of the internal sources

• Need to run additional simulations with external sources outside the HEX cryostat

Routine calibration with radioactive sourcesRoutine calibration with radioactive sources

Plasma UHVPlasma UHV

Present small plasma apparatus

The crystalsThe crystals

A toast by Fred Reines at Neutrino 1972

Here’s to Wolfang Pauli

who made a funny joke,

Here’s to great Enrico

who then of weakness spoke,

Here’s to all those present

to celebrate the fruits

of the patient workers

who followed these astutes

Here’s to the proposition

that we will meet again

and here’s to the found hope

the Sun will shine since then.