Double Beta Decay Spectroscopy and Neutrino mass sensitivities

Hiro Ejiri*, T. Shima　

RCNP Osaka Univ. 　 *NIRS & CTU, Praha

　　 For the MOON collaboration

Sendai 　 TAUP Sep. 07 　

1.Doublr beta decay spectroscopy2. Majorana mass sensitvity

3.Double beta decays to excited states4.Nuclear matrix element

H. Ejiri, J. Phys. Soc. Japan, Invited Review, 74 (2005) 2101.H. Ejiri, Mod. Phys. Lett. A, Vol. 22, No. 18 (2007) pp. 1277-1291.

by RHC, Heavy , SUSY, and others

A2=GM AgM>

Energy spectra 4,3,2 body

LHC m / SUSY m M + kMS

different isotopes and states with different M

ALHC + RHC <m> +SUSY ~k(ML/MR)2

LHC / RHC 21 and E12 correlations

Spectroscopic detectors

ELEGANT- MOON, DCBA NEMOIII - Super NEMO

1. E12-12 identify m term 2. Detector ≠ source Select nuclide by Q, Z, Enrichment, 2 3. Small RI-BG :E(RI) < Q

separation

Major BG : 2tail inwindow. E-resolution !

Interference A0 = XL + XR XL = Light + SUSY (+Heavy )

= m M + kMS = m M [(1 + (k/ m) (Ms/M) ] Cancellation at A=76 (left fig.) or 136(right), but not at other A’ b

ecause of the different short-range/long range matrix elements.

Need measurements with different nuclides.

.

Vergados 07

Nuclear matrix elements 　 QRPA

0.1

1

10

70 80 90 100

Rodin07 RQRPA QRPA Suhonen07 UCOM Jastraw

Nuclear matrix elements M

)

Ge Se Mo Cd Te Xe A

M ~ 24 /r = 18/A1/3 within a factor 1.3

Mass sensitivities and nuclear sensitivity

<m> = SN- １ /2 (Neff)-1/2 1/2

B=[B(RI) + B(2)]

B(2)=4.2(/t1/2)(100/A), 10-7 and t1/2 1020

SN- １ /2 ＝ 13 (GM2 /0.01 A)- １ /2

Nuclear sensitivity : m

N=1 t y and Y = = 1 SN

- １ /2 =20~10 meV for M=25/R

eff = N ton year

= No signals for 90 % CL ~2.3 if B~0 ~1.6 + 1.7 (BN)1/2 BG =B/t y N ton year

M ； excited state and Nd M ＝ M/3

Mass sensitivities and nuclear sensitivity

<mn> meV= (SN)- １ /2 ( N)-1/2 1/2

SN = GM2 /0.01A/170)

M=25/R ~ 4

Small BG or N

~ 2.3 <m> = 2.3 SN

- １ /2 ( N)-1/2 Large BG or N

~ 1.7 (BN)1/2 <m> = 1.3 SN

- １ /2 ()-1/2

N-1/4 B1/4

N-1/2

N-1/4

10

100

0.1 1 10

Neutrino mass sensitivity

Se82 =1.7%,2.2%, Mo100 =1.7%, 2.2%

BCDE

Effective neutrino mass in meV

N ton year

Spectroscopic DBD BG=

130Te B =6000 　 for CUORITINO 　 B=200 for 0.01 /y kev kg of TeO2

Excited 0+ states

Isotope

State

100Mo

GRS

100Mo

EXS

150Nd

GRS

150Nd

EXS

Q (MeV) 3.034 1.903 3.368 2.113

SN1/2 meV 9.6 19.5 19.5 42

<m> meV /5 y t 44 39 78 96

reduce BG’s 2, RI.• Cancellation, but not at both.• GRS and EXS

T = G |Mm +Ms|2 MJ>1+)

Nd M/3 is assumed for deformation change.

Excited state for = 2/3 of GR by , and M= same as GR

150Nd E(2) 0.13 MeV Q MeV G

150Sm GS 0+ E(2) 0.334 MeV 3.36 　　 13.4 0.74 MeV E(2) 0.34 MeV 2.63 3 E0 1.255 MeV E(2) 0.16 MeV 2.11 1.3 E2

150Nd -- 150Sm deformation

M due to change of deformation is 1/3?

M to the excited, but same deformation is 1

RCNP/MSU3He,t t, 3HeZergers R

Simucovic 1/4 ~ 1/6 of M due to deformation change.

RCNP Osaka High E response at low and hi

gh 1+ 2- states

D. Freckers, R. Zegers, MSU/RCNP/KVI

Charge exchange reactions

H. Ejiri, PR 380 ‘2000

2-

1+

Suhonen

z=5,5z=6,6T,Tz=6,6

z=5,5

,Tz=5,4

z=4,4

S

H. Ejiri PRL 21 ’68, H. Ejiri

PR 38 ‘78

Polarized GeV-MeV photons from laser scattered off GeV ele

ctronsfor electric and magneic trasitions. 　

Photon probes

MOON detector conceptional sketch

Multi-layers, 2 for and all others active shields

Each with 1PL+2PS 1.3 m-1.3 m- 4 cm 25 kg

One unit 100 mod., :30 kg, 1 m2–4m,

Based on ELEGANT V

H. Ejiri, et al., PRL, 85, 2000, 2917.H. Ejiri et al., Czech. J. Phsy. 54, 2004, 317.

Concluding remarks

1. DBD studies of E- correlations for 2-3 isotopes and/or states are indispensable for identifying the -mass processes.

2. They can be realistic by spectroscopic DBD studies with detector≠ souces. 82Se , 100Mo 150Nd are good candidates.

3. Recent QRPA/RQRPA give M~18/A1/3. Nuclear sensitivity, the mass for N=1 t y Y=1, is 20 meV for 76Ge and 10 meV for 82Se, 10

0Mo, 130Te, 136Xe.

5. Then QD ~100 meV and IH~30 meV masses are studied by N~0.1 and 1 t y with 76Ge and 82Se, 100Mo, 130Te, 136Xe .

6. Spectroscopic experiments (MOON, SuperNEMO) can access the IH masses with realistic ~ 2.2 % and ~20 mBq/t .

7. Charge exchange nuclear reactions and photo nuclear reactions are used to check the M calculations.

H. Ejiri, J. Phys. Soc. Japan, Invited Review, 74 (2005) 2101.

H. Ejiri, Mod. Phys. Lett. A, Vol. 22, No. 18 (2007) pp. 1277-1291.

MOON collaboration

　　 H.Ejiri*, T.Itahashi, K.Matsuoka, M.Nomachi, T. Shima,

• S. Umehara, RCNP and Physics OULNS, Osaka Univ.• P.J.Doe, R.G.H.Robertson*, D.E.Vilches, J.F.Wilkerson 、 D. I. Will.

CENPA, Univ. Washington.• S.R.Elliott, 　 V. Gehman, LANL• J.Engel. Phys.Astronomy, Univ. North Carolina. • M.Finger, M. Finger, K. Kuroda, M. Slunecka , V. Vrba.• Phys. Charles Univ. and CTU 　 Prague • K.Fushimi, H. Kawauso, K. Yasuda, GAS, Tokushima Univ. 　 Tokushima 　• M. Greenfield, ICU, Tokyo.• R. Hazama, Hiroshima Univ. 　• H. Nakamura, NIRS. • A. Para FNAL• A. Sissakian, V. Kekelidze, V. Voronon, G. Shirkov A. Titov, JINR • V. Vatulin, P. 　 Kavitov, VNIIEF• S. Yoshida, Tohoku Univ. Sendai

• * Contact persons.

Thank you for your attention

• .

3 GeV-p

Neutrino Weak probes

SNS 　　 1 6 1015 7 1014

　　　 J － PARC 　 3 1.2 1015 3 1014

p + Hg n +, + + +　　　　+ e+ + e + anti-

C.Volpe