宇宙背景ニュートリノ崩壊探索
ロケット実験設計と検出器開発
武内勇司 (筑波大)Dec. 7, 2013
ニュートリノフロンティア研究会
＠クロス・ウェーブ府中1

Collaboration Members• As of Dec. 2013
Japan GroupShin-Hong Kim, Yuji Takeuchi, Kenji Kiuchi, Kazuki Nagata,Kota Kasahara, Tatsuya Ichimura, Takuya Okudaira, Masahiro Kanamaru,
Kouya Moriuchi, Ren Senzaki (University of Tsukuba),
Hirokazu Ikeda, Shuji Matsuura, Takehiko Wada (JAXA/ISAS),
Hirokazu Ishino, Atsuko Kibayashi, Yasuki Yuasa(Okayama University),
Takuo Yoshida, Shota Komura, Ryuta Hirose(Fukui University),
Satoshi Mima (RIKEN),
Yukihiro Kato (Kinki University) ,Masashi Hazumi, Yasuo Arai (KEK)US Group
Erik Ramberg, Mark Kozlovsky, Paul Rubinov, Dmitri Sergatskov,
Jonghee Yoo (Fermilab)
Korea Group
Soo-Bong Kim (Seoul National University)2Cosmic neutrino background (C𝜈B)
CMB

𝑛𝛾 = 411/cm3
𝑇𝛾 = 2.73 K

3 𝑇𝜈
𝑛𝜈 = 𝑛𝜈 =4 𝑇𝛾

3CB
𝑛𝛾
2

3= 56 cm𝑇𝜈 =4111
3

𝑇𝛾 = 1.95K

3

Motivation• Search for 𝜈3 → 𝜈1,2 + 𝛾 in cosmic neutrino background (C𝜈B)– Direct detection of C𝜈B– Direct detection of neutrino magnetic dipole moment
2– Direct measurement of neutrino mass: 𝑚3 = 𝑚32 − 𝑚1,22𝐸𝛾• Aiming at sensitivity of detecting 𝛾 from 𝜈 decay for 𝜏 𝜈3 =Ο 1017 yr– SM expectation 𝜏 = Ο(1043 yr)– Current experimental lower limit 𝜏 > Ο(1012 yr)– L-R symmetric model (for Dirac neutrino) predicts down to 𝜏 = Ο(1017 yr)
for 𝑊𝐿 -𝑊𝑅 mixing angle 𝜁 < 0.024

Neutrino Magnetic Dipole Moment
Neutrino magnetic moment term

𝜈𝑗𝐿 𝑖𝜎 𝜇𝜈 𝑞𝜈 𝜈𝑖𝑅

SM: SU(2)Lｘ U(1)Y𝜈𝑗𝐿γ𝑊𝐿𝜈𝑖𝐿ℓ𝐿 = 𝑒𝐿 , 𝜇𝐿 , 𝜏𝐿
𝑚 𝜈𝑖
𝜈𝑖𝑅

Suppressed by 𝑚𝜈 , GIM−𝟏
𝚪~ 𝟏𝟎𝟒𝟑 𝒚𝒓

𝜈𝑗𝐿γ

𝜈𝑖𝑅
LRS: SU(2)LｘSU(2)RｘU(1)B-L
PRL 38,(1977)1252, PRD 17(1978)1395

𝜈𝑗𝐿γ

𝑊1ℓ𝐿𝑚𝜏ℓ𝑅
𝜈𝑖𝑅1026
enhancement toSM
𝟏𝟕

𝚪~ 𝟏𝟎𝒚𝒓−𝟏

Suppressed only by 𝜁~0.02
𝑊1 ≃ 𝑊𝐿 − 𝜁𝑊𝑅cos𝜁 −sin𝜁 𝑊𝐿
𝑊1=𝑊2sin𝜁 cos𝜁 𝑊𝑅5

Photon Energy in Neutrino Decay
ν3 → 𝜈1,2 + 𝛾•

From neutrino oscillation

𝛾2𝑚32 − 𝑚1,2𝐸𝛾 =2𝑚3

𝜈32– Δ𝑚23= |𝑚32 − 𝑚22 | = 2.4 × 10−3 𝑒𝑉 22– Δ𝑚12= 7.65 × 10−5 𝑒𝑉 2

𝜈2From CMB fit (Plank+WP+highL+BAO)– ∑𝑚𝑖 < 0.23 eV

 50meV<𝑚3 <87meV, 𝑬𝜸 =14~24meV
𝝀𝜸 =51~89m
m3=50meVE =24.8meV

m2=8.7meV
m1=1meV𝐸𝛾 distribution in ν3 → 𝜈2 + 𝛾
dN/dE(A.U.)•𝐸𝛾

𝑚3 = 50 meVRed Shift effectSharp Edge with
1.9K smearingE =24meVE =4.4meV

25meV

𝐸𝛾 [meV]6

Backgrounds to C𝜈B decay
Zodiacal Emission AKARIGalaxy evolution model

Galactic dust emissionIntegrated flux from galaxy counts

CMBdN/dE(A.U.)

COBE

Zodiacal Light

Expected 𝑬𝜸 spectrum

𝑚3 = 50meV, 𝜏(𝜈3 ) = 1.5 × 1017 yr
CIB (fit from COBE data)
Sharp edge with 1.9K smearing and energy
resolution of a detector(0%-5%)CB decay
Red shift effect

𝐸𝛾 = 25meV

𝐸𝛾 = 25meV• ニュートリノ崩壊光(𝑚3 = 50meV, 𝜏(𝜈3 ) = 1.5 × 1017 yrを仮定)の~3x104倍の宇宙赤外線背景放射(CIB)• 更に黄道光がCIB観測データ(COBE)の約20倍
7Neutrino lifetime lower limit from AKARI data
Published in Jan. 2012AKARI CIB data after subtracting foregrounds
and distant galaxies
Best fit 𝐸𝛾 spectrum
from CB decay

𝜈3 lifetime lower limit as a function of 𝑚3x1012 yr

𝑚3 = 50 meV

Fit CIB data to 𝐸𝛾 spectrum expectedfrom 𝜈 decay assuming all contribution toCIB is only from 𝜈 decay

𝑚3 = 50 meV~ 150 meV
8Detector requirements• Requirements for detector– Continuous spectrum of photon energy around 𝐸𝛾 ~25 meV(𝜆 = 50𝜇m,far infrared photon)– Energy measurement for single photon with better than 2% resolution
for 𝐸𝛾 = 25meV to identify the edge spectrum– Rocket and satellite experiment with this detector• Superconducting Tunneling Junction (STJ) detectors in development– Array of 50 Nb/Al-STJ pixels with diffraction grating covering 𝜆 = 40 − 80𝜇m

• For rocket experiment aimed at launching in 2016 in earliest,
aiming at improvement of lower limit for 𝝉(𝝂𝟑 ) by 2 order– STJ using Hafnium: Hf-STJ for satellite experiment (after 2020)• Δ = 20𝜇eV : Superconducting gap energy for Hafnium• 𝑁q.p. = 25meV 1.7Δ = 735 for 25meV photon: Δ𝐸 𝐸 < 2% if Fano-factor isless than 0.39STJ(超伝導トンネル接合）検出器• Superconducting Tunnel Junction• 超伝導体 / 絶縁体 / 超伝導体のジョセフソン接合素子

2Δ

上下の超伝導電極間に電位差を与える
放射線(光)によって励起された準粒子がトンネル電流として観測

10

STJのエネルギー分解能
発生する準粒子の個数のゆらぎがエネルギー分解能の限界を決める

超伝導ギャップエネルギーが小さいものが有利
Δ: バンドギャップエネルギー
F: fano factor
E: 放射線のエネルギー

STJのエネルギー分解能

𝜎𝐸 =1.7Δ 𝐹𝐸

Hfを用いた場合の発生準粒子数
N=25meV/1.7Δ=735個Nbの場合の発生準粒子数
N=25meV/1.7Δ=9.5個

Energy resolution はないがphotoncounting は可能

SiΔE/E < √ F/√N= √ F/√735=3.7 √ F % ＠25meV
Fano factor <0.3なら分解能2％を達成可能

NbAlHf9.231.200.165

Δ[meV] 1100 1.550

0.172

0.020

Hc[G]105

Tc[K]

1980

1311Tc :相転移温度
超伝導膜に用いた金属のTc（相転移温度）の1/10程度で安定動作
Hc :臨界磁場11

STJ検出器の性能評価法• STJの電流電圧(I-V)特性を測定

 STJの超伝導転移，ジョセフソン接合の有無，リーク電流，エネルギーギャップなど素子の性能がわかる

ジョセフソン電流は磁場を印加して抑制

12

STJバックトンネリング増幅効果• トンネルバリアの近傍の準粒子は，次々とトンネル効果を引き起こし電荷を増幅する– トンネルバリアの近傍の準粒子の存在確率を上げるためトラップ層を置く– Nb/Al-STJ Nb(200nm)/Al(10nm)/AlOx/Al(10nm)/Nb(100nm)• 近接効果によりAlの超伝導転移温度はNbの転移温度に近づく• 増幅効果 2～200倍

放射線(光子）Nb

AlAlNb13

FIR photon spectroscopy with diffraction grating + Nb/Al-STJ array

Diffraction grating covering 𝜆 = 40 − 80𝜇m (16-31meV)Array of Nb/Al-STJ pixels: 50()x8() We use each Nb/Al-STJ cell as a single-photon counting detector with extremely good

S/N for FIR photon of 𝐸𝛾 = 16~31meV
 Δ = 1.5 meV for Nb: 𝑁q.p. = 60~120 if consider factor 10 by back-tunneling Expected average rate of photon detection is ~350Hz for a single pixelNeed to develop ultra-low temperature (<2K) preamplifier In collaboration with Fermilab Milli-Kelvin Facility group (Japan-US collaboration:Search for Neutrino Decay)
 SOI-STJ in development with KEK
Nb/Al-STJ array

Assuming 1𝜇𝑠 for STJ response
time, requirements for STJ• Leak current <0.1nA
Need T<0.9K for detector operation
 Need to 3He sorption or ADR forthe operationΔ𝜃Δ𝜆 𝐸𝛾 = 16~31meV

14

Feasibility of FIR single photon detection• Assume typical time constant from STJ response to pulsed light is ~1μs
• Assume leak current is 0.1nA
0.1𝑛𝐴 = 6.25 × 108 𝑒 𝑠 = 6.25 × 102 𝑒 𝜇𝑠Fluctuation due to electron statistics in 1μs is
6.25 × 102 𝑒 𝜇𝑠 = 25 𝑒 𝜇𝑠
While expected signal charge for 25meV are
25meV 1.7Δ × 10𝑒 =•25meV× 10𝑒 = 98𝑒
1.7×1.5meV(Assume back tunneling gain x10)More than 3sigma away from leakage fluctuation
Requirement for amplifier• Noise<16e• Gain: 1V/fC  V=16mV

15

JAXA Rocket Experiment for Neutrino Decay Search

JAXAのロケット実験
 ロケットで高度200km~300kmまで上昇．

約5分の観測 検出器，光学系，冷凍機のR&D完了から2年程度で打ち上げ可能 (2016年~)
 𝜆 = 40 − 80𝜇m (16-31meV)の範囲で連続スペクトラムを測定(回折格子で50分割)
100μm x 100μm x 50x8 array

Focal length 1m

Cosmic Infrared Background measured by COBE and AKARI
COBE: M. G. Hauser et al. Astrophys. J. 508 (1998) 25, D. P. Finkbeiner et al. Astrophys. J. 544 (2000) 81.
AKARI: S. Matsuura et al. Astrophys. J. 737 (2011) 2.

ロケット実験観測範囲 ４0μ m ～８０μ m
Zodiacal Emission
Zodiacal Light

Galaxy evolution model

Galactic dust emission
Integrated flux from galaxy counts

AKARI

Zodiacal Emission
COBE • 𝜆𝐼𝜆 ~500nW/m2/sr
CMBCIB (COBE)• 𝜆𝐼𝜆 ~30nW/m2/s
Neutrino decayfor 𝜏 = 5 × 1012 yr• 𝜆𝐼𝜆 ~30nW/m2/s
for 𝜏 = 1.5 × 1017 yr• 𝜆𝐼𝜆 ~1pW/m2/s
at λ＝50μm

𝐸𝛾 = 25meV

17

JAXA Rocket Experiment for Neutrino Decay Search
Event Rate and expected Lifetime Limit• 前景放射強度(黄道光): 𝜆𝐼𝜆 ~500nW/m2/sr at λ＝50μm
100𝜇𝑚 2
= 1 × 10−8 sr
1𝑚dN/dE• Pixelあたりの立体角: ΔΩ =• 望遠鏡口径: S=π x 0.0752 m2
Pixelあたりの前景放射レート𝜆𝐼𝜆 ⋅ 𝑆 ⋅ ΔΩ = 0.88 × 10−16 𝑊 = 0.55 × 103 𝑒𝑉 𝑠80𝜇𝑚 − 40𝜇𝑚
Δ𝜆 𝜆 =50𝜇𝑚 = 0.016
508.8𝑒𝑉 𝑠Δ𝜆 𝜆 ⋅ 𝜆𝐼𝜆 ⋅ 𝑆 ⋅ ΔΩ 𝐸𝛾 =~350𝐻𝑧
25𝑚𝑒𝑉
Measurements for 200s x 50 pixel x 8列→ N=28M events / 50x8 pixels
Sensitivity to detecting an edge spectrum→ 𝛿(𝜆𝐼𝜆 )~ 2 𝑁 𝑁 ⋅ 𝜆𝐼𝜆 =0.19nW/m2/sr𝜏 𝜈3 > 1014 yr (95%CL)の寿命下限設定が可能

E18Summary• 宇宙背景ニュートリノ崩壊探索実験ためのロケット実験を提案– 高度200kmで約5分の遠赤外域分光測定– Nb/Al-STJ arrayと回折格子の組み合わせによる波長𝜆 = 40 − 80𝜇mの連続スペクトラム– 𝜏 𝜈3 > 1014 yr (95%CL)の寿命下限設定(現在の下限値を1~2桁改善)• R&D– Nb/Al-STJによる25meV(50μm)フォトンの1光子計数• leakage <0.1nA, 受光面積100μmx100μm/pixel, back-tunneling gain>10– そのための超低ノイズアンプ(極低温アンプnoise <16e, gain>1V/fC): SOI-STJなど– 分光素子・光学系の設計:望遠鏡口径 15cmΦ, 焦点距離1m– ロケット搭載クライオスタットの設計 (<0.9K)• LHe減圧(1.8K)＋3He sorption
– DAQ
19

Backup20

Energy/Wavelength/Frequency

𝐸𝛾 = 25 meV
𝜈 = 6 THz

𝜆 = 50𝜇𝑚
21Feasibility of VIS/NIR single photon detection• Assume typical time constant from STJ response to pulsed
light is ~1μs
• Assume leakage is 160nA
160𝑛𝐴 = 𝑒 × 1012 𝑠 = 𝑒 × 106 𝜇𝑠
Fluctuation from electron statistics in 1μs is𝑒 × 106 𝜇𝑠 = 103 𝑒 𝜇𝑠
While expected signal for 1eV are(Assume back tunneling gain x10)
1𝑒𝑉

1𝑒𝑉
1.7Δ × 10𝑒 =× 10 = 4 × 103 𝑒
1.7×1.5𝑚𝑒𝑉More than 3sigma away from leakage fluctuation

22

Nb/Al-STJによる可視光分光• 国立天文台– λ=475nｍ

23