Paleo Detector
technological development and future prospects
Tatsuhiro NAKA
Toho University/KMI, Nagoya

Workshop, Cutting Edge Technology for Understanding the Earth, 2022.1.12 @Tohoku Uniersity, SendaiCollaboration
 JAMSTECHIROSE Shigenobu
ABE Natsue
KAWAMURA Yoji

 Toho U.

Particle Physics
×Astrophysics

 ISEE, Nagoya U.
KATO Takenori
KAZAMA Shingo
ITO Yoshitaka
KOUKETSU Yui
MICHIBAYASHI Katsuyoshi

 Kanagawa U.

×HOSHINO Yasushi

Geoscience×

Material Science Pennsylvania State U.
MURASE Kota

NAKA Tatsuhiro
IDO Yuki
SHIRAISHI Takuya Kochi U.
KOZAKA Yukiko

 Kyoto U.
IGAMI Yohei

Detectors for the particle physics
Scintillator

Cherenkov detector

・high energy physics
・neutrino physics
・dark matter searchetc

・high energy physics
・neutrino physics
・proton decay searchetc.

Tracking detector

Semiconductor

・High energy physics
・Neutrino physics
・Nuclear physics
・Dark matter searchetc

・High energy physics
・Neutrino physics
・Dark matter searchetcPaleo detector

Damage track detection in mineral

https://en.wikipedia.org/wiki/Celestine_%28mineral%Track formation

Example of fission tracks by the Zircon

Chemical etchinglattice defectHigh energy deposition is needed to enough create
the lattice defect.

5Mineral as particle detector
Fission track dating

238U : abundance of 99.3 % in isotope of U

Life time of S.F. : 8.2 x 1015 y
Decay constant λ : 8.4 x 10-17 y-1

238U

Fission track density = λ × n (density of U) × T (date)

Spontaneous fission

e.g., In case of 1 ppm U contamination and 1 G year
Mean atomic
number : 140

Mean atomic
number : 90

Fission track density ~ 108 S.F. /g
Fission tack dating by observation of the tracks

Particle Physics

×Geological scienceSerious problem for the particle physics
 Symmetry breaking → asymmetry of particle and anti-particle
 Hierarchy Problem
 Neutrino mass Strong CP problem
 Baryogenesis (mechanism of generation of baryon in the early universe) Dark matter Dark energy* All is the Nobel Prize-worthy theme

Dark Matter Standard matter consist of only 5 % in the universe,
and 95 % is unknown yet.

DEDark energy (68%)

 There are various evidence of existence of darkmatter from motion of galaxy, gravitation lens, cosmic
microwave background and so on.

Dark matter(27%)
DMStandard matter (5%)
BaryonPlanck 2013 results

However, we don’t know the identity and properties of dark matter.

Standard model for the particle physics
Interaction (gage boson)atom

QuarkUp

Charm

BottomDown

StrangeTop

Electromagnetic

PhotonMass

Weak

Weak boson（β-decay、neutrino）

Leptonelectron

muon

tauon

Stronge neutrinoµ neutrino

Higgs boson

Tau neutrino

Gluon(nuclear force)＋ anti-particles
10Standard model for the particle physics
Interaction (gage boson)atom

QuarkUp

Charm

BottomElectromagnetic

PhotonMass

No candidate in the standard model
Down

StrangeTop

WeakWeak boson（β-decay、neutrino）

Leptonelectronmuon

tauon

Stronge neutrinoµ neutrino

Higgs boson

Tau neutrino

Gluon(nuclear force)＋ anti-particles
11

Dark Matter in the milky way galaxy

solar system

Center of galaxy

Astrophys. J. 295: 422-436, 1985

𝒗=Local dark matter density : 0.4 GeV/cm3𝑴(𝒓)𝑮𝒓With out dark matter :𝑐𝑜𝑛𝑠𝑡.
𝑣∝𝑟Case of w/o dark mtter

Actual data : 𝑣 ∝ 𝑐𝑜𝑛𝑠𝑡.

~ 1000000/cm2/s on the earth incase of DM mass of 10 GeV/c2

𝑖. 𝑒. , 𝑀(𝑟) ∝ 𝑟 almost visible matter is condensed
around galactic center

12

Dark matter candidate for particle physics• Weakly Interacting Massive Particle (WIMP)• Q-ball• Monopole
Paleo detector targets• Axion・・・・・

There are previous study by the mica in 1980-90.

Direct dark matter search in the earth
Particle model: Weakly Interacting Massive Particle (WIMP)

Dark Matter wind

Elastic scattering : DM + N → DM + NDM velocity : O(100) km/s
DM mass : > O(10) GeV/c2Darkmatter

検出器内の原子核

Darkmatter

Detector
Nuclear recoil signal : O(10-100) keV
Recoil range : O(10-100) nm* Neutrino is also same signal

𝑵𝒖𝒎𝒃𝒆𝒓 𝒐𝒇 𝒔𝒊𝒈𝒏𝒂𝒍 𝑵 = 𝑹 [/ 𝒌𝒈 𝒚𝒆𝒂𝒓] × 𝑴 𝒌𝒈 × 𝑻 𝒚𝒆𝒂𝒓
𝐸𝑣𝑒𝑛𝑡 𝑟𝑎𝑡𝑒 ∶ 𝑅 [/ 𝑘𝑔 𝑦𝑒𝑎𝑟] = 𝜌 𝑡𝑎𝑟𝑔𝑒𝑡 𝑛𝑢𝑐𝑙𝑒𝑖 𝑘𝑔 × 𝑓𝑙𝑢𝑥 [/ 𝑐𝑚2 𝑠𝑒𝑐] × 𝜎 [𝑐𝑚2 ] × (3.2 × 107 𝑠𝑒𝑐/𝑦𝑒𝑎𝑟)
3𝑓𝑙𝑢𝑥 =

𝜌 [𝐺𝑒𝑉 𝑐𝑚 ]× 𝑣 [𝑐𝑚 𝑠𝑒𝑐]
𝑀𝐷𝑀 [𝐺𝑒𝑉 𝑐 2 ]𝜌: local dark matter density 0.4 𝐺𝑒𝑉 𝑐𝑚3 𝑓𝑟𝑜𝑚 𝑟𝑜𝑡𝑎𝑡𝑖𝑜𝑛 𝑐𝑢𝑟𝑒𝑣𝑒 𝑜𝑓 𝑔𝑎𝑙𝑎𝑥𝑦
v: dark matter velocity (typically 300 𝑘𝑚 𝑠𝑒𝑐)

DM-nuclei cross section(unknown parameter)

DMDM

VS
Mass scale> 0.001 kg (1g)

~ 104 kgTime scale

109 years

O(1) years

Exposure（Mass × Time)> 106 kg・year•>~104 kg・year

Final sensitivity depends on the detection performance such as energy threshold, readout efficiency, background etc..

 Dark matter density is expected to be notuniform as sub-halo from the simulation.
 Solar-system is running in the dark matter
halo with such density fluctuation.
Mineral may record such information during 1 Gyear
because the revolution period has 0.2 Gyear.
Sebastian Baum et al., (2021)

Galactic archaeology !!

Previous research for WIMP search

Scanning area : 80720 μm2=8x10-4 cm2( Probably ~ 10-9 g )Null signal for unexposed
sample (DM search)

Exposure : 0.5 Gyear~ 0.5 g・year exposure

Nuclear recoil due to neutron

Readout technique : AFM

First upper limit of WIMP dark matter
using the mineral

Prospect of WIMP search for each mineral
Sensitivity limit of WIMP DM

Sebastian Baum et al., Phys. Lett. B 803 (2020) 135325

DM sensitivity : 100g + 1Gyear sample is consistent with current
most sensitive dark matter search with 10 t scale
Requirement : Low U contamination (< 0.01 ppb)
Low neutron level+How much the track formation efficiency ?
Efficient readout system

Q-ball dark matter
Non-topological soliton by scalar field theory with global U(1) symmetry
Bound quantum condition with squark, slepton in the SUSY

Afleck-Dyne mechanism (Nucl. Phys. B. B249 (1985) )Baryogensis by inflation and SUSY
→ coherent oscillation and large fluctuation for the A-D field ： Q-ballSupersymmetric Electrically Charged Soliton JCAP 1608, 053（2016）
・positive charge by gage mediated lepton decay
・EM interaction
Charged Q-ball (ZQ<137) exist and candidate dark matter as thestate of Q-ball atom or ions in the universe

Very heavy charged dark matter (MQ > 1010 GeV/c2)

From Prof. M. Kawasaki’s slide
19Serious problem for the particle physics
 Symmetry breaking → asymmetry of particle and anti-particle
 Hierarchy Problem
 Neutrino mass Strong CP problem

Q-ball related

 Baryogenesis (mechanism of generation of baryon in the early universe) Dark matter Dark energy* All is the Nobel Prize-worthy theme

Current charged Q-ball search limit
MACRO experiment [1989-2000]

PRD,62 (2000) 105013
No dark matterregionCR-39 (plastic damage detectors)
Observed area : O(10 x 10) m2

The Mica limit is converted from the monopole search by P. B. Priceand M. H. Salamon, Phys. Rev. Lett. 56, 1226 (1986).

Exposure time : O(1) year21

Past highest sensitive Q-ball search
MACRO experiment [1989-2000]

MICA [1986]

CR-39 (plastic damage detectors)

Mica (mineral detector)

Observed area : O(10 x 10) m2

Observed area : > O(0.1 x 0.1) m2

Exposure time : O(1) year

Exposure time : O(109) year

Expected signature
Q-ballMonopole

WIMPs, neutrinoO(10-100) nm* Required specific model to form
the track in mineralEasier

Challenging

Subjects from experiment side Track formation efficiency
 Handling optimization such as chemical etching Readout technology
 Older sample
 Low-background sample

Geoscience side

Our sideEnergy loss mechanism
Lindhard mechanism

Bethe-Bloch mechanism(ionization dominant )High energy particle physics

O(100) km/sec (v/c ~ 10-3)
Our target

Low-velocity region (β < 10-3) : NSP + ESP (NSP>ESP)

Nuclear collision + excitation, ionization

High-velocity region (β < 10-3) : ESP (ESP >> NSP)High density electron excitation

25

Required energy loss for track formation in the mineral
Energy per nucleon

Case of “muscovite mica”
Required energy deposition due to ionization𝑑𝐸> ~ 10 𝑀𝑒𝑉 𝑚𝑔 𝑐𝑚2𝑑𝑥(~ 30 GeV/cm in the mica)

However, it’s possible to form the track inlow-velocity region

α-ray
Phys. Rev. 156 (1966)2

Low-velocity region of around 103 is easier to form the tracks ?

Velocity βStudy by Dr. Hirose et al., at JAMSTEC

Readout scale for each microscope techniques
SEM
10000

1000000
100000

1000

10000

1001000

10100

1

100.1

10.01

0.1

0.001

0.01

0.0001

Optical MS

0.0001 0.001 0.01

0.1

110100 1000

Image data taking speed [sec/(100 um x 100 um)]

Scanning spped per 1m2 [year]

Scanning time per 1 g [year]

AFM Higher speed readout will be required Optical microscope is promising for firstcandidate trigger.
 Finally, combined analysis between optical
microscope and higher resolution microscopeshould be importantOptical readout technology for the nuclear emulsion
PTS system for nuclear emulsion scanning

Tracks in the nuclear emulsion

1.5μm

5 mm

Nuclear recoil(DM candidate)

proton recoil(neutron)

High energy interaction

Automatic readout of charged particle in the nuclear emulsion

This system will be applicable to the Paleo detector

β= 1x10-3Nuclear recoil by the WIMP

Energy loss [GeV/cm]

Energy loss [GeV/cm]

Energy loss of charged Q-ball (Preliminary)

Z_Q=20Velocity

Q-ball charge Z_Q
Dark matter expected30

HIMAC @ QST

National Institute for Quantum Science and Technology
https://www.qst.go.jp/site/qst-english/[Accelerator for heavy ion therapy]

Available Ion beam
Ion

Energy [MeV/u]Max. Intensity [/s]

He

150

1.2 x 1010

C

135,290,350,400

2.0 x 109

Ne230,400

5.5 x 108Si490

4.7 x 108Ar500

2.7 x 108Fe500

2.5 x 108

Candidate for Q-ball calibration31

Fe ion calibration at the HIMAC
Fe ion in the mica

Fe 500MeV/u in the mica
Attenuated Fe ion

energy loss [GeV/cm]

100.0

Fe 500MeV/nQ-ball expected
10.0

Attenuator
Electron Stopping Power

1.0

Nuclear Stopping Power

Attenuated Fe ion

0.1

1.E-02

1.E-01

1.E+00

1.E+01

1.E+02

1.E+03

1.E+04

Projectrd range [μm]Similar energy loss process with charged Q-ball Optical recognition ability
 Tracking threshold depending on the dE/dx
 dE/dx dependence for above factor

32

Phase contrast optical microscope image of Fe ion beam (500 MeV/u)[HF 20℃, 80 min etching ]Track band

α-recoil track due to 238U
238U→234Th + α-ray
70 keVFe ionFe ion track

Brightness of Fe ion tracks aroundstopping region (on going study)
①

②

①

②

Low-velocity region seems
higher contrast (!?)

Expected achievement for Q-ball search with the mica
+ current cutting-edge technologies

Current best limit

Target for this experiment36

Conclusion
Particle physic×Geoscience

Paleo detector using mineral→ Recorded signal in the galaxy during 1 Gyear scale

New value for galactic archeology!!
Detection target
 WIMP dark matter Neutrino
 Q-ball as the DM
 Monopole

Damage tracking in the mineral Readout technology
 Selection of suitable mineral Understanding the backgroundand detection performance•••

Lower Uranium contamination
Track formation possibility
observation with chemicaletching

On going the experimental study!!
It will be able to start to search in our group soon!

High-resolution readout
Coherent X-ray microscope imaging
 Imaging technique with reconstruction from coherent Xray diffraction pattern Tomographic imaging with 10 nm resolution is possible

Now, we started to discuss about application of the NanoTeras
with Prof. Yoshida of SRIS ( International Center for Synchrotron
Radiation Innovation Smart), Tohoku University about
application of the NanoTeras.

http://www.spring8.or.jp/ja/news_publications/press_release/2010/100420/

Nano Lett. 2010, 10, 5, 1922–1926• BL29XU@SPring-8、11.8keV