XAX Can DM and DBD detectors combined?

04/22/23 Katsushi Arisaka 1

University of California, Los Angeles

Department of Physics and Astronomy

[email protected]

Katsushi ArisakaKatsushi Arisaka

XAXXAXCan DM and DBD detectors Can DM and DBD detectors

combined?combined?

04/22/23 Katsushi Arisaka, UCLA 2

XAX paper by UCLA Group

14 m

12 m

XAX (Xenon-Argon-Xenon)


Water Tank Veto

4 m 12 m

129/131Xe12 ton(6 ton)

40Ar70 ton(50 ton)

WIMP (Spin odd)Solar Neutrino

WIMP (Spin even)Double Beta Decay WIMP (Spin even)

2 m

136Xe7 ton(4 ton)

1.2 m

Separation of Odd and Even SpinXenon


Why Multiple Targets? Systematic Study of Dark Matter Interaction

Target mass dependence of Cross section and Energy spectrum• Xenon vs. Argon

Spin dependence of Cross section • 129/131Xe (Spin odd) vs. 132/134/136Xe (Spin even)

Precise determination of Mass and Cross section

Neutrino-less Double Beta Decay > 1028 years by 136Xe

Solar Neutrino 1% measurement of the pp chain flux by 129/131Xe.

Supernova Neutrino Measurement of the total energy and temperature by coherent

elastic scattering.• Xenon vs. Argon

Katsushi Arisaka, UCLA 504/22/23

Energy Spectrums (Natural Xe)

Be7 Solar

B8 Solar

2 DBD (1022 yrs)

pp Solar

0 DBD (1027 yrs)

100 GeV WIMP (10-44 cm2)


Concept of one of XAX Detectors


2 m

Radiation- freePhoton Detector(3” QUPID, Total 3950)

OFHC (Oxygen-Free High Conductivity Copper)Vacuum Vessel

TPB + Resistive Coating (ATO)+ Acrylic Vessel

Liquid Xe (19 ton)


Concept of Double Layer XAX

2 m

2 m

-17.5 kV

-200 kV

-10

kV

-10 kV

0 V

-10 kV

Gas Xe

136Xe7 ton

Radiation-freePhoton Detectors(QUPID)

TPB +ATO+ Acrylic Vessel+ ITO Coating

TPB + ITO Acrylic Sheet + ITO Coating

Acrylic Sheet+ ITO + TPB Coating

TPB+ Acrylic Sheet+ ATO Coating

129/131Xe12 ton

Equipotential lines and Electron Trajectories


ATO (Antimony Tin Oxide) Transparent Resistive Coating (~ 1 G⁄☐)

ITO (Indium Tin Oxide)Transparent ConductiveCoating (~1 k⁄☐)

ElectronTrajectories

ITO (Indium Tin Oxide)Transparent ConductiveCoating (~1 k⁄☐)

-13.5 kV

-200 kV

-6 kV0 V

-6kV

0 V

Expected No. of Photoelectrons per keV(Abs. Length = 10 m, Scat. Length = 50 cm)


PTFE on Side Wall (Reflectivity = 98%) Photon Detectors on Side Wall

~ 1.5 pe/keV ~ 3 pe/keV

Expected No. of Photoelectrons per keV(Center of 2m Xenon Detector)


Absorption Length

Scattering Length

50 cm 1 m 2 m

PTFE on side (Reflectivity = 95%)

5 m 1.0 1.2 1.4

10 m 1.7 2.0 2.2

20 m 2.4 2.8 3.1


5 m 1.0 1.3 1.5

10 m 1.7 2.1 2.3

20 m 2.6 3.0 3.2


5 m 1.0 1.3 1.5

10 m 1.8 2.1 2.4

20 m 2.7 3.1 3.3

QUPID on side

5 m 1.6 2.1 2.5

10 m 2.4 3.0 3.5

20 m 3.2 3.8 4.3


(1) Dark Matter


Gamma Backgrounds after S2/S1 cut(1 mBq / QUPID, 2m Xenon Detector)

100 GeV WIMP (10-44 cm2)

1 TeV

10 TeV

2 DBD (1022 yrs)

pp Solar Neutrino BG (10 cm shield)

BG (0 cm shield)

Be7 Solar Neutrino

BG (5 cm shield)


Expected Background from Gammas(1 mBq / QUPID, 1 year, Multi Hit Cut, No S2/S1 cut)

10 ton

0.01 /10ton-yearafter S2/S1 cut

< 10–8 DRU

Xenon (2m)

Neutron Backgrounds after Multi-hit Cut(1 n/year/QUPID, 2m Xenon Detector)


100 GeV WIMP (10-44 cm2)

1 TeV

10 TeV

0 cm

10 cm20 cm

30 cm


Expected Background from Neutrons(1 n/year/QUPID, 10 year, Multi Hit Cut)

10 ton

0.4 n /10ton-year

< 10–8 DRU

Xenon (2m)

Expected No. of WIMP Signals and Backgrounds(10 ton-year of Liquid Xenon, Window = 3 – 15

keVee)

04/22/23 17

Self Shielding Cut (cm from wall) WIMP Mass (GeV)

No. of Background Events No. of WIMP Signals

10-48 cm2

10-44 cm2

10-45 cm2

10-46 cm2

10-47 cm2

19.2 ton 9.8 ton14.0 ton

Katsushi Arisaka, UCLA

2-Neutrino DBD (S2/S1 cut)

pp-chain Solar (S2/S1 cut)

Neutron (no cut)

Neutron(multi-hit cut)

Gamma(no cut)

Gamma(S2/S1 cut)

G2

G3

1 mBq /QUPID

G1

Summary of WIMP Detection Sensitivity:

< 10-47 cm2 at 100 GeV WIMP mass. (< 10-46 cm2 at 1 TeV) Background:

Completely free from external gamma ray backgrounds.• < 10 mBq / PMT

– QUPID is < 1 mBq (Goal is < 0.1 mBq)• 10 cm active shielding• S2/S1 cut

Neutrons background is negligible too.• < 1 neutron / year / PMT required.

– QUPID goal is < 0.1 n/year (Current R8778 is < 5 n/year) Irreducible background comes from pp-chain solar neutrino.

• ~10-7 /kg/keV/day ~0.5 event /ton/year (in 3-15 keVee window) – Assuming 99% rejection by S2/S1 cut.

Still investigating other backgrounds• Internal Krypton and Radon in Xenon

Photon Detection: Complete surface coverage by QUPID ensures > 3 pe/keV.



(2) Neutrino-less Double Beta Decay

Cosm

ology

Cosm

ology

(Figure from C. Giunti)

1027 yr

1028 yr

Normal Scheme Inverted Scheme

Sensitivity of Neutrinoless Double Beta Decayto Neutrino Mass

DBD Life Time

1026 yr

Laurent SIMARD, LAL - Orsay


Energy Resolution of XENON 10


Xe-129236 keV

Xe-131164 keV

= 0.9% at 2.5 MeV FWHM = 50 keV expected

Xe-129236 keV

Xe-131164 keV

136Xe Double Beta Decay and Gamma Background

(1 mBq / QUPID, 2m Xenon Detector)

2 DBD (1022 yrs)

0 DBD (1027 yrs)

0 cm

10 cm

30 cm

20 cm

B8 Solar

BG ~ 10-7 dru FWHM = 50 keV 5*10-4 /FWHM*kg*year

40 cm


50 cm


Expected Background from Gammas(1 mBq / QUPID, 1 year, Multi Hit Cut)

4.1 ton

6 /year

< 10–8 DRU

Expected No. of DBD Signals and Backgrounds(10 ton-year of Liquid Xenon, Window = 2479 ± 25

keV)


Self Shielding Cut (cm from wall) Life Time (Year)

No. of Background Events No. of 0-Neutrino DBD Signals

19.2 ton 9.8 ton 4.1 ton14.0 ton 6.6 ton

0.1 mBq/Qupid

1 mBq/Qupid

Expected No. of DBD Signals and Backgrounds(1 ton-year of Liquid Xenon, Window = 2479 ± 25

keV)


Self Shielding Cut (cm from wall) Life Time (Year)

No. of Background Events No. of 0-Neutrino DBD Signals

2.4 ton 0.5 ton1.2 ton 0.2 ton

0.1 mBq/Qupid

1 mBq/Qupid

Double Beta Decay Sensitivities


XAX (1 mBq) 136Xe 4000 50 0.0005 ~1027 15 – 95XAX (0.1mBq) 136Xe 4000 50 0.00005 ~1028 10 – 60

Double Beta Decay Experiments


EXO 1Ton

EXO200

NEMO3 (Mo)

NEMO3 (Se)

Mass (kg)

No.

of

Bac

kgro

unds

(/y

ear)

Cuoricino

GERDA I

GERDA II

GERDA IIISuper-NEMO (Se)

CUORE I

CUORE II

CUORE III

COBRA

CANDLES III

EXO 1Ton(Ba tag)

1025 yrs 1026 yrs 1027 yrs 1028 yrs

XAX (Enriched)

XAX (Natural)

XENON1T

Summary of DBD Detection All the gamma ray background can be

effectively removed. Low-radioactive QUPID is essential.

• < 1 mBq for > 1027 years• < 0.1 mBq for > 1028 years

Extensive active shielding. • 40 cm cut required (4 ton fiducial volume out of 19 ton.)

Multiple hit cut. Ba2+ tagging is not necessary, unlike EXO.

The tail from two neutrino double beta decays is negligible. based on XENON10, the energy resolution of the

double-phase Xenon should be superior to EXO. = 1.0% at 2.5 MeV (FWHM = 50 keV)• > 3 pe/keV is required



From MAX to XAX

MAX Detector


1 m

2 m

Xe2.4 ton(1.2 ton)

40Ar5 ton(2.5 ton)

DUSEL S4 Study funded by NSF ($3.5M)

MAX


2 m

Xe2.4 ton

(1.2 ton)

WIMP Double Beta Decay

40Ar10 ton(5 ton)

1 m

WIMP

G2

XAX Phase I


4 m

40Ar70 ton

(50 ton)

WIMP

2 m

Xe20 ton

(10 ton)

WIMP Double Beta Decay

129/131Xe2.4 ton

(1.2 ton)

Solar Neutrino

G3

XAX Phase II


4 m

40Ar70 ton

(50 ton)

WIMP

2 m

129/131Xe12 ton(6 ton)

WIMP (Spin odd)Solar Neutrino

WIMP (Spin even)Double Beta Decay

136Xe7 ton

(4 ton)

1.2 m

G4

MAX and XAX


Detector Size Target Mass

1m x 1m 2m x 2m 4m x 4mTotal Mass

Fiducial Mass

QUPID

3" at Top 190 750 3000

6" at Side/Bottom 210 850 3400

(ton) (ton)

MAX Xe 2.4 1.2

40Ar 10 5

XAX (Phase I) 129/131Xe 2.4 1.2

Xe 20 10

40Ar 70 50

XAX (Phase II) 129/131Xe 13 6

136Xe 7 4

40Ar 70 50

G2

G3

G4

MAX and XAX


Detector Size Target Mass No. Events


Fiducial Mass

WIMPDouble

Beta Decay

pp Solar Neutrino

Super Nova

Neutrino

QUPID 10-46 cm2 1027 years 10 kpc

3" at Top 190 750 3000 100 GeV 3x1053 erg

6" at Side/Bottom 210 850 3400 / 1yr / 1 yr / 1yr

(ton) (ton)

MAX Xe 2.4 1.2 12 0.4 11

40Ar 10 5 10 14

XAX (Phase I) 129/131Xe 2.4 1.2 12 500 11

Xe 20 10 100 3.3 95

40Ar 70 50 100 141

XAX (Phase II) 129/131Xe 13 6 60 2500 56

136Xe 7 4 40 30 39

40Ar 70 50 100 141

G2

G3

G4

MAX and XAX


Detector Size Target Mass No. Events


Fiducial Mass

Cost for Target

WIMPDouble

Beta Decay

pp Solar Neutrino

Super Nova

Neutrino

QUPID 10-46 cm2 1027 years 10 kpc

3" at Top 190 750 3000 100 GeV 3x1053 erg

6" at Side/Bottom 210 850 3400 / 1yr / 1 yr / 1yr

Cost for QUPID $2M $9M $36M (ton) (ton)

MAX Xe 2.4 1.2 $7M 12 0.4 11

40Ar 10 5 $3M 10 14

XAX (Phase I) 129/131Xe 2.4 1.2 ? 12 500 11

Xe 20 10 $40M 100 3.3 95

40Ar 70 50 $20M 100 141

XAX (Phase II) 129/131Xe 13 6 ? 60 2500 56

136Xe 7 4 ? 40 30 39

40Ar 70 50 100 141

G2

G3

G4


Summary

Summary on XAX XAX incorporates several innovative concepts:

The largest detector (> 10 ton) compatible with Argon and Xenon Background free

• Radiation-free photon detector: QUPID• Thick (20 cm) self shielding• Multi-hit cut and S2/S1 cut by double phase TPC• Pulse shape discrimination (for Ar) with “reconstructed” S1 signal

Best photon collection• 4π coverage of photon detectors (like single phase detectors)

XAX can achieve four important scientific goals: Systematic study of WIMP properties

• Sensitivity below 10-47 cm2 at 100 GeV (< 10-46 cm2 at 1 TeV)• Determination of Mass and Cross section• Target mass (A) dependence of Cross section (Argon vs. Xenon)• Spin dependence (129/131Xe vs. 132/134/136Xe)

Neutrino-less Double Beta Decay (by 136Xe)• Sensitivity up to 1028 years

pp-chain Solar Neutrino (by 129/131Xe)• Flux with 1% statistical error

Supernova Neutrino by elastic scattering• Total Energy with 8% statistical error• Temperature with 5% statistical error


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XAX Can DM and DBD detectors combined?

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