Sensitivity of Xenon dual-phase time projection chambers to rare event searches

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Submitted on 19 Sep 2019

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Sensitivity of Xenon dual-phase time projection chambers to rare event searches

Maxime Pierre

To cite this version:

Maxime Pierre. Sensitivity of Xenon dual-phase time projection chambers to rare event searches. 25ème Congrès Général de la Société Française de Physique, Jul 2019, Nantes, France. �hal-02292255�

Sensitivity of Xenon dual-phase time projection chambers to rare event searches

Subatech, UMR 6457 CNRS, IMT Atlantique, Université de Nantes, 4 rue Alfred Kastler, Nantes

maxime.pierre@etu.univ-nantes.fr

Maxime Pierre

2- Working Principle

1-Rare-events search

4-DARWIN

Dark Matter

Neutrinoless double beta decay 0

𝛖𝜷𝜷

3- Evolution & Results

• _{Current best limit on WIMP-nucleon}

cross-section achieved by XENON1T [1]

• _{Sensitive to other rare event searches:}

• _{First Observation of the double electron}

capture of 124Xe with XENON1T [2]:

!

• ! analysis in progress for XENON1T

T

= 1.8 × 10

y

0νββ

• _{S1 signal: Scintillation} • _{S2 signal: Ionisation}

• _{S1+S2 = 3D reconstruction}

• _{S1 & S2 = Energy reconstruction}

• _{S1/S2 = NR vs ER discrimination}

• _{Dark Matter evidences: Astrophysics and}

cosmological evidences indicate a missing mass that counts for 25% of the total mass of the universe.

• _{Best candidate: Weakly Interacting Massive Particle}

(WIMP)

• _{Massive, neutral particle} • _{Non-baryonic matter}

• _{Weakly interactive with baryonic matter and}

itself

• _{Stable particle}

• Neutrinos nature: Dirac or

Majorana particles ?

• Experimental signature:

Electronic recoil

• Energy deposition of the two

emitted electrons: Q-value of

the process = 2457 keV

• Observable: 0𝛖𝜷𝜷 Half-life

• _{Cylindrical dual-phase TPC : 2.6 m}

diameter and 2.6 m height

• _{40 tons active volume of LXe}

• _{Two arrays of PMTs (top and bottom)} • _{Muon and neutron veto systems}

• _{DARWIN will be sensitive to explore the}

WIMP parameter space down to the

irreducible background from neutrinos (neutrino floor) [3]

• _{If dark matter is observed DARWIN will}

be able to constrain its mass and its cross-section

Baseline Design

₀

_𝛖𝜷𝜷

_Sensitivity

Sketch of the DARWIN detector.

DM Sensitivity

χ

χ + N ⟶ χ + N

θ

Nucleus

Nuclear recoil energy < 100 keV

• _{After 10 years of exposure:}

! • 0𝛖𝜷𝜷 dedicated experiments: 136Xe abundance ≥ 90% • _{DM dedicated experiments:} natural abundance of 136Xe = 8.9% • 136Xe enrichement studied

S

= 3.0 × 10

y

Nuclear recoil (NR) Electronic recoil (ER)

• _{Detector requirements:}

• _{Large target mass, to}

increase probability of interaction/decay

• _{Background suppression,}

using shielding, radiopure

materials, modelization of the expected backgrounds

• WIMP

• Neutrons

• 𝜶-, 𝜷-, 𝛾- decay • _Electrons

References

[3] J. Aalbers et al, DARWIN: towards the ultimate Dark Matter detector, in Journal of Cosmology and Astroparticle Physics, 017-017 (2016)

¯ν e -e -¯ν 2𝛖𝛃𝛃 0𝛖𝛃𝛃 e -e -1 T0ν 1/2 = |mββ| 2 _{. |M}0ν_|2 _{. G}0ν_{(Q, Z)}

S

=

ln(2)

×

N

×

ϵ

×

enr

σ

×

M

bkg

exposure

×

ΔE

Phase-space factor Effective Majorana mass

Nuclear matrix element (NME)

• _{Direct detection:}

• _{Observable: WIMP-Nucleus}

cross-section and WIMP mass

• Physical constants and confidence level factor

• Studied isotope properties such as its abundance

• Detector characteristics: detection efficiency,

energy resolution, exposure