Noble Elements Roxanne GuenetteJocelyn Monroe

Jonathan AsaadiHugh LippincottAndrea PocarJen Raaf

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Our ScienceNeutrinos

• Oscillation precision measurements (δCP, mass ordering, θ23 octant, sterile νs)

• Neutrino interactions (from CEνNS to DIS)

• Astro neutrinos

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Dark Matter

• Direct detection (WIMPs, … )

0νββ

• Search for Majorana neutrinos

EXO/nEXO

Our Experiments (not exhaustive)

Neutrinos

• Current generation: ✓ArgoNeuT ✓MicroBooNE ✓LArIAT ✓35 ton ✓protoDUNEs ✓CAPTAIN ✓ ICARUS ✓SBND ✓COHERENT

• Future generation: ✓DUNE modules 1 & 2 ✓DUNE near detectors ✓DUNE modules 3 & 4

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Dark Matter

• Current generation: ✓LUX / LZ ✓XENON 10/100/1T/nT ✓Dark Side 50/20k ✓DEAP-3600 ✓Panda-X

• Future generation: ✓DARWIN / G3 LXe ✓GADMC/Argo ✓HeRALD ✓SBC

0νββ

• Current generation: ✓EXO-200 ✓NEXT-White ✓KamLand-Zen

• Future generation: ✓nEXO ✓NEXT-100/tonne ✓KL-Z+

Our TechnologiesNeutrinos

• Single-Phase Liquid Argon TPCs

• Dual-Phase Liquid Argon TPCs

• High-Pressure Argon Gas TPCs

• …

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Dark Matter

• Dual-phase Liquid Xenon TPCs

• Dual-phase LAr TPCs

• Single-phase LAr

• Liquid Helium

• Liquid Argon / Xenon Scintillating Bubble Chambers

• …

0νββ

• Single-phase Liquid Xenon TPCs

• High-Pressure Xenon Gas TPCs

• …

Our Current Physics NeedsNeutrinos

• Push Energy thresholds down to ~1MeV to enhance oscillation physics, supernovae νs study, to enable solar νs …

• Unambiguous readout

• Scalability

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Dark Matter

• Push Energy thresholds down to 1 meV/10 eV/1 keV to enable low mass DM/1 GeV DM/WIMPs.

• Reduce background rates

• Scalability

0νββ

• Improve Energy Resolution to sub-% FWHM

• Reduce background rates

• Scalability

Challenges for the Noble Element program

• Each science driver would highly benefit from enhanced capabilities of noble elements detectors

• Very different science goals lead to very different requirements

• Very different technologies have very different challenges

• Solutions to different challenges will vary widely based on needs

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Gathering input from the community

• Directly reached out to all neutrino/dark matter/0νββ collaborations

• Directly reached out to several experts (focused per institutions/labs)

• Gathered feedback via google form (23 responses)

• CPAD Workshop (4 submissions)

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Inputs• Light signals

✓ Looking at Infrared ✓ Liquid/Gas mixtures, doping to enhance light

collection ✓New PMTs, higher QE, readout electronics

and timing ✓High efficiency (~100%) light detectors for

VUV ✓New detection devices

• Purity/Backgrounds ✓Radon removal technics

• High Voltages ✓Understand dielectric strengths ✓Develop filters and feedthroughs

• …8

• Charge signals ✓ Purity impact, radio pure

electronics for cryogenics ✓Understand much better role/

impact of impurities ✓ Signal amplification ✓ Ion detection

• Calibration ✓Better understand neutrons

interactions, develop better simulations tools, study non-understood processes

✓ Field responses on channels

• Solid Xe

• Computing challenges

• Magnetization

Original idea• Keep PRDs and Key Challenges general to allow for R&D to

address all science. Specifics are in the text and can be detailed for each Science Drivers.

• Make sure to leave space for new ideas we have not even thought about yet!

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PRD #1 (More signal) Develop large area, high granularity, high efficiency signal collection technologies.

PRD #2 (Better Calibration) Develop calibration techniques to understand the response of noble elements to very low energy nuclear recoils, to better resolve energy depositions from different particles of all energies, and to fully characterize the entire volume of very large scale liquid and gaseous detectors.

PRD #3 (Scalability) Develop strategies to address known and hidden challenges associated with scalability of future noble element experiments.

PRD#1 (More Signal)Signal:

✓ Charge (from ionization electrons) ➡ Unambiguous 3D imaging like novel pixel charge readout ➡ Lower energy thresholds (large dynamic ranges)

✓ VUV light (from scintillation): ➡ High efficiency sensors ➡ High sensitivity to VUV light or efficient wavelength shifting

techniques to visible ➡ Large collection areas

✓ Potential novel channels (bubble formation (sound), quasiparticles, phonons, infrared light, ions)

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PRD#1 (More Signal) Some Key Challenges1.Addressing large channel count, low power consumption,

resilience to single point failure, and low energy threshold requirements

2.Improving light detection (all wavelengths), innovation with existing silicon-based detectors, exploration of non-silicon-based technologies sensitive to VUV signals, research into infrared and Cherenkov light sensors, and further development of wavelength shifting technologies and techniques

3.Exploring further signal amplification for both light, charge, and heat collection to allow for lower detection thresholds, which could significantly increase the physics reach of these detectors

•

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PRD#2 (Better Calibration)Effective calibration is a critical component for any science driver

✓ Resolve a new physics signal

✓ Reject backgrounds

✓ Tease out small shape effects

✓ Precisely measure of detector parameters requires deep understanding of detectors only possible through calibration

•

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PRD#2 (Better Calibration) Some Key Challenges1. Understanding the response of noble elements to sub-keV

recoils, an essential element for dark matter experiments

2.Uniform calibration of ton- and kiloton-scale detectors throughout their volume in the relevant energy range

3.Detailed understanding of the electric field responses

4. Improving energy resolution, particle and event ID, and topology to resolve signals and reject backgrounds. This includes responses to particles over a wide range of energies

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PRD#3 (Scalability)✓ Increased need for radiologically pure materials and their high

throughput screening, as well as removal of radioactive impurities.

✓ Advances in cryogenics and purification systems.

✓ Higher drift voltages, necessitating advances in the design of high voltage feedthroughs and their testing.

✓ The procurement and clean storage of large quantities of noble elements.

✓ Isotopic separation for enriched sources (e.g. for 0νββ) and background suppression (e.g. underground argon for dark matter).

✓ Deluge of data that will overwhelm existing computing resources without new R&D to approach all areas of computing from data acquisition to data analysis. 14

PRD#3 (Scalability) Some Key Challenges1. Very high voltage delivery solutions (use of resistive materials,

understanding the dielectric properties of elements under different purity conditions).

2. Large-scale purification solutions (for both electronegative species and radioactive contaminants and study the effects impurities).

3. New solutions for material screening and procurement of low-background detector materials (electronics components and understanding how those backgrounds generate signals in sensitive detectors).

4. Isotope separation and enrichment solutions.

5. Trigger, handling, processing, and analyzing the exponential increase in data volumes.

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New Guidance

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Neutrinos

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Very Preliminary

Dark Matter

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Very Preliminary

0νββ

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Very Preliminary

Not technically under HEP, but very close

overlap with DM

Conclusions• Our previous structure did include a lot of feedback from the

community. The “keeping things general” approach, allowed to ensure future R&D could find a home in our PRDs

• We have all the information we need (requirements, timescales, inputs, challenges, technology needs)

• We made a first attempt at arranging the ideas within the new framework -> May need extra Key Challenge(s) to relate to

• Intense discussions with the other groups will happen in the next few days to optimize (and reduce) the Noble Elements PRDs

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