The SABRE South Technical Design Report Executive Summary

A. Di Giacinto; A. E. Stuchbery; A. G. Williams; A. Mariani; A. R. Duffy; B. Suerfu; C. Vignoli; D. Tempra; E. Barberio; F. Dastgiri

REVIEW 2 major objections 5 minor 73 references

The SABRE South Technical Design Report Executive Summary

T0 review · 2 major / 5 minor · reviewed 2026-08-12 · deepseek-v4-flash

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Pith's one-line read This technical design report claims that SABRE South, a 35–50 kg NaI(Tl) detector in a Southern Hemisphere underground laboratory, can confirm or refute the DAMA/LIBRA annual modulation signal as dark matter with 5σ discovery or 3σ…

desk verdict A solid, detailed TDR executive summary whose abstract overstates the headline sensitivity and is internally inconsistent with the body's 50 kg/0.72 cpd and 35 kg/0.5 cpd scenarios. read the letter →

arxiv 2411.13889 v3 pith:NOBGZDO4 submitted 2024-11-21 physics.ins-det hep-ex

E. Barberio , T. Baroncelli , V. U. Bashu , L. J. Bignell , I. Bolognino , G. Brooks , S. S. Chhun , F. Dastgiri

show 37 more authors

A. Di Giacinto G. D'Imperio A. R. Duffy M. B. Froehlich T. Fruth G. Fu G. C. Hill R. S. James K. Janssens S. Kapoor G. J. Lane K. T. Leaver A. Mariani P. McGee L. J. McKie P. C. McNamara J. McKenzie W. J. D. Melbourne M. Mews G. Milana L. J. Milligan J. Mould V. Pettinacci K. J. Rule F. Scutti Z. Slavkovská O. Stanley A. E. Stuchbery B. Suerfu G. N. Taylor D. Tempra T. Tunningly P. Urquijo C. Vignoli A. G. Williams Y. Xing M. J. Zurowski

This is my paper · ORCID

classification physics.ins-dethep-ex PACS 95.35.+d29.40.Mc

keywords darkmatterdirectdetectionannualmodulationDAMA/LIBRANaI(Tl)scintillatorliquidvetoradiopuritySABRESouthundergroundlaboratory

topics Dark Matter

verification ladder T0 review T1 audit T2 compute T3 formal

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The reading

This technical design report describes SABRE South, a 35–50 kg sodium-iodide (NaI(Tl)) dark matter detector being built in the Southern Hemisphere, and argues it can settle the long-standing DAMA/LIBRA annual modulation claim by using the same target material with a lower background. The paper projects a total background of 0.72 cpd/kg/keV in the 1–6 keV region, below DAMA's own 0.8 cpd/kg/keV, which would make the reported 0.01 cpd/kg/keV modulation detectable. With that background, the paper claims a 5σ discovery or 3σ exclusion of the DAMA/LIBRA signal within two years of data taking. The design achieves the low background through seven ultra-pure crystals, a liquid scintillator veto that tags 40K decays, and a muon veto, with the Southern Hemisphere location also separating genuine dark matter modulation from seasonal effects.

What carries the argument

The machine is the combination of seven ultra-high purity NaI(Tl) crystals (35–50 kg) read out by two PMTs each, immersed in an 11,600 L linear alkylbenzene liquid scintillator instrumented with 18–32 R5912 PMTs, plus a plastic scintillator muon veto. The liquid scintillator actively vetoes events where a crystal-internal decay produces a high-energy gamma (notably the 40K electron-capture decay, whose 3 keV Auger/X-ray signature in the crystal is coincident with a 1.5 MeV gamma), which is the key mechanism that brings the background below DAMA's. The background model and the statistical sensitivity calculation are carried by simulations and the Poisson-sampling method of Ref. [10] that converts the projected 0.72 cpd/kg/keV into discovery/exclusion power.

What would settle it

Measure the total background rate in the 1–6 keVee region during the first months of operation and compare with 0.72 cpd/kg/keV; if the measured rate exceeds about 1 cpd/kg/keV, or the 40K coincidence veto efficiency falls below the simulated factor, the two-year 5σ discovery / 3σ exclusion projection is falsified.

Watch

Extended reading notes

Core claim

The central claim is that a NaI(Tl) detector with the same target material as DAMA/LIBRA, but with radiogenic background below DAMA's, can decisively test the annual modulation signal. Using measured radiopurity of a Proof-of-Principle crystal (natK 4.3 ppb, 210Pb 0.5 mBq/kg) and a full Geant4 background simulation, SABRE South predicts 0.72 cpd/kg/keV total background in 1–6 keVee, of which 0.52 cpd/kg/keV is intrinsic crystal radiogenic background after liquid scintillator veto. The veto suppresses 40K by a factor of 10 and the total background by 27%. The resulting sensitivity reaches 5σ discovery of a DAMA-like modulation (amplitude 0.0105–0.0118 cpd/kg/keV) after two years and 3σ exclusion after two years (5σ exclusion after about three years).

Load-bearing premise

The projected 0.72 cpd/kg/keV background assumes the seven production crystals reach the radiopurity of the single measured Proof-of-Principle crystal and that the simulated liquid scintillator veto rejection (factor of 10 for 40K, 27% total background reduction) is achieved in the real detector.

Editorial extensions

If this is right

If the projection holds, SABRE South will deliver a same-target-material test of DAMA/LIBRA with better background than DAMA, so the annual modulation claim is either confirmed at 5σ or excluded at 3σ within two years.
A null result would rule out the DAMA/LIBRA modulation as a WIMP signal for standard halo assumptions, given the same NaI(Tl) target.
A positive detection would corroborate DAMA/LIBRA and motivate follow-up with SABRE North for a two-hemisphere seasonal check.
The liquid scintillator veto technique, if validated, gives other NaI(Tl) experiments a path to suppress 40K backgrounds.
Beyond dark matter, the veto can serve as a supernova neutrino early warning with roughly six events from a 10 kpc core-collapse supernova.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

The two-year sensitivity timeline is optimistic if crystal growth or insertion slips; the real early discriminator will be the measured background after commissioning, which can be checked against 0.72 cpd/kg/keV well before any modulation accumulates.
If production crystals fail to match the Proof-of-Principle crystal's 210Pb level, the 210Pb continuum is largely un-vetoable, so that single contaminant is the most important crystal parameter to watch for preserving the sensitivity projection.
The Southern Hemisphere location only helps if seasonal backgrounds are modelled; a combined two-hemisphere dataset could directly fit a global modulation phase against hemisphere-specific seasonal backgrounds.
If the background comes in at 1 cpd/kg/keV instead of 0.72, achieving the same sensitivity would require roughly 40% more exposure than the two-year plan.

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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Desk Editor's Note

read the letter

This is a competent, useful TDR executive summary for SABRE South, but read the body, not just the abstract. The abstract says 5σ discovery or 3σ exclusion after two years at 0.72 cpd/kg/keV, while Section 3.1 explicitly requires <0.5 cpd/kg/keV for the 35 kg scenario, and Section 10 only derives 5σ discovery in two years and 5σ exclusion in 3.1 years for the 50 kg scenario. The 3σ exclusion at two years never appears in the calculations. That is a genuine internal inconsistency, not a nitpick.

What the paper does well: it gives a concrete, self-contained description of the full SABRE South design—crystals, copper enclosures, LAB veto, muon veto, calibration systems, DAQ, and shielding. The engineering detail is solid and specific: the insertion system, gas handling, cleanliness protocols, and PMT characterisation plans are all described at a level that makes the detector real. The background estimate is traced to measured radiopurity of the NaI-033 crystal and the simulation study in Ref [11], so the provenance is clear, even though no new data or code ship with this report.

Soft spots, in order of seriousness: first, the abstract inconsistency is a real flaw that needs fixing—either by restricting the abstract to the 50 kg scenario or by adding the 3σ exclusion curve for two years. Second, Table 4 lists bis-MSB as ~15 g/L, which is a three-orders-of-magnitude typo; the text and summary correctly say 15 mg/L. Third, the sensitivity projection has no systematic uncertainties attached; the extrapolation from one test crystal to seven production crystals is a stated risk in the text but deserves at least one cautionary sentence in the conclusions. None of this undermines the central argument that an ultra-low-background NaI(Tl) detector in the Southern Hemisphere can give a definitive same-target test of DAMA/LIBRA.

This is a paper for the NaI(Tl) dark matter community and for detector physicists interested in active veto designs. It is not a new physics result, but it is a careful design document that merits referee time. With the abstract reconciled to the body and the table typo fixed, it would be a solid JINST-style TDR summary. I would send it to peer review with a request for those revisions.

Referee Report

2 major / 5 minor

Summary. The SABRE South Technical Design Report executive summary describes the technical design of the SABRE South NaI(Tl) dark matter detector to be installed at the Stawell Underground Physics Laboratory. It covers the crystal modules, liquid scintillator veto, muon veto, calibration systems, DAQ, shielding, and projected sensitivity to a DAMA/LIBRA-like annual modulation signal. The paper claims an expected total background of 0.72 cpd/kg/keV in the 1–6 keV region and states that SABRE South can test the DAMA/LIBRA signal with 5σ discovery or 3σ exclusion after two years of data taking.

Significance. If the projected sensitivity is realized, SABRE South would provide a decisive, same-target test of the DAMA/LIBRA annual modulation claim, with the unique advantage of a Southern Hemisphere location for disentangling seasonal effects. The paper's strengths are its detailed, engineering-level technical design, the use of Geant4 simulations and measured radiopurity of the NaI-033 proof-of-principle crystal, and the explicit discussion of two crystal growth scenarios with different background requirements. The projected sensitivity rests on extrapolating the radiopurity of one crystal to seven production crystals and on simulated veto performance, which are reasonable but should be clearly labeled as projections.

major comments (2)

[Abstract / Sec. 3.1 / Sec. 10] The abstract's headline sensitivity is internally inconsistent with the body. The abstract states that 'with an expected total background of 0.72 cpd/kg/keV, SABRE South can test the DAMA/LIBRA signal with 5σ discovery or 3σ exclusion after two years' while also stating that the target mass is 'either 35 kg or 50 kg'. Section 3.1 explicitly requires a total background of less than 0.5 cpd/kg/keV for the 35 kg scenario to achieve 5σ discovery or 3σ exclusion. Section 10 computes sensitivity only for the 50 kg scenario at 0.72 cpd/kg/keV, reporting 5σ discovery after two years and 5σ exclusion after 3.1 years; no derivation of a 3σ exclusion after two years is given. The abstract should be revised to report the sensitivity separately for each mass scenario and to either derive the 3σ exclusion timescale or remove it.
[Sec. 3.1 / Sec. 5 / Sec. 10] The projected background rate of 0.72 cpd/kg/keV is a load-bearing input, but it rests on extrapolating the measured radiopurity of the single NaI-033 proof-of-principle crystal (Ref. [34]) to seven production crystals grown by SICCAS or RMD, and on simulated veto rejection of 40K by a factor of 10 and total background suppression of 27% (Sec. 5, Ref. [11]). The paper notes that the 35 kg scenario requires radiogenic background below 0.3 cpd/kg/keV via zone refining, but no production-crystal measurements are yet reported. The authors should state the systematic uncertainty on the 0.72 cpd/kg/keV background, specify the contingency if production crystals do not meet NaI-033 purity, or explicitly label the sensitivity projection as a design goal.

minor comments (5)

[Sec. 4.5] In the gas handling system section, 'nitrogren' should be 'nitrogen'.
[Sec. 3.1] The phrase 'much lower than than the other' contains a duplicated 'than' and should be corrected.
[Sec. 8.1] The V2730 digitiser is referred to as 'V7230' in the first sentence of the V2730 paragraph; this should be 'V2730'.
[Sec. 11] The summary states '5σ discovery (5σ exclusion) power to a DAMA-like signal after 2 (3) years', which differs from the abstract's '3σ exclusion after two years'; these statements should be made consistent.
[Sec. 5.4] Several passages lack spaces between words (e.g., 'Thenoisecharacteristics' in Sec. 5.4); these should be fixed in the final typeset version.

Circularity Check

0 steps flagged · score 2.0 of 10

No forbidden circularity: the sensitivity projection is a Monte Carlo forecast from measured crystal purity and a generic statistical method; the abstract's 35 kg/50 kg sensitivity mismatch is a correctness issue, not a circular step.

full rationale

The paper's central sensitivity claim is an input-to-output projection, not a fitted prediction. The expected background of 0.72 cpd/kg/keV is taken from the collaboration's own simulation (Ref. [11]) and ultimately from measured radiopurity of the NaI-033 proof-of-principle crystal (Ref. [34]); the 5-sigma discovery/exclusion power is computed with the published methodology of Ref. [10], sampling Poisson time bins for background-only and signal-plus-background hypotheses. Neither quantity is defined in terms of the DAMA/LIBRA signal being tested, and no parameter is fitted to DAMA data to produce the quoted sensitivity. The self-citations are load-bearing in the sense that the expected performance rests on the collaboration's own simulation and analysis papers, but those papers are themselves based on measured crystal purity and stated statistical assumptions, so the derivation does not reduce to its own conclusion. Separately, and as a correctness rather than circularity issue, the abstract states "5$\sigma$ discovery or 3$\sigma$ exclusion after two years of data taking" while Sec. 10 computes sensitivity only for the 50 kg, 0.72 cpd/kg/keV scenario and reports 5$\sigma$ exclusion after 3.1 years, not after two years; Sec. 3.1 says the 35 kg scenario requires a total background below 0.5 cpd/kg/keV to reach the same 5$\sigma$/3$\sigma$ goals. This internal inconsistency is not a circular derivation and therefore does not raise the circularity score beyond a low value reflecting the paper's reliance on its own prior work.

Assumptions & free parameters 4 free parameters · 4 assumptions · 0 invented entities

The paper introduces no new particles, forces, or entities. Its central claim rests on assumed detector parameters: the projected background rate, light yield, veto threshold, and target mass, all of which are inputs from earlier SABRE work or design choices. The simulations and the representativeness of the single test crystal are the key assumptions that the reader does not pay for upstream.

free parameters (4)

Total background rate in 1-6 keV ROI = 0.72 cpd/kg/keV
Projected total background used to compute the 5 sigma discovery and 3 sigma exclusion sensitivity. It is taken from the collaboration's own simulation (Ref [11]) based on measured NaI-033 crystal purity; the claim in this paper depends directly on this assumed value.
Crystal light yield = 11.1 PE/keV
Measured on the proof-of-principle crystal (Ref [34]) and used to justify the 1 keV energy threshold assumed in the sensitivity calculation. The paper notes the final light yield might be about 20% higher, so the 1 keV threshold is not guaranteed.
Veto energy threshold = 50 keV (nominal); 20 keV for 50% efficiency
Design parameter used to compute the liquid scintillator veto efficiency, the 40K rejection factor of 10, and the 27% total background suppression. The sensitivity projection depends on this threshold.
Active target mass = 50 kg or 35 kg
Design choice. The sensitivity numbers in Section 10 assume 50 kg; the 35 kg scenario requires a stricter background of less than 0.5 cpd/kg/keV to reach the same sensitivity, so the claimed reach is conditional on the mass scenario.

assumptions (4)

domain assumption Geant4 simulations accurately model the detector response, background energy depositions, and veto performance.
All projected backgrounds and veto efficiencies in Sections 3, 5, and 10 are based on Geant4 simulations (Refs [11], [26], [35]). The sensitivity claim inherits any bias in the simulation code.
ad hoc to paper The radiopurity of the SABRE Proof-of-Principle crystal NaI-033 is representative of the seven production crystals.
Section 3.1 states the crystal background spectrum is taken from NaI-033 measurements (Ref [34]), while the production crystals are being grown by different vendors (SICCAS and RMD). The central background rate of 0.72 cpd/kg/keV relies on this extrapolation.
domain assumption The standard halo model annual modulation conditions apply, including a 1-year period, a June peak, and keV-scale energies.
Section 1.1 lists these conditions from the dark matter halo literature (Refs [2], [6]), and the sensitivity calculation adopts them as the signal hypothesis.
domain assumption DAMA/LIBRA's reported modulation amplitude of 0.0118 cpd/kg/keV is the correct target signal.
The discovery potential calculation in Section 10 uses this amplitude from DAMA/LIBRA data as the signal model. If the DAMA signal's amplitude or phase were materially different, the projected sensitivity would change.

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Cite this review

Pith. "Pith review of The SABRE South Technical Design Report Executive Summary." pith.science (2026). https://pith.science/paper/NOBGZDO4

@misc{pith2026241113889,
  author       = {Pith},
  title        = {Pith review of: The SABRE South Technical Design Report Executive Summary},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/NOBGZDO4}},
  note         = {Machine review of arXiv:2411.13889}
}

abstract

In this technical design report (TDR) executive summary we describe the SABRE South detector to be built at the Stawell Underground Physics Laboratory (SUPL). The SABRE South detector is designed to test the long-standing DAMA/LIBRA signal of an annually modulating rate consistent with dark matter by using the same target material. Located in the Southern Hemisphere, the detector is uniquely positioned to disentangle modulating seasonal effects. SABRE South uses seven ultra-high purity NaI(Tl) crystals (with a total target mass of either 35 kg or 50 kg), hermetically sealed in copper enclosures that are suspended within a liquid scintillator active veto. High quantum efficiency and low background Hamamatsu R11065 photomultiplier tubes are directly coupled to both ends of the crystal, and enclosed with the crystal in an oxygen free copper enclosure. The active veto system consists of 11.6 kL of linear alkylbenzene (LAB) doped with a mixture of fluorophores and contained in a steel vessel, which is instrumented with at least 18 Hamamatsu R5912 photomultipliers. The active veto tags key radiogenic backgrounds intrinsic to the crystals, such as ${^{40}}$K, and is expected to suppress the total background by 27% in the 1-6 keV region of interest. In addition to the liquid scintillator veto, a muon veto is positioned above the detector shielding. This muon veto consists of eight EJ-200 scintillator modules, with Hamamatsu R13089 photomultipliers coupled to both ends. With an expected total background of 0.72 cpd/kg/keV, SABRE South can test the DAMA/LIBRA signal with 5$\sigma$ discovery or 3$\sigma$ exclusion after two years of data taking.

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Works this paper leans on

73 extracted references · 59 canonical work pages

[11]

REMOVE ALL SHARP EDGES & SPATTER

work page
[34]

Carlin et al.,COSINE-100 Full Dataset Challenges the Annual Modulation Signal of DAMA/LIBRA, arXiv:2409.13226

COSINE-100Collaboration, N. Carlin et al.,COSINE-100 Full Dataset Challenges the Annual Modulation Signal of DAMA/LIBRA, arXiv:2409.13226

arXiv
[7]

TUBE O.D, NON-ROTATABLE S/S 304L 8 7 CONFLAT HALF NIPPLE, N3 1N-600, 6

BOTTOM TORI. HEAD STIFFENING RING TO BE STITCH WELDED BUT WITH 200mm CONTINOUS WELDING AS IT APPROACHES THE LEGS 0 ISSUED FOR CONSTRUCTION DH JBL - 24/01/2018 REV DETAILS DRN CHK APP DATE 24/01/2018 13:16:51 INSIDE 2600 O.D 6 THK. W1 SHELL LONG. WELD 2576 O/S HEADS (356) 76 S.F 1500 W1 W1 60° 2983 3132 1 2 1 6 5 4 3 N1 N2N3 1600 520 30° TYP. 0° 90° 180°...

work page 2018
[8]

FLANGE BOLT HOLES TO STRADDLE NATURAL CENTERLINES UNO

work page
[9]

ALL NOZZLES TO BE PROTECTED WITH WOODEN BLANKS AND SECURED WITH AT LEAST 2 BOLTS DURING TRANSPORTATION

work page
[10]

AND LONG

ALL CIRC. AND LONG. WELDS TO BE FULL PENETRATION BUTT WELDS

work page
[12]

LOW RADIOACTIVE PLATES AND SPECIFIC CLEANLINESS PER UoM REQUIREMENTS

work page
[13]

PAD AND LIFTING LUG WELDS

100% SURFACE INSPECTION FOR ALL COMP. PAD AND LIFTING LUG WELDS

work page

Show all 73 references

[14]

BOTTOM TORI. HEAD STIFFENING RING TO BE STITCH WELDED BUT WITH 200mm CONTINOUS WELDING AS IT APPROACHES THE LEGS 0 ISSUED FOR CONSTRUCTION DH JBL - 24/01/2018 REV DETAILS DRN CHK APP DATE 24/01/2018 13:16:51 INSIDE 2600 O.D 6 THK. W1 SHELL LONG. WELD 2576 O/S HEADS (356) 76 S....

2018
[15]

Freese,Review of Observational Evidence for Dark Matter in the Universe and in upcoming searches for Dark Stars,EAS Publ

K. Freese,Review of Observational Evidence for Dark Matter in the Universe and in upcoming searches for Dark Stars,EAS Publ. Ser.36(2009) 113–126, [arXiv:0812.4005]

2009 arXiv
[16]

Froborg and A

F. Froborg and A. R. Duffy,Annual Modulation in Direct Dark Matter Searches, J. Phys. G47 (2020), no. 9 094002, [arXiv:2003.04545]

2020 arXiv
[17]

V. C. Rubin and W. K. Ford, Jr.,Rotation of the Andromeda Nebula from a Spectroscopic Survey of Emission Regions,Astrophys. J.159 (1970) 379–403

1970
[18]

Zwicky,On the Masses of Nebulae and of Clusters of Nebulae, Astrophys

F. Zwicky,On the Masses of Nebulae and of Clusters of Nebulae, Astrophys. J.86 (1937) 217–246

1937
[19]

PlanckCollaboration, P. A. R. Ade et al.,Planck 2015 results. XIII. Cosmological parameters, Astron. Astrophys.594 (2016) A13, [arXiv:1502.01589]

2016 arXiv
[20]

Freese, M

K. Freese, M. Lisanti, and C. Savage,Colloquium: Annual modulation of dark matter,Rev. Mod. Phys.85(Nov, 2013) 1561–1581

2013
[21]

Antonello et al.,The SABRE project and the SABRE Proof-of-Principle, Eur

SABRECollaboration, M. Antonello et al.,The SABRE project and the SABRE Proof-of-Principle, Eur. Phys. J. C79(2019), no. 4 363, [arXiv:1806.09340]

2019 arXiv
[22]

Bernabei et al.,Annual modulation results from DAMA/LIBRA,Int

R. Bernabei et al.,Annual modulation results from DAMA/LIBRA,Int. J. Mod. Phys. Conf. Ser.51 (2023) 2361008

2023
[23]

Cataldi,Status of SABRE North at LNGS and radiopurity of SABRE NaI(Tl) crystals,PoSICHEP2024(2025) 754

Sabre NorthCollaboration, G. Cataldi,Status of SABRE North at LNGS and radiopurity of SABRE NaI(Tl) crystals,PoSICHEP2024(2025) 754

2025
[24]

Zurowski and E

M. Zurowski and E. Barberio,Influence of NaI background and mass on testing the DAMA modulation,Eur. Phys. J. C82(12, 2022) 1122

2022
[25]

Barberio et al.,Simulation and background characterisation of the SABRE south experiment,The European Physical Journal C83 (Sept., 2023)

SABRE SouthCollaboration, E. Barberio et al.,Simulation and background characterisation of the SABRE south experiment,The European Physical Journal C83 (Sept., 2023)

2023
[26]

Ibe et al.,Migdal Effect in Dark Matter Direct Detection Experiments,JHEP03 (2018) 194, [arXiv:1707.07258]

M. Ibe et al.,Migdal Effect in Dark Matter Direct Detection Experiments,JHEP03 (2018) 194, [arXiv:1707.07258]

2018 arXiv
[27]

Pospelov et al.,Bosonic super-WIMPs as keV-scale dark matter,Phys

M. Pospelov et al.,Bosonic super-WIMPs as keV-scale dark matter,Phys. Rev. D78(2008) 115012, [arXiv:0807.3279]

2008 arXiv
[28]

Al Kharusi et al.,SNEWS 2.0: a next-generation supernova early warning system for multi-messenger astronomy,New J

SNEWSCollaboration, S. Al Kharusi et al.,SNEWS 2.0: a next-generation supernova early warning system for multi-messenger astronomy,New J. Phys.23(2021), no. 3 031201, [arXiv:2011.00035]

2021 arXiv
[29]

Bernabei et al.,The DAMA project: Achievements, implications and perspectives,Progress in Particle and Nuclear Physics114 (2020) 103810

DAMACollaboration, R. Bernabei et al.,The DAMA project: Achievements, implications and perspectives,Progress in Particle and Nuclear Physics114 (2020) 103810

2020
[30]

R. Bernabei et al.,The dark matter: DAMA/LIBRA and its perspectives, in16th Marcel Grossmann Meeting on Recent Developments in Theoretical and Experimental General Relativity, Astrophysics and Relativistic Field Theories, 10, 2021.arXiv:2110.04734

2021 arXiv
[31]

Navas et al.,Review of particle physics,Phys

Particle Data GroupCollaboration, S. Navas et al.,Review of particle physics,Phys. Rev. D110 (2024), no. 3 030001

2024
[32]

Adhikari et al.,An induced annual modulation signature in COSINE-100 data by DAMA/LIBRA’s analysis method,Sci

COSINE-100Collaboration, G. Adhikari et al.,An induced annual modulation signature in COSINE-100 data by DAMA/LIBRA’s analysis method,Sci. Rep.13(2023), no. 1 4676, [arXiv:2208.05158]

2023 arXiv
[33]

SABRE SouthCollaboration, R. S. James et al.,The DAMA/LIBRA signal: an induced modulation effect?, arXiv:2408.08697. – 41 –

arXiv
[35]

Coarasa et al.,ANAIS–112 three years data: a sensitive model independent negative test of the DAMA/LIBRA dark matter signal,Commun

ANAIS–112Collaboration, I. Coarasa et al.,ANAIS–112 three years data: a sensitive model independent negative test of the DAMA/LIBRA dark matter signal,Commun. Phys.7 (2024), no. 1 345, [arXiv:2404.17348]

2024 arXiv
[36]

Adhikari et al.,Three-year annual modulation search with COSINE-100,Phys

COSINE-100Collaboration, G. Adhikari et al.,Three-year annual modulation search with COSINE-100,Phys. Rev. D106 (2022), no. 5 052005, [arXiv:2111.08863]

2022 arXiv
[37]

Coarasa et al.,Improving ANAIS-112 sensitivity to DAMA/LIBRA signal with machine learning techniques,JCAP11 (2022) 048, [arXiv:2209.14113]

ANAISCollaboration, I. Coarasa et al.,Improving ANAIS-112 sensitivity to DAMA/LIBRA signal with machine learning techniques,JCAP11 (2022) 048, [arXiv:2209.14113]. [Erratum: JCAP 06, E01 (2023)]

2022 arXiv
[38]

COSINE-100Collaboration, G. H. Yu et al.,Lowering threshold of NaI(Tl) scintillator to 0.7 keV in the COSINE-100 experiment,JINST19 (2024), no. 12 P12013, [arXiv:2408.14688]

2024 arXiv
[39]

ANAISCollaboration, I. Coarasa Casas,ANAIS-112: the most sensitive experiment to test the DAMA/LIBRA signal in a model independent way, in15th International Workshop on the Identification of Dark Matter, L’Aquila Italy, 2024

2024
[40]

Agostinelli et al.,GEANT4 - A Simulation Toolkit,Nucl

GEANT4Collaboration, S. Agostinelli et al.,GEANT4 - A Simulation Toolkit,Nucl. Instrum. Meth. A 506 (2003) 250–303

2003
[41]

Fedynitch, W

A. Fedynitch, W. Woodley, and M.-C. Piro,On the Accuracy of Underground Muon Intensity Calculations, Astrophys. J.928 (2022), no. 1 27, [arXiv:2109.11559]

2022 arXiv
[42]

Guo et al.,Muon flux measurement at China Jinping Underground Laboratory,Chin

JNECollaboration, Z. Guo et al.,Muon flux measurement at China Jinping Underground Laboratory,Chin. Phys. C45 (2021), no. 2 025001, [arXiv:2007.15925]

2021 arXiv
[43]

K. W. Kim et al.,Tests on NaI(Tl) crystals for WIMP search at the Yangyang Underground Laboratory,Astropart. Phys.62(2015) 249–257, [arXiv:1407.1586]

2015 arXiv
[44]

Calaprice et al.,High sensitivity characterization of an ultrahigh purity NaI(Tl) crystal scintillator with the SABRE proof-of-principle detector,Phys

F. Calaprice et al.,High sensitivity characterization of an ultrahigh purity NaI(Tl) crystal scintillator with the SABRE proof-of-principle detector,Phys. Rev. D104(2021), no. 2 L021302, [arXiv:2105.09225]

2021 arXiv
[45]

Amaré et al.,Analysis of backgrounds for the ANAIS-112 dark matter experiment, Eur

ANAISCollaboration, J. Amaré et al.,Analysis of backgrounds for the ANAIS-112 dark matter experiment, Eur. Phys. J. C79 (2019) 412

2019
[46]

Adhikari et al.,Background model for the NaI(Tl) crystals in COSINE-100,Eur

COSINECollaboration, P. Adhikari et al.,Background model for the NaI(Tl) crystals in COSINE-100,Eur. Phys. J.C78(2018) 490, [arXiv:1804.05167]

2018 arXiv
[47]

Suerfu et al.,Growth of ultra-high purity NaI(Tl) crystals for dark matter searches,Physical Review Research2 (2020), no

B. Suerfu et al.,Growth of ultra-high purity NaI(Tl) crystals for dark matter searches,Physical Review Research2 (2020), no. 1

2020
[48]

Antonello et al.,Characterization of sabre crystal nai-33 with direct underground counting, The European Physical Journal C81(Apr, 2021)

SABRECollaboration, M. Antonello et al.,Characterization of sabre crystal nai-33 with direct underground counting, The European Physical Journal C81(Apr, 2021)

2021
[49]

Antonello et al.,Monte Carlo simulation of the SABRE PoP background, Astropart

SABRECollaboration, M. Antonello et al.,Monte Carlo simulation of the SABRE PoP background, Astropart. Phys.106(2019) 1–9, [arXiv:1806.09344]

2019 arXiv
[50]

G. H. Yu et al.,Depth profile study of210Pb in the surface of an NaI(Tl) crystal,Astropart. Phys.126 (2021) 102518, [arXiv:2001.06132]

2021 arXiv
[51]

Bernabei et al.,The DAMA/LIBRA apparatus,Nucl

DAMACollaboration, R. Bernabei et al.,The DAMA/LIBRA apparatus,Nucl. Instruments Methods Phys. Res. Sect. A Accel. Spectrometers, Detect. Assoc. Equip.592 (2008), no. 3 297–315

2008
[52]

Tomei et al.,Status and prospects for SABRE North,PoSICHEP2022(11, 2022) 1223

C. Tomei et al.,Status and prospects for SABRE North,PoSICHEP2022(11, 2022) 1223. – 42 –

2022
[53]

Suerfu,Developing Ultra Low-Background Sodium-Iodide Crystal Detector for Dark Matter Searches

B. Suerfu,Developing Ultra Low-Background Sodium-Iodide Crystal Detector for Dark Matter Searches. PhD thesis, Department of Physics, Princeton University, 2018

2018
[54]

L. J. Bignell et al.,Quenching factor measurements of sodium nuclear recoils in NaI:Tl determined by spectrum fitting, JINST16(2021), no. 07 P07034, [arXiv:2102.02833]

2021 arXiv
[55]

Barrow et al.,Qualification tests of the R11410-21 photomultiplier tubes for the XENON1T detector, Journal of Instrumentation12(jan, 2017) P01024

P. Barrow et al.,Qualification tests of the R11410-21 photomultiplier tubes for the XENON1T detector, Journal of Instrumentation12(jan, 2017) P01024

2017
[56]

Akimov et al.,Peculiarities of the Hamamatsu R11410-20 photomultiplier tubes, PoS PhotoDet2015(2016) 025

D. Akimov et al.,Peculiarities of the Hamamatsu R11410-20 photomultiplier tubes, PoS PhotoDet2015(2016) 025

2016
[57]

D. Y. Akimov et al.,Characterization of the low-background Hamamatsu R11410- 20 cryogenic PMTs for the RED100 detector,
[58]

Bernabei et al.,Particle Dark Matter and DAMA/LIBRA,AIP Conf

DAMACollaboration, R. Bernabei et al.,Particle Dark Matter and DAMA/LIBRA,AIP Conf. Proc. 1223 (2010), no. 1 50–59, [arXiv:0912.0660]

2010 arXiv
[59]

Bernabei et al.,First Model Independent Results from DAMA/LIBRA–Phase2,Universe4 (2018), no

DAMACollaboration, R. Bernabei et al.,First Model Independent Results from DAMA/LIBRA–Phase2,Universe4 (2018), no. 11 116, [arXiv:1805.10486]. [Nucl. Phys. Atom. Energy19,no.4,307(2018)]

2018 arXiv
[60]

Anderson et al.,Development, characterisation, and deployment of the SNO+ liquid scintillator, Journal of Instrumentation16(5, 2021) P05009

M. Anderson et al.,Development, characterisation, and deployment of the SNO+ liquid scintillator, Journal of Instrumentation16(5, 2021) P05009

2021
[61]

M. Li et al.,Separation of scintillation and cherenkov lights in linear alkyl benzene,Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment830(11, 2015)

2015
[62]

Abe et al.,Characterization of the Spontaneous Light Emission of the PMTs used in the Double Chooz Experiment,JINST11 (2016), no

Double ChoozCollaboration, Y. Abe et al.,Characterization of the Spontaneous Light Emission of the PMTs used in the Double Chooz Experiment,JINST11 (2016), no. 08 P08001, [arXiv:1604.06895]

2016 arXiv
[63]

Eljentechnology plastic scinitllators

“Eljentechnology plastic scinitllators.”https://eljentechnology.com/products/ plastic-scintillators/ej-200-ej-204-ej-208-ej-212 . Accessed: 2022-05-1

2022
[64]

V1743 & VX1743 User Manual UM2750

CAEN S.p.A, “V1743 & VX1743 User Manual UM2750.” https://www.caen.it/products/v1743/, Nov, 2020

2020
[65]

Mei and A

D. Mei and A. Hime,Muon-induced background study for underground laboratories,Phys. Rev. D73 (2006) 053004, [astro-ph/0512125]. [Erratum: Phys.Rev.D 109, 019901 (2024)]

2006 arXiv
[66]

Allison et al.,Recent developments in Geant4,Nucl

J. Allison et al.,Recent developments in Geant4,Nucl. Instrum. Meth. A835 (2016) 186–225

2016
[67]

Hagmann, D

C. Hagmann, D. Lange, and D. Wright,Cosmic-ray shower generator (CRY) for Monte Carlo transport codes, in10.1109/NSSMIC.2007.4437209, 10, 2007

2007
[68]

Amaré et al.,Performance of ANAIS-112 experiment after the first year of data taking,The European Physical Journal C79(2019), no

ANAISCollaboration, J. Amaré et al.,Performance of ANAIS-112 experiment after the first year of data taking,The European Physical Journal C79(2019), no. 3

2019
[69]

Y. Z. et al,Laser calibration system in JUNO,JINST14 (2019) P01009

2019
[70]

Grafana documentation

Grafana Labs, “Grafana documentation.” https://grafana.com/docs/, 2018

2018
[71]

Rabenstein and J

B. Rabenstein and J. Volz,Prometheus: A next-generation monitoring system (talk), USENIX Association (May, 2015)

2015
[72]

V1730/VX1730 & V1725/VX1725 User Manual UM2792

CAEN S.p.A, “V1730/VX1730 & V1725/VX1725 User Manual UM2792.” https://www.caen.it/products/v1730/, May, 2021. – 43 –

2021
[73]

V2730/VX2730 User Manual UM9713

CAEN S.p.A, “V2730/VX2730 User Manual UM9713.” https://www.caen.it/products/vx1730/, October, 2024

2024
[74]

V2495/VX2495 User Manual UM5175

CAEN S.p.A, “V2495/VX2495 User Manual UM5175.” https://www.caen.it/products/v2495/, Aug, 2019

2019
[75]

SY5527-SY5527LC Power Supply System User Manual UM2707

CAEN S.p.A, “SY5527-SY5527LC Power Supply System User Manual UM2707.” https://www.caen.it/products/sy5527/, Apr, 2020

2020
[76]

A7435 A7435 24 Channel 3.5 kV/3.5 mA (9W)

CAEN S.p.A, “A7435 A7435 24 Channel 3.5 kV/3.5 mA (9W).” https://www.caen.it/products/A7435/, Sep, 2022

2022
[77]

Krishnan et al.,A scalable and reconfigurable industrial-grade slow control system for sabre-south dark matter experiment,Journal of Instrumentation16 (mar, 2021) P03002

S. Krishnan et al.,A scalable and reconfigurable industrial-grade slow control system for sabre-south dark matter experiment,Journal of Instrumentation16 (mar, 2021) P03002

2021
[78]

ethercat

D. L. S. Controls, “ethercat.”https://github.com/dls-controls/ethercat, 2022

2022
[79]

Aprile et al.,Material screening and selection for XENON100, Astroparticle Physics35(2011), no

XENON100Collaboration, E. Aprile et al.,Material screening and selection for XENON100, Astroparticle Physics35(2011), no. 2 43 – 49. – 44 –

2011

Pith tools

Reviewed August 12, 2026 · model on record in the stance chip above.

[1] [11]

REMOVE ALL SHARP EDGES & SPATTER

work page

[2] [34]

Carlin et al.,COSINE-100 Full Dataset Challenges the Annual Modulation Signal of DAMA/LIBRA, arXiv:2409.13226

COSINE-100Collaboration, N. Carlin et al.,COSINE-100 Full Dataset Challenges the Annual Modulation Signal of DAMA/LIBRA, arXiv:2409.13226

arXiv

[3] [7]

TUBE O.D, NON-ROTATABLE S/S 304L 8 7 CONFLAT HALF NIPPLE, N3 1N-600, 6

BOTTOM TORI. HEAD STIFFENING RING TO BE STITCH WELDED BUT WITH 200mm CONTINOUS WELDING AS IT APPROACHES THE LEGS 0 ISSUED FOR CONSTRUCTION DH JBL - 24/01/2018 REV DETAILS DRN CHK APP DATE 24/01/2018 13:16:51 INSIDE 2600 O.D 6 THK. W1 SHELL LONG. WELD 2576 O/S HEADS (356) 76 S.F 1500 W1 W1 60° 2983 3132 1 2 1 6 5 4 3 N1 N2N3 1600 520 30° TYP. 0° 90° 180°...

work page 2018

[4] [8]

FLANGE BOLT HOLES TO STRADDLE NATURAL CENTERLINES UNO

work page

[5] [9]

ALL NOZZLES TO BE PROTECTED WITH WOODEN BLANKS AND SECURED WITH AT LEAST 2 BOLTS DURING TRANSPORTATION

work page

[6] [10]

AND LONG

ALL CIRC. AND LONG. WELDS TO BE FULL PENETRATION BUTT WELDS

work page

[7] [12]

LOW RADIOACTIVE PLATES AND SPECIFIC CLEANLINESS PER UoM REQUIREMENTS

work page

[8] [13]

PAD AND LIFTING LUG WELDS

100% SURFACE INSPECTION FOR ALL COMP. PAD AND LIFTING LUG WELDS

work page