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Darkside-50, DarkSide-20k and the Global Collaboration to reach the Neutrino Floor with liquid argon
Cristiano Galbiati Gran Sasso Science Institute and Princeton University
The quest for dark matter with liquid argon APC Université Paris Diderot
September 4, 2018
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2−10 1−10 1 10 210]2 [TeV/cχM
50−10
49−10
48−10
47−10
46−10
45−10
44−10
43−10
42−10
41−10]2
[cm
SI
σDark Matter-Nucleon
proj.
yrt
DarkSide
-20k 100 proj
.yrt
DarkSide
-20k 200
proj.
yrt
Future 3
00-tonne
GADMC D
etector
1k
DEAP-360
0 proj.
LUX 2017
LZ proj.
PANDAX-I
I 2017
XENON1T
2018
XENONnT
proj.
WARP 200
7
DarkSide
-50 2015
DEAP-360
0 2017
proj.
yrt
Future 3
00-tonne
GADMC d
etector
3k
DarkSide
-50 2018
Neutrino
floor o
n xenon
100 t×yr
101 t×yr
102 t×yr
103 t×yrLHC
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1 10]2 [GeV/cχM
46−10
45−10
44−10
43−10
42−10
41−10
40−10
39−10
38−10]2
[cm
SI
σ90% CL upper limit on
DarkSide-LMDarkSide-50 2018NEWS-G 2018 LUX 2017XENON1T 2017 PICO-60 2017PICASSO 2017 CDMSLite 2017CRESST-III 2017 PandaX-II 2016XENON100 2016 DAMIC 2016CDEX 2016 CRESST-II 2015SuperCDMS 2014 CDMSlite 2014COGENT 2013 CDMS 2013CRESST 2012 DAMA/LIBRA 2008Neutrino Floor
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3−10 2−10 1−10 1 10 210]2 [TeV/cχM
50−10
49−10
48−10
47−10
46−10
45−10
44−10
43−10
42−10
41−10
40−10
39−10
38−10
37−10]2
[cm
SI
σDark Matter-Nucleon
ATLAS Dijet 2018
ATLAS Dilepton 2018
+ X 2018TmissATLAS E
DarkSide-50 2018
CRESST-III 2017
proj.yrt
DarkSide-2
0k 100
proj.yrt
DarkSide-2
0k 200
proj.yrt
Future 300
-tonne GAD
MC Detecto
r 1k
DEAP-3600
proj.LUX 2
017
LZ proj.
PANDAX-II
2017
XENON1T 20
18
XENONnT pr
oj.
proj.yrt
Future 300
-tonne GAD
MC detecto
r 3k
DarkSide-5
0 2018
DarkSide-LM proj.
Neutrino floor on xenon
direct detection limits at 90% CLATLAS limits at 95% CL
=1DM
=0.01, gl
=0.1, gqgVector mediator, Dirac DM
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PandaX-xT
�5
▪ Intermediatestage:▫ PandaX-4T(4-tontarget)withSIsensitivity~10-47cm2▫ On-siteassemblyandcommissioning:2019-2020
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TheCathodeHigh-VoltageFeedthrough
TheOuterDetectorPMTs(120)
Dual phase xenon TPC, 7 tonnes fully active
LXeHeatExchanger
ExistingWaterTank,and
SURFInfrastructure
Gadolinium-LoadedLiquidScintillatorVeto
InstrumentationConduits
D-Dneutrontube
The LUX-ZEPLIN detector
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Radon dominates ER backgrounds
Gamma backgrounds (PMTs, cryostat) are negligible.
pp solar neutrinos, elastic scattering on atomic electrons
Coherent neutrino scattering on xenon nuclei
LZ backgrounds summary5.6 tonnes, 1000 days
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The phases of the XENON Program
8
M. Schumann (AEC Bern) – XENON 8
XENON1T
96cm
● 3.5 t liquid xenon in total● 2.0t active target● ~1t after fiducialization
● 248+6 PMTs
XENON10 XENON100 XENON1T XENONnT
2005-2007 2008-2016 2012-2018 2019-2023
25 kg- 15cm drift 161 kg- 30 cm drift 3200 kg- 100 cm drift
8000 kg-150 cm drift
~10-43 cm2 ~10-45 cm2 ~10-47 cm2 ~10-48 cm2
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XENON1T and XENONnT science reach
• XENON1T: 1.6 x 10-47 cm2 with an exposure of 2 tonnes x year
• XENONnT: to start in mid 2019, aiming for 20 tonnes x year exposure
]2
WIMP mass [GeV/c
7 10 20 30 100 200 1000 2000 10000
]2
[c
mσ
WIM
P-n
ucle
on
49−10
48−10
47−10
46−10
45−10
44−10
43−10
PandaX-II (2
017)
LUX (2017)
XENON100 (2016)
y)⋅
XENON1T (0.1 t y)⋅
XENON1T (2 t
y)⋅
XENONnT (20 t
Billard 2013, N
eutrino Disc
overy Limit
Bagnaschi 2016
�9
XENON1T
XENON1T First Result
XENONnTLZ
2016 2018 2020 2022 202410-48
10-47
10-46
10-45
10-44
Calendar Year
Crosssection @ 50GeV [cm2]
Apr2020
Aug2019
Aug2018
Figure 2: A comparison, as function of calendar year, of the projected sensitivity to spin-independent WIMP-nucleon interactions for a 50GeV/c2 WIMP for XENON1T (1 ton fiducialmass), XENONnT (4 ton fiducial mass), and LZ (5.6 ton fiducial mass). Curves in this plot havebeen calculated using the o�cial values that each experiment has estimated for WIMP energyrange, NR acceptance, ER rejection and background. See text for comments on the comparisonof the various curves.
XENON1T XENONnT LZ
Fiducial Volume [tons] 1 4 5.6Livetime Fraction 80% 80% 80%WIMP Energy
4-50 4-50 6-30Range [keVnr]NR Acceptance 40% 40% 50%ER Rejection 99.75% 99.75% 99.5%Bkg rate [evt/year] 2.08 1.15 2.35
Table 1: Assumptions for the projected sensitivity to spin-independent interaction shown inFigure 2. The background rate is defined as the rate of NR and ER falling into the definedWIMP search box, after having accounted for acceptance and rejection, respectively. Numbersfor LZ are the “goal” values extracted from Reference [J.Dobson, 2016].
6
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XENON1T Presentation at LNGS on May 28 2018
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0 50 100 150 200 250 300 350 400 450 500S1 [PE]
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Expected number of background events0 2 4 6 8 10
Number of WIMP-like events needed
0
10
20
30
40
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100% Background Model Errors
10% Background Model Errors
1% Background Model Errors
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“Zero Background” condition (<0.1 background events)
necessary to conduct discovery program
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]2WIMP mass [TeV/c
2−10 1−10 1 10
]2 [cm
SI
σWIMP-nucleon
50−10
49−10
48−10
47−10
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45−10
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DarkSide-20k
(100 t yr p
roj.)
DarkSide-20k
(200 t yr p
roj.)
Future 300-t
onne GADMC D
etector (100
0 t yr proj.
)
DEAP-3600 (p
roj.)
LUX (2017)
LZ (proj.)
PANDAX-II
(2017)
XENON1T (2
017)
XENON1T (p
roj.)
XENONnT (p
roj.)
WARP (2007)
DarkSide-5
0 (2015)
DEAP-3600 (2
017)
Neutrino f
loor on xe
nonFuture
300-tonne G
ADMC detecto
r (3000 t yr
proj.)
The Global Argon Dark Matter CollaborationArDM DarkSide DEAP MiniCLEAN
}A Single Global Program for Direct Dark Matter Searches Currently taking data: ArDM, DarkSide-50, DEAP-3600 Next step: DarkSide-20k at LNGS (2021-)Last Step: 300 tonnes detector, location t.b.d (2027-)
DarkSide-20k approved by INFN and LNGS in April 2017 and by NSF in Oct 2017 Officially supported by LNGS, LSC, and SNOLab 30 tonnes (20 tonnes fiducial) of low-radioactivity underground argon 14 m2 of SiPM coverage
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Questionnaire for Requestingthe Status of Recognized Experiment at CERN
The DarkSide Collaboration &The Global Argon Dark Matter Collaboration
October 24, 2017
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Letter of Intent September 8, 2017
Rev B
Scientists at LNGS, LSC, and SNOLAB are joining in an international effort to mount a
phased argon dark matter program with the goal of being sensitive to the neutrino floor. This effort will include a broad collaboration of scientists and will represent the global community for dark matter searches with argon. This letter is an update of a previous communication dating June 2017, which detailed the first conception of the program; this letter was expanded to capture the intent of all institutions and scientists participating in the program.
In this document, the undersigned representatives of groups working on argon dark matter searches, including Brazilian, Canadian, Chinese, French, German, Greek, Italian, Mexican, Polish, Romanian, Russian, Spanish, Swiss, US, and UK groups among others, memorialize their intent to form a Global Argon Dark Matter Collaboration to carry out a program for direct dark matter searches, consisting of two main elements.
The first element of the program is the DarkSide-20k experiment at LNGS, whose science goal is to perform a dark matter search with an exposure of 100 tonne·yr of low-radioactivity underground argon (the low intrinsic background, free from any background other than that induced by atmospheric neutrinos, may also permit a 200 tonne·yr exposure for extended operation). This detector will be competitive with next generation liquid xenon dark matter searches at high WIMPs masses and will be built in time to start data taking by 2021.
The second element of the program is a low-radioactivity underground argon detector with a fiducial mass of a few hundred tonnes. The science goal is to perform a dark matter search with an exposure of 1,000 tonne·yr with sensitivity reaching to the neutrino floor, to identify coherent nuclear scattering of atmospheric neutrinos, and to perform a high-precision measurement of intermediate energy solar neutrinos (pep, CNO, low energy 8B). All groups have agreed to the continuing collaboration towards the development of a depleted argon detector at the scale of a few hundred tonnes, working together to select a design and site based on technical and scientific requirements. Decisions on technical design will be informed by data collected with the precursor DEAP and DarkSide detectors. The groups will also develop low radioactivity argon to allow for the multi-hundred tonne detector.
The proposal to build DarkSide-20k, submitted to the Italian INFN and to LNGS, reviewed well, and INFN and LNGS approved the DarkSide-20k experiment in April 2017. The scope of the INFN contributions is €40M. The proposal submitted to the US NSF reviewed well, and the collaboration is now awaiting the approval decision by the US NSF. The capital funding for DarkSide-20k under discussion with the US NSF is $13M.
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Deepundergroundlaboratorysupportforglobalcollaborationtowardsdiscoveryofdarkmatterutilisingliquidargondetectors.Towhomitmayconcern;As hosts of the existing operational liquid argon direct dark matter detectors,and asproponentsandsupportersoftheUnderground-GRIinitiative,theLNGS,SNOLABandLSCdeepundergroundresearchfacilitiesarepleasedtorecognizethecollaborativedevelopmentswithinthegloballiquidargondarkmattercommunity.TheDarkSideprojectatLNGS,theDEAPprojectatSNOLABandtheArDMprojectatLSCarealldevelopingnewtechnologiesandcapabilitiestosearchforWIMPdarkmatter,andarebeginningtocoalesceintoonecollaborationtodevelopfuture, larger generations of liquid argon direct dark matter detectors. We encourage andsupport the development of this global community, with a focus on the development ofDarkSide-20katLNGSinthefirstinstance,andalargerdetectoratalocationtobedeterminedfromscientific requirements, in the future.Usingavailableassayand research infrastructure,thethreedeepundergroundresearchfacilitieswill support theactivitiesanddevelopmentofthevariousgenerationsofliquidargondetectors.
Stefano Ragazzi Director, LNGS
Aldo Ianni Director, LSC Nigel J.T. Smith
Director, SNOLAB
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DarkSide-20k20-tonnes fiducial dark matter detectorstart of operations at LNGS within 2021
100 tonne×year background-free search for dark matter
Future 300-tonne Detector300-tonnes depleted argon detector
start of operations within 20261,000 tonne×year background-free search for dark matter
precision measurement of solar neutrinos
20- 15 16 17 18 19 20 21 22 23 24 25 26 27 28 29 30 31 32 33 34
DS-20k
300k
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Urania to Aria to LNGS
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• Volatilità relative => 1.007
• Valori tipici >1.5
• Numero di stadi teorici => ordine delle migliaia
• HETP = 10 cm
• H=200-400 m
• Usuali = 20-30 m
• Fuori terra
• A sezioni separate
325
m
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Liquid Argon TPC 153 kg 39Ar-Depleted Underground Argon
Target
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4 m Diameter 30 Tonnes
Liquid Scintillator Neutron Veto
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10 m Height 11 m Diameter 1,000 Tonnes
Water Cherenkov Muon Veto
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Liquid Argon TPC 153 kg 39Ar-Depleted Underground Argon
Target
4 m Diameter 30 Tonnes
Liquid Scintillator Neutron Veto
10 m Height 11 m Diameter 1,000 Tonnes
Water Cherenkov Muon Veto
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DarkSide-50• P. Agnes et al. (The DarkSide Collaboration), “DarkSide-50 532-day Dark Matter Search with Low-Radioactivity Argon”, arxiv:1802.07198.
• P. Agnes et al. (The DarkSide Collaboration), “Constraints on Sub-GeV Dark Matter-Electron Scattering from the DarkSide-50 Experiment”, arxiv:1802.06998.
• P. Agnes et al. (The DarkSide Collaboration), “Low-mass Dark Matter Search with the DarkSide-50 Experiment”, arxiv:1802.06994.
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+min S2/S1
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0 50 100 150 200 250 300 350 400 450 500S1 [PE]
0
0.1
0.2
0.3
0.4
0.5
0.6
0.7
0.8
0.9
190
fEntries 548087
Integral 5.34e+05
0
0.2
0.4
0.6
0.8
1
310×Entries 548087
Integral 5.34e+05
+max S2/S1
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0 50 100 150 200 250 300 350 400 450 500S1 [PE]
0
0.1
0.2
0.3
0.4
0.5
0.6
0.7
0.8
0.9
190
fEntries 547837
Integral 5.338e+05
0
0.2
0.4
0.6
0.8
1
310×Entries 547837
Integral 5.338e+05
+S2 i90/i1
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0 50 100 150 200 250 300 350 400 450 500S1 [PE]
0
0.1
0.2
0.3
0.4
0.5
0.6
0.7
0.8
0.9
190
fEntries 545966
Integral 5.319e+05
0
0.2
0.4
0.6
0.8
1
310×Entries 545966
Integral 5.319e+05
+S1 TBA
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0 50 100 150 200 250 300 350 400 450 500S1 [PE]
0
0.1
0.2
0.3
0.4
0.5
0.6
0.7
0.8
0.9
190
fEntries 543779
Integral 5.297e+05
0
0.2
0.4
0.6
0.8
1
310×Entries 543779
Integral 5.297e+05
+TPB Tail
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0 50 100 150 200 250 300 350 400 450 500S1 [PE]
0
0.1
0.2
0.3
0.4
0.5
0.6
0.7
0.8
0.9
190
fEntries 540450
Integral 5.266e+05
0
0.2
0.4
0.6
0.8
1
310×Entries 540450
Integral 5.266e+05
+NLL
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0 50 100 150 200 250 300 350 400 450 500S1 [PE]
0
0.1
0.2
0.3
0.4
0.5
0.6
0.7
0.8
0.9
190
fEntries 361687
Integral 3.576e+05
0
100
200
300
400
500
600
700
800Entries 361687
Integral 3.576e+05
+R 2
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0 50 100 150 200 250 300 350 400 450 500S1 [PE]
0
0.1
0.2
0.3
0.4
0.5
0.6
0.7
0.8
0.9
190
fEntries 227934
Integral 2.258e+05
0
100
200
300
400
500Entries 227934
Integral 2.258e+05
+Veto
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0 50 100 150 200 250 300 350 400 450 500S1 [PE]
0
0.1
0.2
0.3
0.4
0.5
0.6
0.7
0.8
0.9
190
fEntries 16213
Integral 1.619e+04
0
10
20
30
40
50
60
70Entries 16213
Integral 1.619e+04
14+r<10 cm && 50% loss S2/S1 cut (70d)
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3−10 2−10 1−10 1 10 210]2 [TeV/cχM
50−10
49−10
48−10
47−10
46−10
45−10
44−10
43−10
42−10
41−10
40−10
39−10
38−10
37−10]2
[cm
SI
σDark Matter-Nucleon
ATLAS Dijet 2018
ATLAS Dilepton 2018
+ X 2018TmissATLAS E
DarkSide-50 2018
CRESST-III 2017
proj.yrt
DarkSide-2
0k 100
proj.yrt
DarkSide-2
0k 200
proj.yrt
Future 300
-tonne GAD
MC Detecto
r 1k
DEAP-3600
proj.LUX 2
017
LZ proj.
PANDAX-II
2017
XENON1T 20
18
XENONnT pr
oj.
proj.yrt
Future 300
-tonne GAD
MC detecto
r 3k
DarkSide-5
0 2018
DarkSide-LM proj.
Neutrino floor on xenon
direct detection limits at 90% CLATLAS limits at 95% CL
=1DM
=0.01, gl
=0.1, gqgVector mediator, Dirac DM
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The DarkSide Strategy
• Background-free through the neutrino limit
• Neutrino limit reached with detector of few hundred tonnes located very deep underground
• Complementary science: solar neutrinos
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Energy [MeV]1−10×6 1 2 3 4
yr]
× 400 tonne
×Events / [10 keV
1
10
210
310MC Data
AllνBe-7
νCNO-
νpep-νB-8
P32
Radon
Other Cosmogenics
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Bq / 100 tonne]µRadon Activity [ 10 20 30 40 50 60 70 80 210 210×2
Uncertainty [%]
0
5
10
15
20
25
30CNO (HZ)
pep (HZ)
Be (HZ)7
CNO (LZ)
pep (LZ)
Be (LZ)7
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Ionization-Only (S2-Only) Signals1. The PMTs have zero dark rate at 88 K so a signal is always real
2. The gain in the gas region (~70 PE/e-, reduced to 23 PE/e- when accounting for the 30% QE of the PMTs) means that we are sensitive to a single extracted electron
3. The radioactivity rate in the detector is remarkably low, so …
4. We don’t need PSD
5. The electron yield for nuclear recoils rises at low energy
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0 10 20 30 40 50 60 70 80 90S2 [PE]
0.05
0.1
0.15
0.2
0.25
0.3
0.35
0.4
0.45
0.5Acceptance
Fiducialization
Trigger efficiency×
<0.15)90
S2 Identification (f×
arxiv:1802.06994
4 e-100 eVeeAnalysis Threshold
0.4 e-10 eVee
10% Detector Threshold
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0 0.5 1 1.5 2 2.5 3-eN
2−10
1−10
1
10
210
day]
×
kg
×
- eN
[0.05
/
Events PE
S2=30
Center PMT DS-50 DATAGetter OffGetter OnFit
-1 Ext. e's-2 Ext. e
arxiv:1802.06994
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0 20 40 60 80 100-eN
3−10
2−10
1−10
1
10
210
310 day]
× kg
×
- eEvents / [0.5 N
First 100 days
Last 500 days
d)(500Single S2
d)(500S1 + S2
0 50 100-eN
0
0.2
0.4
0.6
day]
× kg
× - e
[N
/ Events
0.01 ± 0.11 = Ratio BR L/K
arxiv:1802.06994
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10 20 30 40 50 60 70 80 90 100-eN
0
100
200
300
400
500
600
700
800
900- e
Events / N
AmBe Data241
G4DS Fit
Single S2
S1 + S2
arxiv:1802.06994
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10 20 30 40 50 60 70 80 90 100-eN
0
10
20
30
40
50
60
70
80
90
100- e
Events / N
C Data13Am241
G4DS Fit
Single S2
S1 + S2
γC 13Am241
arxiv:1802.06994
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3−10 2−10 1−10 1 ε
0
1
2
3
4
5
6
7
8
9
10]
nr
/keV
- [e
yQ
Xe Data
LUX 2016
ZEPLIN-III 2011
XENON10 2011
Manzur et al. 2010
XENON10 2009
Aprile et al. 2006
1 10 210 310] nr [keVXeE
2−10 1−10 1 10 210] nr [keVArE
Ar Data
ARIS
SCENE
AmBe - AmC - ARIS - SCENE
Joshi et al. 2014
Joshi et al. 2014 Cross Calibrated
Xe Model
Bezrukov et al. 2011
arxiv:1802.06994
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0 0.5 1 1.5 2 2.5 3310×
Energy [keV]
1
10
210
310
410
510
Events / [2 keV]
Th232 Cryo
K40 Co60
lowU238upU238
U235 Kr85
Ar39 DATA
arxiv:1802.07198
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0 5 10 15 20 25 30 35 40 45 50-eN
3−10
2−10
1−10
1
10
210 day]
× kg
×
- eEvents / [N
Data
G4DS MC All
-rays γCryostat
-rays γPMTs
Kr 85Ar + 39
2 cm-40=10χσDM spectra
2=2.5 GeV/cχM
2=5.0 GeV/cχM
2=10.0 GeV/cχM
1 2 3 4 5 6 7 8 9 10 11 12131415] nrE [keV
1 2 3] eeE [keV
1−10
1
10
210
310
day]
× kg
×
ee
Events / [keV
2−10
1−10
1
10
210
day]
× kg
×
nr
Events / [keV
arxiv:1802.06994
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1−10×5 1 2 3 4 5 6 7 8 9 10]2 [GeV/cχM
45−10
44−10
43−10
42−10
41−10
40−10
39−10
38−10]2
[cm
SI
σDark Matter-Nucleon
DarkSide-50 BinomialDarkSide-50 No Quenching Fluctuation NEWS-G 2018 LUX 2017XENON1T 2017 PICO-60 2017PICASSO 2017 CDMSLite 2017CRESST-III 2017 PandaX-II 2016XENON100 2016 DAMIC 2016CDEX 2016 CRESST-II 2015SuperCDMS 2014 CDMSlite 2014COGENT 2013 CDMS 2013CRESST 2012 DAMA/LIBRA 2008Neutrino Floor
arxiv:1802.06994
No Quenching
Fluctuations
0.6 keVnr Threshold
Binomial
Fluctuations
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0 5 10 15 20 25 30-eN
3−10
2−10
1−10
1
10
210 day]
× kg
×
- eEvents / [N
Data
G4DS MC All
-rays γCryostat
-rays γPMTs
Kr 85Ar + 39
2 cm-36=10χσDM spectra
2=10 MeV/cχM
2=100 MeV/cχM
2=1000 MeV/cχM
0.2 0.4 0.6 0.8 1 1.2] eeE [keV
arxiv:1802.01427
arxiv:1802.06998
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10 210 310 [MeV]χM
39−10
38−10
37−10
36−10]2
[cm
eσDark Matter-Electron
=1DMFDarkSide-50XENON100XENON10
arxiv:1802.06998
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Drift electric field [V/cm]0 200 400 600 800 1000
S1 yield relative to 0 field
0.7
0.75
0.8
0.85
0.9
0.95
1
1.05
1.1
1.15 57.2 keV
dεParallel to
dεPerpendicular to
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ProductionandPurification
Renshaw,PNNLLRUAWorkshop20184
Preliminary lay-out
a^erPOLARISSrl
Production:Urania• Commercial-scaleplanttoextractUAr• LocatedinSouthwesternColorado
• UAr extractedfromCO2 wellgasatthetonne scaleFocusofthistalk Purification:Aria
(seeM.Simeone’s talkfordetails)• 350mtallcryogenicdistillationcolumntopurifyUAr and
isotopicallyseparateargonandotherelements• LocatedinrefurbishedcarbonmineshaftinSardinia,Italy• WillchemicallypurifytheUAr forDS-20ktodetectorgrade
UAr transportedviaboatforfinalpurificationatAria
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Renshaw,PNNLLRUAWorkshop201810
EntertheAgeofUrania
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• Volatilità relative => 1.007
• Valori tipici >1.5
• Numero di stadi teorici => ordine delle migliaia
• HETP = 10 cm
• H=200-400 m
• Usuali = 20-30 m
• Fuori terra
• A sezioni separate
325
m
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Tile
FEBs
Top View
Side View Side View
3D View
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Amplitude [Arb.Units]0 50 100 150 200 250 300
Entries
0
200
400
600
800
1000
1200
Gain: 52.68: 2.19bσ
SNR: 24.1
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The End