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DarkSideCristiano Galbiati
Gran Sasso Science Institute and Princeton University XLI LNGS Scientific Committee Meeting
LNGS March 26, 2018
“Zero Background” condition (<0.1 background events)
necessary to conduct discovery program
0 50 100 150 200 250 300 350 400 450 500S1 [PE]
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fEntries 361687
Integral 3.576e+05
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800Entries 361687
Integral 3.576e+05
+R 2
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fEntries 227934
Integral 2.258e+05
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Integral 2.258e+05
+Veto
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fEntries 16213
Integral 1.619e+04
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Integral 1.619e+04
14+r<10 cm && 50% loss S2/S1 cut (70d)
]2WIMP mass [TeV/c
2−10 1−10 1 10
]2 [cm
SI
σWIMP-nucleon
50−10
49−10
48−10
47−10
46−10
45−10
44−10
43−10
42−10
41−10
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.)
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
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
10 20 30 40 50 60 70 80 90 100-eN
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100- e
Events / N
C Data13Am241
G4DS Fit
Single S2
S1 + S2
γC 13Am241
arxiv:1802.06994
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
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
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
DarkSide-20k• Scientific and technical motivation stronger than ever
• Approved by INFN Apr 2017 and by NSF Oct 2017
• Received request by LNGS to drop consideration of liquid scintillator veto Sep 2017
• Experiment re-designed to eliminate liquid scintillator and water buffers in favor of large atmospheric liquid argon veto and plastic scintillator veto
• DarkSide Resources Board installed: Marcello Giorgi (Chair), Ed Hungerford, and Art McDonald
• Darkside Review Committee installed: MOU on its way
• NOA spending started, Aria under construction, Urania tender soon to be released
Amplitude [Arb.Units]0 50 100 150 200 250 300
Entries
0
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1200
Gain: 52.68: 2.19bσ
SNR: 24.1
The End
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