Carla Bonifazi

Coherent elastic neutrino-nucleus

scattering

Carla Bonifazi

ICAS-ICIFI-UNSAM CONICET

1

[email protected]

What is CE 𝜈 NS?

Coherent Elastic

Neutrino-Nucleus Scattering

is a process in which neutrinos scatter off a nucleus acting as a single particle

A

A

A

A

2

What is CE 𝜈 NS?

Coherent Elastic

Neutrino-Nucleus Scattering

is a process in which neutrinos scatter off a nucleus acting as a single particle

Predicted in 1974 by Freedman

Measurement for the first in 2017 by COHERENT Dominant process for E

≲ 50 eV

Cross section increase with N

D. Freedman, Phys.Rev. D 9 1389 (1974)

A

A

A

A

3

What is CE 𝜈 NS?

Coherent Elastic

Neutrino-Nucleus Scattering

is a process in which neutrinos scatter off a nucleus acting as a single particle

Predicted in 1974 by Freedman

Measurement for the first time in 2017 by COHERENT Dominant process for E

≲ 50 eV

Cross section increase with N

D. Akimov et al, Science 357 (2017)

A

A

A

A D. Freedman, Phys.Rev. D 9 1389 (1974)

4

What is CE 𝜈 NS?

Coherent Elastic

Neutrino-Nucleus Scattering

is a process in which neutrinos scatter on a nucleus acting as a single particle

Predicted in 1974 by Freedman

Measurement for the first time in 2017 by COHERENT Dominant process for E

≲ 50 MeV

Cross section increase with N

keV MeV GeV TeV PeV

CE 𝜈 NS

Interaction with nuclei and

electrons, minimally

disruptive of the nucleus

Interaction with nucleons inside nuclei, often disruptive, hadroproduction

Deep Inelastic Scattering

A

A

A

A

D. Akimov et al, Science 357 (2017) D. Freedman, Phys.Rev. D 9 1389 (1974)

5

What is CE 𝜈 NS?

Coherent Elastic

Neutrino-Nucleus Scattering

is a process in which neutrinos scatter on a nucleus acting as a single particle

Predicted in 1974 by Freedman

Measurement for the first time in 2017 by COHERENT Dominant process for E

≲ 50 MeV

Cross section increases with N

GF = Fermi coupling constant

Z = atomic number of the nucleus N = neutron number of the nucleus

E𝜈 = neutrino energy 𝜃^w = weak mixing angle Qw = weak charge

sin² ✓_W ⇠ 1

4(⇡ 0.22)

for:

A

A

A

A

For:

q<latexit sha1_base64="b80ZNm6R6CpiMo3uNvPvuvELkMA=">AAAB9XicbVA9SwNBEJ3zM8avqKXNYhCswl0UtEgRtLGMYj4gOcPe3iZZsrd77u4p4cj/sLFQxNb/Yue/cZNcoYkPBh7vzTAzL4g508Z1v52l5ZXVtfXcRn5za3tnt7C339AyUYTWieRStQKsKWeC1g0znLZiRXEUcNoMhlcTv/lIlWZS3JlRTP0I9wXrMYKNle4fUIeE0qBbVKkgr1souiV3CrRIvIwUIUOtW/jqhJIkERWGcKx123Nj46dYGUY4Hec7iaYxJkPcp21LBY6o9tPp1WN0bJUQ9aSyJQyaqr8nUhxpPYoC2xlhM9Dz3kT8z2snpnfhp0zEiaGCzBb1Eo6MRJMIUMgUJYaPLMFEMXsrIgOsMDE2qLwNwZt/eZE0yiXvtFS+OStWL7M4cnAIR3ACHpxDFa6hBnUgoOAZXuHNeXJenHfnY9a65GQzB/AHzucPKnSQ/A==</latexit> · R << 1

q = three-momentum transfer R = nuclear radius

d _SM

dE_R (E_⌫¯e) = G²_F

8⇡ Q²_W

"

2 2E_R

E_⌫¯e +

✓ E_R E_⌫¯e

◆2

M E_R E_⌫¯²_e

#

M |F (q)|²

<latexit sha1_base64="rzy6ZDia1tnxh8P750k9JMKl4Ds=">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</latexit>

Q<latexit sha1_base64="1ewqpBjddpK9biqUcyD9OZ4Tvyc=">AAACCnicbVC7SgNBFJ2NrxhfUUub0SDEImE3BrQRgjZWkoB5YDYus5NJMmR2dpm5K4SQ2sZfsbFQxNYvsPNvnDwKTTxw4XDOvdx7jx8JrsG2v63E0vLK6lpyPbWxubW9k97dq+kwVpRVaShC1fCJZoJLVgUOgjUixUjgC1b3+1djv/7AlOahvIVBxFoB6Ure4ZSAkbz0YcWr4wt8g3M46+BcEbuay/uCCz0GxKuf3LleOmPn7QnwInFmJINmKHvpL7cd0jhgEqggWjcdO4LWkCjgVLBRyo01iwjtky5rGipJwHRrOHllhI+N0sadUJmSgCfq74khCbQeBL7pDAj09Lw3Fv/zmjF0zltDLqMYmKTTRZ1YYAjxOBfc5opREANDCFXc3IppjyhCwaSXMiE48y8vkloh75zmC5VipnQ5iyOJDtARyiIHnaESukZlVEUUPaJn9IrerCfrxXq3PqatCWs2s4/+wPr8ASp9l28=</latexit> _W = N (1 4 sin² ✓_W )Z

F(q) = form factor

M = mass of the nucleus

q = p

2M E

<latexit sha1_base64="Wx0Q+5+lKV5Ep62fvffjEAw0vqc=">AAAB+nicdVDLSsNAFJ34rPWV6tLNYBFchaQKuhGKIrgRKtgHtCFMppN26OTRmRulxH6KGxeKuPVL3Pk3TtoKPg9c7uGce5k7x08EV2Db78bc/MLi0nJhpbi6tr6xaZa2GipOJWV1GotYtnyimOARqwMHwVqJZCT0BWv6g7Pcb94wqXgcXcMoYW5IehEPOCWgJc8sDfEJ7qihhKyCL889OfbMsm1V7Bz4N3GsSbfLaIaaZ751ujFNQxYBFUSptmMn4GZEAqeCjYudVLGE0AHpsbamEQmZcrPJ6WO8p5UuDmKpKwI8Ub9uZCRUahT6ejIk0Fc/vVz8y2unEBy7GY+SFFhEpw8FqcAQ4zwH3OWSURAjTQiVXN+KaZ9IQkGnVdQhfP4U/08aFcs5sCpXh+Xq6SyOAtpBu2gfOegIVdEFqqE6ougW3aNH9GTcGQ/Gs/EyHZ0zZjvb6BuM1w/mQJMg</latexit>

D. Akimov et al, Science 357 (2017) D. Freedman, Phys.Rev. D 9 1389 (1974)

6

What is CE 𝜈 NS?

Coherent Elastic

Neutrino-Nucleus Scattering

is a process in which neutrinos scatter on a nucleus acting as a single particle

Predicted in 1974 by Freedman

Measurement for the first time in 2017 by COHERENT Dominant process for E

≲ 50 MeV

Cross section increases with N

Raimund Strauss – Magnificent CEvNS 2018

A

A

A

A

SM

⇠ G

4⇡ N

E

<latexit sha1_base64="gl4FNuTpDDKlQshgAaMT2k8hL0A=">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</latexit>

D. Akimov et al, Science 357 (2017) D. Freedman, Phys.Rev. D 9 1389 (1974)

7

What is CE 𝜈 NS?

Coherent Elastic

Neutrino-Nucleus Scattering

is a process in which neutrinos scatter on a nucleus acting as a single particle

A

A

A

A

Large cross section...

...but hard to observe due to tiny nuclear recoil energies:

0

< E

>= 2 3

(E

/MeV)

A keV

Energies below the typical detection threshold of conventional neutrino experiments

Now low threshold and background detectors available thanks to the efforts done for dark matter experiments.

deposited energy 8

Why CE 𝜈 NS?

Background for DM experiments

https://doi.org/10.1016/j.dark.2014.10.005 Phys. Rev. D 89, 023524 (2014)

Solar

Neutrinos

Supernova Neutrinos

Atmospheric Neutrinos

9

What is

CE 𝜈 NS good for?

Fundamental neutrino interactions

Precision test of SM

‣ cross section measurements

‣ Weinberg angle

arXiv: 1407.7524; arXiv: 2007.15688 arXiv:2102.06153; arXiv:2108.07310

10

What is

CE 𝜈 NS good for?

Fundamental neutrino interactions

Precision test of SM

‣ cross section measurements

‣ Weinberg angle

Beyond SM physics

‣ neutrino non-standard interactions (NSI)

‣ neutrino electromagnetic properties

‣ light mediators

‣ axion-like particles

‣ light sterile neutrinos

‣ dark matter

arXiv: 1407.7524; arXiv: 2007.15688 arXiv:2102.06153; arXiv:2108.07310

arXiv:1708.02899; arXiv:1708.04255; arXiv:1812.02778; arXiv:1911.09831

arXiv:1910.04951; arXiv:1804.03660; arXiv:2008.05022 arXiv:1912.05733

arXiv:1201.3805; arXiv:151102834; arXiv:1708.09518 arXiv:1403.6344

arXiv:1711.04531; arXiv: 1710.10889 Panel Neutrino 6 – #47, #144 & #230

11

Fundamental neutrino interactions

Precision test of SM Beyond SM physics

Nuclear physics

Nuclear form factor

‣ form factor suppresses cross section at large three momentum transfer

‣ very well known, < ~5% uncertainty on event rate Neutron distribution radius (Rn)

Cadeddu et al., PRD 101, 033004 (2020)

What is

CE 𝜈 NS good for?

12

Fundamental neutrino interactions

Precision test of SM Beyond SM physics

Nuclear physics

Nuclear form factor

Neutron distribution radius (Rn)

Supernova neutrino

Energy transport in supernovae: all neutrinos flavors with E ~ tens-of-MeV

To detect SN neutrinos (tonne-scale DM detectors)

What is

CE 𝜈 NS good for?

Lang et al PRD 94, 10 (2016) 103009

13

Fundamental neutrino interactions

Precision test of SM Beyond SM physics

Nuclear physics

Nuclear form factor

Neutron distribution radius (Rn)

Supernova neutrino

Energy transport in supernovae: all neutrinos flavors with E ~ tens-of-MeV

To detect SN neutrinos (tonne-scale DM detectors)

Reactor physics

Reactor monitoring

Application for non-proliferation

What is

CE 𝜈 NS good for?

14

A. Bernstein, et al Rev. Mod. Phys. 92 (2020) no.1, 011003

for CE 𝜈 NS

Neutrino Sources

Requirements:

High flux

Neutrino production well understood Low background rates

Multiple flavors etc

15

for CE 𝜈 NS

Requirements:

High flux

Neutrino production well understood Low background rates

Multiple flavors etc

Neutrino Sources

Pion-decay-at-rest neutrino source:

neutrinos are produced from the decay of pions and muons

intermediate neutrino energies (~ 30 MeV) slightly incoherent

pulsed beam for background rejection

‣Stopped-pion beams

16

for CE 𝜈 NS

Neutrino Sources

‣Nuclear reactors

Neutrinos are produced in beta decays of fission fragments

high flux ~ 10

𝜈 /s (power reactors)

Intense @ MeV energies (up to 10 MeV)

Clean in background, active and passive shielding Requirements:

High flux

Neutrino production well understood Low background rates

Multiple flavors etc

17

Experiments

Coherent CAPTAIN-Mills (CCM)

LANSCE Lujan

Nuclear reactors

Stopped-pion beams

2023

vIOLETA

GaNESS

Future/Planned

PPC-Ge

@ Dresden-II

18

Stopped-

pion beam experiments

COHERENT Experiment – SNS

Spallation Neutron Source – 1 GeV proton beam Pion-decay-at-rest neutrino source

prompt monochromatic ~ 30 MeV

Pulsed beam @ 60Hz for background rejection (factor ~ 10⁴) Multi-target program to measure N² dependence

19

Stopped-

pion beam experiments

COHERENT CsI

‣ 2017 First CE𝜈NS detection

‣ 14.6 kg CsI scintillating cristal

‣ 19.3 m from the source

‣ 134 ± 22 events observed (173 ± 48 predicted)

‣ 6.7σ significance

M. Green @ Magnificent CEvNS 2019

20

Stopped-

pion beam experiments

COHERENT CsI 2020

‣ 2020 More statistics! +2x

‣ Better signal reconstruction

‣ 306 ± 20 events observed (333 ± 11 (th) ± 42 (ex) predicted)

‣ No CE𝜈NS rejection: 11.6σ

‣ Result consistent with SM prediction at 1σ

‣ Flux uncertainty dominates the systematic uncertainties !"#$%

D. Pershey @ Magnificent CEvNS 2020

21

Stopped-

pion beam experiments

COHERENT in Argon

c

‣ 2020 first results with he CENNS-10 detector

‣ Active mass 24 kg at 27.5 m from the source

‣ Single phase only (scintillation) with a threshold at 20 keVnr

‣ 2 independent blind analyses

‣ 3σ CE𝜈NS detection significance

Cross section = (2.3 ± 0.7 )10^-39 cm²

22

Stopped-

pion beam experiments

COHERENT in Argon

First confirmation of SM prediction of N² dependence !

J. Newby @ Neutrino2020

‣ 2020 first results with he CENNS-10 detector

‣ Active mass 24 kg at 27.5 m from the source

‣ Single phase only (scintillation) with a threshold at 20 keVnr

‣ 2 independent blind analyses

‣ 3σ CE𝜈NS detection significance

23

Stopped-

pion beam experiments

Ongoing and new experiments

European Spallation Source

• Gaseous detector for Neutrino physics at the ESS (GaNESS)

• Other proposed projects

ex: JHEP 2020,123 (2020);

arXiv:1911.00762

Panel Neutrino 6 – #20

Coherent CAPTAIN- Mills (CCM)

Lujan Center @ LANSCE

24

Brokdorf nuclear power plant in Germany

17 m

Experiment @ 17 m from the 3.9 GW reactor core Flux:

Reactor-OFF periods (~1 month/year) allows to study the surrounding background

Four 1kg-HPGe detectors (low-background crystals) Passive and active shield (10⁴ fold suppression)

Lead + polyethylene

Active muon-veto (plastic scintillators)

Energy threshold ~ 300 eVee (efficiency ~ 100%)

Nuclear reactors

CONUS

2<latexit sha1_base64="D2kquSzLUN138YH9a8RrxR0m6AQ=">AAACIXicbVBNSwMxEM36bf1a9eglWAQvlt1WsEfRi8cKVoVuLdl02oZms0syK5Zl/Sle/CtePCjSm/hnTGsFrT4IvHlvhsm8MJHCoOe9OzOzc/MLi0vLhZXVtfUNd3Pr0sSp5lDnsYz1dcgMSKGgjgIlXCcaWBRKuAr7pyP/6ha0EbG6wEECzYh1legIztBKLbdapgFvx0h97ybzK/l9EDKdBSptgeUId5jxKL/JDsrfpRlVft5yi17JG4P+Jf6EFMkEtZY7DNoxTyNQyCUzpuF7CTYzplFwCXkhSA0kjPdZFxqWKhaBaWbjC3O6Z5U27cTaPoV0rP6cyFhkzCAKbWfEsGemvZH4n9dIsVNtZkIlKYLiX4s6qaQY01FctC00cJQDSxjXwv6V8h7TjKMNtWBD8KdP/ksuyyW/UiqfHxaPTyZxLJEdskv2iU+OyDE5IzVSJ5w8kCfyQl6dR+fZeXOGX60zzmRmm/yC8/EJY92kVg==</latexit> · 10¹³ ⌫¯_e cm ² s ¹

J. Hakenmüller @ Magnificent CEvNS 2020

25

Nuclear reactors

CONUS

Measurement spectra

Best limit on CE𝜈NS in the fully coherent

regime as a function of the quenching factor parameter k

k < 0.27 desfavorece by data

CONUS, PRL 126, 041804 (2021)

Panel Neutrino 6 – #288

26 J. Hakenmüller @ Magnificent CEvNS 2020

Nuclear reactors

CONNIE

Experiment @ 30 m from the 3.9 GW reactor core Flux:

Reactor-OFF periods (~1/14 months) for background measurements

14 CCDs of 6 g each

Passive shield (Lead + polyethylene)

Energy threshold ~ 50 eVee

Angra 2 nuclear power plant in Brazil

CONNIE, PRD 100, 092005 (2019)

⇠<latexit sha1_base64="fGty5yGY+kF2FqOE35Wzbcav/X4=">AAACHnicbVBNSwMxEM36bf2qevQSLIIXy25V9Ch68ahgbaFbSzadajDJLsmsWJb1j3jxr3jxoIjgSf+N6Yeg1geBN+/NMJkXJVJY9P1Pb2x8YnJqema2MDe/sLhUXF45t3FqOFR5LGNTj5gFKTRUUaCEemKAqUhCLbo+6vm1GzBWxPoMuwk0FbvUoiM4Qye1iruhFYoG/kUWVPK7MGImC3XaAscRbjHjKr/Itirfpe1VQd4qlvyy3wcdJcGQlMgQJ63ie9iOeapAI5fM2kbgJ9jMmEHBJeSFMLWQMH7NLqHhqGYKbDPrn5fTDae0aSc27mmkffXnRMaUtV0VuU7F8Mr+9Xrif14jxc5+MxM6SRE0HyzqpJJiTHtZ0bYwwFF2HWHcCPdXyq+YYRxdogUXQvD35FFyXikH2+XK6U7p4HAYxwxZI+tkkwRkjxyQY3JCqoSTe/JInsmL9+A9ea/e26B1zBvOrJJf8D6+AL0Co4Q=</latexit> 10¹² ⌫¯_e cm ² s ¹

27

Nuclear reactors

CONNIE

Panel Neutrino 6 – #188

Constrains to Non-Standard Interactions

Light scalar (φ) mediator Light vector (Z’) mediator

CONNIE, JHEP 04, 054 (2020)

New data set (5x1 binning for better signal-noise ratio)

New detectors recently installed

• Results compatible with previous analysis

• Expected limit in the lowest-energy bin

~30 times the SM prediction

• Skipper-CCDs allows to decrease the detection threshold to ~15 eV

28

Nuclear reactors

nuGeN

Panel Neutrino 6 – #69

1.5 kg HPGe detector

~ 10-11 m of the 3.1 GW reactor core (distance can change) Flux:

Reactor-OFF periods (~2/18 months) for background measurements Overburden ~ 50 m.w.e

Passive and active shield

Copper + B-polyethylene + lead + B-polyethylene Active muon-veto

Kalinin Nuclear Power Plant in Rusia

5<latexit sha1_base64="yYfjADms8jWz0S2V/0OGYtUFZyc=">AAACIXicbVBNSwMxEM3Wr1q/qh69BIvgxbLbKnoUvXisYKvQbUs2nWpoNrsks2JZ1p/ixb/ixYMivYl/xrRW0OqDwJv3ZpjMC2IpDLruu5ObmZ2bX8gvFpaWV1bXiusbDRMlmkOdRzLSVwEzIIWCOgqUcBVrYGEg4TLon478y1vQRkTqAgcxtEJ2rURPcIZW6hSPDqjPuxFSz22nXjW79wOmU18lHbAc4Q5THmbtdK/yXZpR5WWdYsktu2PQv8SbkBKZoNYpDv1uxJMQFHLJjGl6boytlGkUXEJW8BMDMeN9dg1NSxULwbTS8YUZ3bFKl/YibZ9COlZ/TqQsNGYQBrYzZHhjpr2R+J/XTLB31EqFihMExb8W9RJJMaKjuGhXaOAoB5YwroX9K+U3TDOONtSCDcGbPvkvaVTKXrVcOd8vHZ9M4siTLbJNdolHDskxOSM1UiecPJAn8kJenUfn2Xlzhl+tOWcys0l+wfn4BGkOpFk=</latexit> · 10¹³ ⌫¯_e cm ² s ¹

No signal excess observed

29

Nuclear reactors

CE 𝜈 NS @ Dresden-II

3 kg of P-type point contact (PPC) Ge detector

Located @ 8 m of 2.96 GW (BWR) boiling water reactor Flux:

Detector threshold: 0.2 keVee

Passive (lead + cadmium sheet) and active (scintillator) shield

J. Colaresi, et al, arXiv:2108.02880

8.1<latexit sha1_base64="Nvgfxh/+lQ9GnPmSARnGPtd3/rw=">AAACI3icbVDLSgMxFM34tr6qLt0Ei+DGMmkFi6uiG5cK1gqdWjLprQYzmSG5I5Zh/BY3/oobF4q4ceG/mD4EXwcC555zLzf3hImSFn3/3ZuYnJqemZ2bLywsLi2vFFfXzmycGgENEavYnIfcgpIaGihRwXligEehgmZ4fTjwmzdgrIz1KfYTaEf8UsueFByd1Cnu18qMBqIbI2X+Rcaq+V0QcpMFOu2A4wi3mIkov8h2Kl+lHVQs7xRLftkfgv4lbExKZIzjTvE16MYijUCjUNzaFvMTbGfcoBQK8kKQWki4uOaX0HJU8whsOxvemNMtp3RpLzbuaaRD9ftExiNr+1HoOiOOV/a3NxD/81op9mrtTOokRdBitKiXKooxHQRGu9KAQNV3hAsj3V+puOKGC3SxFlwI7PfJf8lZpcyq5crJbql+MI5jjmyQTbJNGNkjdXJEjkmDCHJPHskzefEevCfv1XsbtU5445l18gPexydeNaTP</latexit> · 10¹³ ⌫¯_e cm ² s ¹

Dominant background: epithermal neutrons Best-fit epithermal neutron background

(model)

Lower background and threshold needed !!

30

Nuclear reactors

NeON

Panel Neutrino 6 – #329

Neutrino Elastic-scattering Observation with NaI Detector threshold < 0.3 keV

15 kg (comercial detectors: 3x 1.6 kg & 3x 3.4 kg) Located @ 23.7 m of a 2.8 GW nuclear reactor

Flux:

Passive shield (polyethylene, B-polyethylene and lead) Active shield (liquid scintillator)

7.1<latexit sha1_base64="DIuohor/axpgiJSRx6bILnaIecY=">AAACIHicbVBNSwMxEM36bf2qevQSLIIXy6YK9Sh68ahgtdCtJZtO22A2uySzYlnWf+LFv+LFgyJ6019j+nFQ64PAm/dmmMwLEyUt+v6nNzU9Mzs3v7BYWFpeWV0rrm9c2jg1AmoiVrGph9yCkhpqKFFBPTHAo1DBVXhzMvCvbsFYGesL7CfQjHhXy44UHJ3UKlarZUYD0Y6RMv86Y5X8Pgi5CXTagvsA4Q4zEeXX2V4lH1V2ULC8VSz5ZX8IOknYmJTIGGet4kfQjkUagUahuLUN5ifYzLhBKRTkhSC1kHBxw7vQcFTzCGwzGx6Y0x2ntGknNu5ppEP150TGI2v7Ueg6I449+9cbiP95jRQ7h81M6iRF0GK0qJMqijEdpEXb0oBA1XeECyPdX6noccMFukwLLgT29+RJclkps/1y5fygdHQ8jmOBbJFtsksYqZIjckrOSI0I8kCeyAt59R69Z+/Nex+1TnnjmU3yC97XN27hozk=</latexit> · 10¹² ⌫¯_e cm ²s ¹

Hanbit nuclear power plant in Korea

H. Su Lee @ Magnificent CEvNS 2020

End of 2020 – delivered to Hanbit

Sensitivity:

Flat background of ~ 5 dru (thanks to the veto) Light yield of 22 NPE/keV

Threshold 5 NPE

31

Nuclear reactors

NUCLEUS

Panel Neutrino 6 – #152

g-scale CaWO4 and Al2O3 crystals @ mK temperatures

2 arrays of 3 x 3 cryogenic crystals

Detector threshold ~ 20 eV

Target background 100 events/kg/day/keV

102 m & 72 m of 2 reactors of the Chooz-B plant of 4.25 GW each Flux:

Multi-layer passive shield + active vetos

Ge & Si cryogenic active veto

Muon veto with plastic scintillators

Chooz–B plant in France

R. Cerulli @ Magnificent CEvNS 2020

Assuming flat background:

~ 40 days with a bkg < 100 dru, CE𝜈NS can be observed at 5σ

1.7<latexit sha1_base64="RJbw+PVDbry42Ed1BZDXHRbaoxQ=">AAACIHicbVBNSwMxEM36bf2qevQSLIIXy6YK9Sh68ahgtdCtJZtO22A2uySzYlnWf+LFv+LFgyJ6019j+nFQ64PAm/dmmMwLEyUt+v6nNzU9Mzs3v7BYWFpeWV0rrm9c2jg1AmoiVrGph9yCkhpqKFFBPTHAo1DBVXhzMvCvbsFYGesL7CfQjHhXy44UHJ3UKlZZuUoD0Y6RMv86Y5X8Pgi5CXTagvsA4Q4zEeXX2V4lH1V2ULC8VSz5ZX8IOknYmJTIGGet4kfQjkUagUahuLUN5ifYzLhBKRTkhSC1kHBxw7vQcFTzCGwzGx6Y0x2ntGknNu5ppEP150TGI2v7Ueg6I449+9cbiP95jRQ7h81M6iRF0GK0qJMqijEdpEXb0oBA1XeECyPdX6noccMFukwLLgT29+RJclkps/1y5fygdHQ8jmOBbJFtsksYqZIjckrOSI0I8kCeyAt59R69Z+/Nex+1TnnjmU3yC97XN27Vozk=</latexit> · 10¹² ⌫¯_e cm ²s ¹

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Nuclear reactors

vIOLETA

few kg-scale experiment

skipper-CCDs technology

Detector threshold ~15 eV

Installed at 12 m of a 2GW nuclear reactors

Atucha II plant in Argentina

G. Fernandez-Moroni, et al, arXiv:2009.10741

G. Fernandez-Moroni, et al, arXiv:2108.07310 G. Fernandez-Moroni, et al, arXiv:2107.00168

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Summary CE 𝜈 NS: very active field

Exciting moment: new results from different experiments (and techniques) expected soon.

New facilities and next generation experiments being designed

Synergy between experiments and theory

It’s just the beginning....

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Discussion Panel Neutrinos 6

1 Sep 2021, 17:10 (event timezone)

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Thank you !!

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