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Aug 10, 2023 46 likes •598 views

Neutrino Coherent sca/ering. Will we see it in 2017? Yuri Efremenko, UTK Feb 15 th 2017 HEP&Astro seminar Time scales in HEP 3.5 Neutrinos ApplicaRon 3 2.5 Higgs Discovered 2 1.5 CENS Proposed 1 Super symmetry 0.5 0 1900

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Neutrino Coherent sca/ering. Will we see it in 2017?

Yuri Efremenko, UTK Feb 15th 2017 HEP&Astro seminar

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SLIDE 2

Time scales in HEP

0.5 1 1.5 2 2.5 3 3.5

1900 1920 1940 1960 1980 2000 2020

Proposed Discovered ApplicaRon

Neutrinos Higgs CEνNS

CEνENS à Coherent ElasRc Neutrino Nucleus Sca/ering

Super symmetry

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SLIDE 3

Neutrinos are popular in many communiRes.

This is actual shot at Lead S.D.

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SLIDE 4

What do we know about neutrinos?

  • I. They do exist
  • F. A. Sco/, Phys. Rev. 48, 391 (1935)
  • II. There are three light

neutrino species Nν=2.984±0.008

Z0

  • III. Neutrinos do oscillate and

therefore they are massive

(observed - bg) / expected

H

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SLIDE 5

What we do not Know About Neutrinos?

Exact mass value Mass hierarchy Are neutrino its own anRparRcle How neutrinos affect evoluRon of the universe Are there any sterile neutrinos Neutrino interac;ons

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SLIDE 6

dσ dTA = GF

2

4π mA Z 1− 4sin2θW

( )− N

" # $ %

2

1− mA TA 2Eν

2

" # & $ % 'F 2(Q2) σ tot = GF

2Eν 2

4π Z 1− 4sin2θW

( )− N

" # $ %

2

F 2(Q2) mA − nucleus mass TA − kinetic energy of recoil nucleus Eν − neutrino energy Z − nucleus charge N − number of neutrons in the nucleus F is nucleus form factor Eν < 50MeV

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SLIDE 7
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SLIDE 8

Weinberg (Electro week) angle

cosϑW = mW mZ = 0.23120± 0.00015

It is free parameter in the Standard Model There is no fundamental theory which explain its value It is “running” constant, it depends on the momentum transfer.

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SLIDE 9

CEvNS and Weinberg angle?

arXiv:1411.4088

σcoh ∼ G2

fE2

4π (Z(4 sin2θw − 1) + N)2

Barbeau

Measurement with target having different Z/N raRo is required.

A precision test of 𝜏 is a sensiRve test of new physics above the weak scale. SensiRvity to a hypotheRcal dark Z mediator, a possible explanaRon for the (g-2)μ anomaly, can be reached with a 5% measurement.

CorrecRon to g-2 for muon magneRc moment due to a light mediator COHERENT

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SLIDE 10

Non-Standard InteracRons of Neutrinos:

new interac>on specific to ν’s

LNSI

νH

= −GF √ 2

  • q=u,d

α,β=e,µ,τ

[¯ ναγµ(1 − γ5)νβ] × (εqL

αβ[¯

qγµ(1 − γ5)q] + εqR

αβ[¯

qγµ(1 + γ5)q])

  • J. High Energy Phys. 03(2003) 011
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SLIDE 11

Why to Search for Coherent 𝛏-Nucleus Sca/ering?

  • J. Barranco et al., JHEP0512:021, 2005
  • K. Scholberg, Phys.Rev.D73:033005, 2006

Non-Standard 𝛏 InteracRons (Supersummetry, neutrino mass models) can impact the cross-secRon differently for different nuclei

C O H E R E N T

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SLIDE 12

DUNE

– measuring the charge-parity (CP) violaRng phase CP, – determining the neutrino mass ordering (the sign of Δm2

12)

– precision tests of the three-flavor neutrino oscillaRon paradigm

~1 billion project

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SLIDE 13

arXiv:1604.05772v1

If you allow for NSI to exist, can’t tell the neutrino mass ordering without constrains on NSI

NO w/no NSI... ...looks just like IO w/NSI

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SLIDE 14

New Paper by Pilar et al. and more in the recent literature...

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SLIDE 15

µB µB

Ne target

Neutrino magneRc moment

dσ dE = πα2µ2

νZ2

m2

e

✓1 − E/k E + E 4k2 ◆

Signature is distor>on at low recoil energy E èrequires low energy threshold

See also Kosmas et al., arXiv:1505.03202 Present Limit

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SLIDE 16

Physics for Future Expansions

  • A. Drukier & L. Stodolsky, PRD 30 (84) 2295
  • The cross-secRon is sensiRve to the

magnitude of the Neutrino MagneRc Moment (Supersymmetry, Large Extra Dimensions, Right Handed Weak Currents).

  • COHERENT may be the first experiment

to observe the EffecRve Neutrino Charge Radius.

  • The neutron distribuRon within the

nucleus impacts the recoil energy dependent cross-secRon (Form Factor)

  • K. Patton, et al., PRC 86,

024216

  • A. C. Dodd, et al., PLB 266 (91), 434
  • A. J. Anderson et al., PRD 86 013004 (2012)
  • J. Papavassiliou, J.Bernabeu, M.

Passera, HEP-EPS 2005, Lisbon, arXiv:hep-ph/0512029

16

The development of a coherent neutrino sca/ering detecRon capability provides the most natural way to explore the sterile neutrino sector.

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SLIDE 17

Why to Search for Coherent 𝛏-Nucleus Sca/ering?

J.R. Wilson, PRL 32 (74) 849

Barbeau 17

Large effect on Supernovae dynamics. We should measure it to validate the models

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Why to Search for Coherent 𝛏-Nucleus Sca/ering?

C D M S I I G e ( 2 9 ) Xenon100 (2012)

CoGeNT (2012) CDMS Si (2013)

EDELWEISS (2011)

DAMA

S I M P L E ( 2 1 2 ) Z E P L I N

  • I

I I ( 2 1 2 ) C O U P P ( 2 1 2 ) LUX (2013)

Plot: E. Figueroa-Feliciano

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It will be irreducible background for Dark Ma/er experiments

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SLIDE 19

(Stodolsky)

10 kpc, 10 ton à 100 events

~1K events per ton per year.

+

=

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1.E-44 1.E-43 1.E-42 1.E-41 1.E-40 1.E-39 1.E-38 1.E-37 10 20 30 40 50 1.E-05 1.E-04 1.E-03 1.E-02 1.E-01 1.E+00 1.E+01 10 20 30 40 50

Cross SecRon is Large !!!

Eν, MeV σ , cm2

ν+Xe ν+He ν+He ν+Xe IBD

Eν, MeV

But the Signal is Hard to Detect

Erecoils, MeV

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SLIDE 21

Neutrino Coherent Sca/ering detecRon

A

Z0

A

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SLIDE 22

Stopped Pion FaciliRes Nuclear Reactors

1.3 MW Distance ~20 m Eν ~ 40 MeV Pulsed beam 2*1015 ν/sec 3 GW – 1 MW Distance ~20 m Eν ~ 4 MeV ConRnues operaRon 6*1020 ν/sec

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SLIDE 23

Race for the first CEvNS detecRon

Experiment Neutrino Source EffecRve Ev Distance Technology Target Mass Ricochet at Chooz Chooz 2x4.3GW ~4 MeV 355 m Bolometer Ge, Zn 5 + 5 kg Ricochet at MIT MITR 5 MW ~4 MeV 4 m Bolometer Ge, Zn 5 + 5 kg MINER Texas A&M 1 MW ~4 MeV 2 m IonizaRon Ge, Si ~ kg CONNIE Angra 3.8 GW ~4 MeV 30 m CCD Si 0.1 kg RED-100 Kalinin 3.2 GW ~4 MeV 25 m 2 phase Xe 100 kg vGeN Kalinin 3.2 GW ~4 MeV 10 m IonizaRon Ge ~5 kg COHERENT SNS (DAR) ~40 MeV 20-30 m IonizaRon CsI, Ar, Ge 14, 30, 10 kg

In red shown experiments which are taking data

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SLIDE 24

Si Ge Ar Xe He

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SLIDE 25

25

My Car

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SNS layout

26

1.3 GeV proton linear accelerator Accumulator ring Main target Stripping foil

⋅⋅⋅ x ~1000 ⋅⋅⋅

LINAC: Accumulator Ring:

Repeat 60/sec.

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SLIDE 27

Mercury target

27

Mercury Inventory – 20 t Flow rate 340 kg/sec Vmax 3.5 m/sec Tin 600C Tout 900C

Mercury lasts the entire 40 year lifetime of SNS no change is required Stainless steel vessel should be replaced periodically

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SLIDE 28

Some Details of Interaction in the Target for 1.3 GeV protons

Average interacRon energy is ~1.1 GeV Average interacRon depth ~11 cm

Proton interacts near the front part of the target They break down Mercury nucleus and produce pions.

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SLIDE 29

Decay In Flight or Decay At Rest

29

200 MeV/c pions range in mercury is ~ 5 cm Very few pions have a chance to decay before coming to the rest Pion Spectra

Because of the bulk Mercury target, SNS is a mostly Decay At Rest facility !!

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SLIDE 30

Neutrino ProducRon at SNS

Hg π+ π- ~99% µ+ e+ p νµ νµ νe

τ ≈ 26 nsec τ ≈ 2200 nsec

N e u t r

  • n

s

CAPTURE

DAR +DIF νµ ~1% DIF µ-

CAPTURE

νµ ~94% νe

τ < 2200 nsec

e- νµ

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SLIDE 31

Neutrino Production at the SNS

31

SNS ISIS, LANSCE

The good approximaRon is N π+/proton = 0.14*E(GeV)-0.05 For E~0.8-1.5 GeV Each π+ generates electron neutrino and muon neutrino and anRneutrino

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SLIDE 32

!

Target Max Recoil (keV) Cross secRon 10-42cm2 Threshold, keVnr N events, year He 483 13.8 10 134 C 161 125 10 370 Ne 96 609 10 980 Si 69 688 0.1 990 Ar 48 1700 10 1080 Ge 27 5830 3 2560 I 15 19400 10 732 Xe 15 22300 1 5970

1 MW spallaRon source, 15 m from the target, 100 kg detector, prompt 30 MeV neutrinos, event rates for CEvNS

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SLIDE 33

CollaboraRon to make the first detecRon of the Neutrino Neutral Current Coherent sca/ering at the SNS

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SLIDE 34

n

There are MulRple Fast Neutron Sources inside the Target building. Intermediate Neutrons with energy more than 50 keV can produce nuclear recoils. This is major background!!!!

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SLIDE 35

!

35

*103 cm

Main Target Proton Transport Beam

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SLIDE 36

“Out-of-beam” events, primarily muons. “In-Beam” events, considerably more neutron events (and 16x less “live Rme”)

Started in 2013

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Pos 5 is locaRon with very low neutrons flux. Need shielding against gammas and cosmic. Now it is called Neutrino Alley

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SLIDE 38

Neutrino Alley at the SNS

Basement locaRon is far away from Neutron beam Lines. Extra protecRon from cosmic rays

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SLIDE 39

Never been measured. There are only theoreRcal calculaRons

This reac>on on Lead is used by HALO experiment in the SNOlab, to watch for supernovae. In

In this arRcle authors believe that J.Davis is wrong by a ~6 orders of magnitude.

author explains DAMA seasonal modulaRons by solar neutrino induced interacRons in the DAMA shielding

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SLIDE 40

First Step Is to Measure Neutrino Induced Neutrons NINs (First Neutrino Experiment at the SNS)

Liquid ScinRllator detectors inside Lead, Poly, Cd, Water shield with muon veto On the next day a{er we finished installaRon SNS got water leak in the accelerator, then target failed. Took good staRsRcs during 2014-2015 Total of 175 days of “beam” Have not seen anything above background. This is a good news for us!!!!

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SLIDE 41

Neutrino Induced Neutrons – NINs

Second AFempt

  • Liquid scinRllator detectors with neutron gamma

separaRon capability

  • Two sets with Lead (1 ton) and Iron (700kg) targets.
  • Neutron detecRon Efficiency ~10%

Lead target à almost a year of data accumulated, Iron target data taking is starRng now.

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SLIDE 42

Three Detector Technology for COHERENT Phase I

CsI LAr HPGe

Target Target Mass Max Recoil (keV) Cross secRon 10-42cm2 Threshold, keVnr N events, year Ge ~10 kg 27 5830 3 280 I 14 kg 15 19400 10 170 Ar 30 kg 15 1700 10 250

Neutrons with energy > 50 keV can produce similar recoils à major background

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CsI detector – Major Player is UCh

14.5 kg ultrapure CsI crystal inside comprehensive shielding and acRve muon veto system

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Liquid Argon Detector – Major player is UI

Specs:

  • LAr
  • ~30 kg fiducial volume
  • 2×Hamamatsu R5912-02-MOD 8”PMTs
  • 8 ‘’ borosilicate glass window
  • Standard bialkali photocathode (K2CsSb)
  • 14 dynodes
  • QE: 18%@400 nm
  • WLS - Tetraphenyl butadiene (TPB)
  • Cryomech cryocooler – 90 Wt
  • PT90 single-stage pulse-tube cold head
  • compressor: CP950
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SLIDE 45

LAr ConstrucRon

  • Acrylic cylinders and discs coated by TPB
  • 3 x cylinder by airbrush
  • 2 x disk by evapora>on at ORNL
  • The thickness of the TPB is op>mal

~ 0.2 mg/cm^2

  • Teflon wrap
  • Detector was assembled at clean room at the

staging area

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SLIDE 46

LAr at “Neutrino alley”

LAr filling line Liquefier CENNS-10 Pumping cart Gas rack Cryo compressor SC rack DAQ rack

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LAr detector filling

  • ~ 9 days for filling
  • 160 lbs LAr

12/12/2016

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Shielding design and status

Water - 9 in

(poly tank)

  • On place
  • Not enough water on the top

(~ 1”) -> water bags (~ 5”)

Copper – 1/2 in

  • Done, ready for

installa>on

Lead - 4 in

(2 layers of chevron bricks)

  • Need seismic analysis
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SLIDE 49

Projected event rates for LAr

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SLIDE 50

Array of Germanium Detectors - Major Player is NC

Up to 10 kg of Ge detectors using common LN pool Surrounded by comprehensive shielding

Dewar fabrica>on nearing comple>on. Expected delivery Spring 2017.

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SLIDE 51

Ge array construcRon

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Other potenRal neutrino physics at the SNS

Neutrino oscillaRons – Test of the LSND claim Search for Sterile Neutrinos Neutrino MagneRc moment Measurement of Neutrino Spectra from Muon Decay

Charge Current Cross secRon Measurements

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SLIDE 53

Core-collapse supernovae

SN 1987a Anglo-Australian Observatory

  • Destruction of massive star initiated by the Fe core collapse

– 1053 ergs of energy released – 99% carried by neutrinos – A few happen every century in our Galaxy, but the last one

  • bserved was over 300 years ago
  • Dominant contributor to Galactic nucleosynthesis
  • Neutrinos and the weak interaction play a crucial role in the

mechanism, which is not not well understood

SN neutrino spectra, 0.1 s post-bounce Nuclear reactors Eν<10 MeV Too cold H.E. “accelerators” Eν >100 MeV Too hot

Just right

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SLIDE 54

Supernova neutrino observa;ons

  • Measurement of the neutrino energy

spectra and time distribution from a Galactic supernova would provide a wealth of information on the conditions in supernovae, neutrino oscillations, etc.

Bruenn et al. (2004)

New generaRon of Large mass Dark ma/er experiments could be sensiRve to the GalacRc Supernovae. Need to understand signal in detectors. Low energy neutrino interacRon are never been measured!!!

SN SNS

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Conclusion

SNS is the world most powerful pulsed neutrino source Neutrino Energy range at the SNS is just right for the search of CEvNS There is comprehensive and exciRng neutrino program at the SNS Presently COHERENT collaboraRon is engage in deployment of the first generaRon of detectors to see “First Light” There are many ideas and for the what to do a{er the first

  • bservaRon of SEvNS