Neutrino Coherent sca/ering. Will we see it in 2017? Yuri - PowerPoint PPT Presentation

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 CEνNS Proposed 1 Super symmetry 0.5 0 1900 1920 1940 1960 1980 2000 2020 CEνENS à Coherent ElasRc Neutrino Nucleus Sca/ering

Neutrinos are popular in many communiRes. This is actual shot at Lead S.D.

What do we know about neutrinos? F. A. Sco/, Phys. Rev. 48, 391 (1935) I. They do exist H II. There are three light neutrino species N ν =2.984±0.008 Z 0 III. Neutrinos do oscillate and (observed - bg) / expected therefore they are massive

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

" $ 2 ( ) − N d σ = G F T A 2 " $ 4 π m A Z 1 − 4sin 2 θ W ' F 2 ( Q 2 ) 1 − m A & # % 2 dT A 2 E ν # % 2 E ν 2 ( ) − N σ tot = G F 2 " $ Z 1 − 4sin 2 θ W F 2 ( Q 2 ) # % 4 π m A − nucleus mass T A − kinetic energy of recoil nucleus E ν − neutrino energy Z − nucleus charge N − number of neutrons in the nucleus F is nucleus form factor E ν < 50 MeV

Weinberg (Electro week) angle cos ϑ W = m W = 0.23120 ± 0.00015 m Z 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.

CEvNS and Weinberg angle? 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. Measurement with target having G 2 f E 2 different Z/N raRo is required. ( Z (4 sin 2 θ w − 1) + N ) 2 σ coh ∼ 4 π CorrecRon to g-2 for muon arXiv:1411.4088 magneRc moment due to a light mediator COHERENT Barbeau

Non-Standard InteracRons of Neutrinos: new interac>on specific to ν ’s = − G F � ν α γ µ (1 − γ 5 ) ν β ] × ( ε qL q γ µ (1 − γ 5 ) q ] + ε qR L NSI q γ µ (1 + γ 5 ) q ]) [¯ αβ [¯ αβ [¯ √ ν H 2 q = u,d α , β = e,µ, τ J. High Energy Phys. 03(2003) 011

Why to Search for Coherent 𝛏 -Nucleus Sca/ering? Non-Standard 𝛏 InteracRons (Supersummetry, neutrino mass K. Scholberg, Phys.Rev.D73:033005, 2006 models) can impact the cross-secRon J. Barranco et al., JHEP0512:021, 2005 differently for different nuclei C O H E R E N T

DUNE ~1 billion project – measuring the charge-parity (CP) violaRng phase CP, – determining the neutrino mass ordering (the sign of Δm 2 12 ) – precision tests of the three-flavor neutrino oscillaRon paradigm

arXiv:1604.05772v1 NO w/no NSI... If you allow for NSI to exist, can’t ...looks just like tell the neutrino mass ordering IO w/NSI without constrains on NSI

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

Neutrino magneRc moment Signature is distor>on at low recoil energy E dE = πα 2 µ 2 ν Z 2 d σ ✓ 1 − E/k + E ◆ m 2 E 4 k 2 e Ne target µ B µ B Present Limit è requires low energy threshold See also Kosmas et al., arXiv:1505.03202

Physics for Future Expansions The development of a coherent neutrino The cross-secRon is sensiRve to the • sca/ering detecRon capability provides the magnitude of the Neutrino MagneRc most natural way to explore the sterile Moment (Supersymmetry, Large Extra neutrino sector. Dimensions, Right Handed Weak Currents). A. C. Dodd, et al., PLB 266 (91), 434 A. Drukier & L. Stodolsky, PRD 30 (84) 2295 A. J. Anderson et al., PRD 86 013004 (2012) COHERENT may be the first experiment • to observe the EffecRve Neutrino Charge Radius. J. Papavassiliou, J.Bernabeu, M. Passera, HEP-EPS 2005, Lisbon, arXiv:hep-ph/0512029 The neutron distribuRon within the • nucleus impacts the recoil energy dependent cross-secRon (Form Factor) K. Patton, et al., PRC 86, 024216 16

Why to Search for Coherent 𝛏 -Nucleus Sca/ering? Large effect on Supernovae dynamics. J.R. Wilson, PRL 32 (74) 849 We should measure it to validate the models 17 Barbeau

Why to Search for Coherent 𝛏 -Nucleus Sca/ering? It will be irreducible background for Dark Ma/er experiments CoGeNT (2012) CDMS Si (2013) 2 ) 1 0 2 ( E L P M I S 2 ) 1 DAMA 0 2 ( P P U O C ) 2 1 0 2 I ( I I - N L I P E Z 9 ) 0 0 2 ( e G I I S M EDELWEISS (2011) D C Xenon100 (2012) LUX (2013) Plot: E. Figueroa-Feliciano 18 Barbeau

(Stodolsky) 10 kpc, 10 ton à 100 events ~1K events per ton per year. + =

σ , cm 2 ν+Xe 1.E-37 1.E-38 Cross SecRon 1.E-39 IBD 1.E-40 ν+He is Large !!! 1.E-41 1.E-42 1.E-43 1.E-44 E ν , MeV 0 10 20 30 40 50 E recoils , MeV 1.E+01 ν+He 1.E+00 But the Signal is 1.E-01 ν+Xe 1.E-02 Hard to Detect 1.E-03 1.E-04 1.E-05 E ν , MeV 0 10 20 30 40 50

Neutrino Coherent Sca/ering detecRon Z 0 A A

Nuclear Reactors 3 GW – 1 MW Distance ~20 m E ν ~ 4 MeV ConRnues operaRon 6*10 20 ν/sec Stopped Pion 1.3 MW FaciliRes Distance ~20 m E ν ~ 40 MeV Pulsed beam 2*10 15 ν/sec

Race for the first CEvNS detecRon Experiment Neutrino EffecRve E v Distance Technology Target Mass Source Ricochet at Chooz 2x4.3GW ~4 MeV 355 m Bolometer Ge, Zn 5 + 5 kg Chooz Ricochet at MITR 5 MW ~4 MeV 4 m Bolometer Ge, Zn 5 + 5 kg MIT Texas A&M MINER ~4 MeV 2 m IonizaRon Ge, Si ~ kg 1 MW CONNIE Angra 3.8 GW ~4 MeV 30 m CCD Si 0.1 kg Kalinin RED-100 ~4 MeV 25 m 2 phase Xe 100 kg 3.2 GW Kalinin vGeN ~4 MeV 10 m IonizaRon Ge ~5 kg 3.2 GW CsI, Ar, COHERENT SNS (DAR) ~40 MeV 20-30 m IonizaRon 14, 30, 10 kg Ge In red shown experiments which are taking data

He Si Xe Ge Ar

My Car 25

SNS layout Stripping foil 1.3 GeV proton linear accelerator Accumulator ring LINAC: ⋅⋅⋅ x ~1000 ⋅⋅⋅ Accumulator Ring: Repeat 60/sec. Main target 26

Mercury target Mercury Inventory – 20 t Flow rate 340 kg/sec V max 3.5 m/sec T in 60 0 C T out 90 0 C Mercury lasts the entire 40 year lifetime of SNS no change is required 27 Stainless steel vessel should be replaced periodically

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.

Decay In Flight or Decay At Rest Pion Spectra 200 MeV/c pions range in mercury is ~ 5 cm Very few pions have a chance to decay before coming to the rest Because of the bulk Mercury target, SNS is a mostly Decay At Rest facility !! 29

Neutrino ProducRon at SNS ν e CAPTURE ν µ τ < 2200 nsec e - µ - ~94% ν µ ν µ ~1% DIF ~99% ν e CAPTURE π - τ ≈ 2200 nsec µ + DAR +DIF Hg e + π + τ ≈ 26 nsec ν µ p ν µ s n o t r u e N

Neutrino Production at the SNS The good approximaRon is N π + /proton = 0.14*E(GeV)-0.05 For E~0.8-1.5 GeV Each π + generates SNS ISIS, LANSCE electron neutrino and muon neutrino and anRneutrino 31

! 1 MW spallaRon source, 15 m from the target, 100 kg detector, prompt 30 MeV neutrinos, event rates for CEvNS Target Max Recoil (keV) Cross secRon 10 -42 cm 2 Threshold, keV nr 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

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

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!!!!

Main Target *10 3 cm ! Proton Transport Beam 35

Started in 2013 “In-Beam” events, “Out-of-beam” considerably more events, primarily neutron events (and muons. 16x less “live Rme”)

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

Neutrino Alley at the SNS Basement locaRon is far away from Neutron beam Lines. Extra protecRon from cosmic rays

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 author explains DAMA seasonal modulaRons by solar neutrino induced interacRons in the DAMA shielding In this arRcle authors believe that J.Davis is wrong by a ~6 orders of magnitude.

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!!!!