1. Robert Cooper

2. What is CENNS? Coherent Elastic Neutrino-Nucleus Scattering To probe a “large” nucleus Recoil energy small Differential energy spectrum 2R.L. Cooper E E M

3. Fundamental But Unobserved Low energy threshold is difficult Cross section actually dominates at low energy! Dark matter development is crucial Cross section goes as N 2 Maximum recoil energy goes as M -1 Rate vs. threshold optimization problem 3R.L. Cooper K. Scholberg at Coherent NCvAs mini-workshop at FNAL Neutrino Cross Sections vs Energy Coherent 40 Ar electrons

4. Physics Cases for CENNS 4R.L. Cooper Never been observed! SM tests: measure sin 2  W Form factors Supernova physics Non-standard Interactions Irreducible dark matter background

5. Physics Cases for CENNS 5R.L. Cooper Bentz et al., Phys Lett B 693 (2010) 462-466 see also Scholberg, Phys Rev D 73 (2006) 033005 sin 2  W vs. Q with possible CENNS Never been observed! SM tests: measure sin 2  W Form factors Supernova physics Non-standard Interactions Irreducible dark matter background

6. Physics Cases for CENNS 6R.L. Cooper Bentz et al., Phys Lett B 693 (2010) 462-466 see also Scholberg, Phys Rev D 73 (2006) 033005 sin 2  W vs. Q with possible CENNS Never been observed! SM tests: measure sin 2  W Form factors Supernova physics Non-standard Interactions Irreducible dark matter background  /  ~ 10%   W /  W ~ 5% New channel could be sensitive in next generation experiments

7. Physics Cases for CENNS 7R.L. Cooper Ar-C data + models Patton et al., arXiv/1207.0693 3.5 ton Ar, 16 m from SNS, 1 year,  = 0 4 th vs 2 nd Form Factor Moments Never been observed! SM tests: measure sin 2  W Form factors Supernova physics Non-standard Interactions Irreducible dark matter background

8. Physics Cases for CENNS 8R.L. Cooper Never been observed! SM tests: measure sin 2  W Form factors Supernova physics Non-Standard Interactions Irreducible dark matter background

9. Physics Cases for CENNS 9R.L. Cooper Never been observed! SM tests: measure sin 2  W Form factors Supernova physics Non-Standard Interactions Irreducible dark matter background Very wide limits on  ee &  e  terms

10. Physics Cases for CENNS 10R.L. Cooper Never been observed! SM tests: measure sin 2  W Form factors Supernova physics Non-Standard Interactions Irreducible dark matter background Scholberg, Phys Rev D 73 (2006) 033005  ee constraints in Ne & Xe 100 kg / yr, 20 m from SNS

11. Accelerator Neutrino Sources Few GeV protons on target produces  + Prototypical source is SNS SNS flux at 20 m  SNS = 1×10 7 s -1 cm -2 Other alternatives? 11R.L. Cooper Avignone & Efremenko, J Phys G 29 (2003), 2615-2628 SNS Stopped Pion Energy Spectrum

12. Accelerator Neutrino Sources Few GeV protons on target produces  + Prototypical source is SNS SNS flux at 20 m  SNS = 1×10 7 s -1 cm -2 Other alternatives? 12R.L. Cooper SNS Neutrino Rates in Time beam

13. Pion Decay in Flight Source FNAL BNB is a pion decay in-flight source (8 GeV p + ) On-axis multi-GeV neutrinos Far off-axis spectrum is much softer and narrower BNB flux at 20 m, cos  < 0.5  BNB = 5×10 5 s -1 cm -2 13R.L. Cooper J. Yoo & S. Brice, Booster Neutrino Beam Monte Carlo Angle Off-Axis Neutrino Rate

14. Pion Decay in Flight Source FNAL BNB is a pion decay in-flight source (8 GeV p + ) On-axis multi-GeV neutrinos Far off-axis spectrum is much softer and narrower BNB flux at 20 m, cos  < 0.5  BNB = 5×10 5 s -1 cm -2 14R.L. Cooper J. Yoo & S. Brice, Booster Neutrino Beam Monte Carlo Off-Axis Neutrino Energy Spectrum

15. Detection of Coherent Scattering Pick a dark matter technology PPC high purity Ge CsI[Na] inorganic scintillators Dual phase LXe Single phase LAr & LNe 15R.L. Cooper SNS Detection Rate [ton -1 year -1 ]

16. Detection of Coherent Scattering Pick a dark matter technology PPC high purity Ge CsI[Na] inorganic scintillators Dual phase LXe Single phase LAr & LNe 16R.L. Cooper Red-1 and Red-100

17. Detection of Coherent Scattering Pick a dark matter technology PPC high purity Ge CsI[Na] inorganic scintillators Dual phase LXe Single phase LAr & LNe 17R.L. Cooper PSD from S1 & S2 Signals

18. Detection of Coherent Scattering Pick a dark matter technology PPC high purity Ge CsI[Na] inorganic scintillators Dual phase LXe Single phase LAr & LNe 18R.L. Cooper CLEAR Proposal & FNAL Effort Expect 200 events ton -1 year -1 20 m from BNB at 32 kW and 30 keV threshold

19. Detection of Coherent Scattering Pick a dark matter technology PPC high purity Ge CsI[Na] inorganic scintillators Dual phase LXe Single phase LAr & LNe 19R.L. Cooper Scintillation PSD Possible

20. Detection of Coherent Scattering Pick a dark matter technology PPC high purity Ge CsI[Na] inorganic scintillators Dual phase LXe Single phase LAr & LNe 20R.L. Cooper Scintillation PSD Possible Beam duty factor & PSD mitigates 39 Ar contamination

21. Typical Sources of Uncertainty Duty factor (~ 10 -5 ) give total exposure ~ 300 s / year  cosmic background small Neutrino flux uncertainty ~ 5-10%  improvements? Quenching & scintillation efficiency L eff uncertainties Beam correlated neutrons mimic neutrino signal 21R.L. Cooper LAr Nuclear Recoil Scintillation Efficiency

22. Typical Sources of Uncertainty Duty factor (~ 10 -5 ) give total exposure ~ 300 s / year  cosmic background small Neutrino flux uncertainty ~ 5-10%  improvements? Quenching & scintillation efficiency L eff uncertainties Beam correlated neutrons mimic neutrino signal 22R.L. Cooper ErEr EnEn M Neutron Scatter on 40 Ar where

23. In-Beam Neutron Measurements R.L. Cooper23 BNB Neutron Spectrum at 20 mIndiana-Built SciBath Detector

24. Phases of Coherent -A Experiments Detector technology exists, neutrinos sources exist, with neutron background mitigation experiments can operate near surface How can we engage your expertise? 24R.L. Cooper PhaseDetector ScalePhysics GoalsComments Phase 110-100 kgFirst DetectionPrecision flux not needed Phase 2100 kg – 1 tonSM tests, NSI searchesBecoming systematically limited Phase 31 ton – multi-tonNeutron structure, neutrino magnetic moment Systems control a dominant issue; multiple targets useful Table from K. Scholberg at Coherent NCvAs mini-workshop at FNAL

25. PINCH HITTERS (BACKUPS) 25R.L. Cooper

26. Physics Cases for CENNS 26R.L. Cooper Supernova energy spectrum similar to stopped pions K. Scholberg at Coherent NCvAs mini-workshop at FNAL See also Horowitz, Coakley, McKinsey Phys Rev D 68 (2003) 023005, astro-ph/0302071 Never been observed! SM tests: measure sin 2  W Form factors Supernova physics Non-standard Interactions Irreducible dark matter background

27. Physics Cases for CENNS 27R.L. Cooper J. Yoo at Coherent NCvAS mini-workshop at FNAL Solar, Atmosphere, and SN Neutrinos Never been observed! SM tests: measure sin 2  W Form factors Supernova physics Non-standard Interactions Irreducible dark matter background

28. Physics Cases for CENNS Never been observed! SM tests: measure sin 2  W Form factors Supernova physics Non-standard Interactions Irreducible dark matter background 28R.L. Cooper J. Yoo at Coherent NCvAS mini-workshop at FNAL Dark Matter Sensitivity

29. Reactor Neutrino Sources Reactors give very high flux Single neutrino flavor Low energy forces detector thresholds < 10 keV Steady state running and backgrounds Reactor off for backgrounds Reactor monitoring applications 29R.L. Cooper Murayama & Pierce, Phys Rev D 65 (2002), 013012, hep-ph/0012075 at 20 m

30. Detection of Coherent Scattering Pick a dark matter technology PPC high purity Ge CsI[Na] inorganic scintillators Dual phase LXe Single phase LAr & LNe 30R.L. Cooper Majorana PPC Ge Detector sub-keV thresholds PPC allows multi- scattering site discrimination

31. Detection of Coherent Scattering Pick a dark matter technology PPC high purity Ge CsI[Na] inorganic scintillators Dual phase LXe Single phase LAr & LNe 31R.L. Cooper FNAL 1-ton LAr Detector

32. Background Rejection in Signal Beam duty factor ~ 10 -5 Total exposure 300 s / year PSD can reject 39 Ar betas and gamma backgrounds Require beam-correlated neutrons < 10 year -1 ton -1 SciBath deployed to measure this rate 32R.L. Cooper J. Yoo at Coherent NCvAS mini-workshop at FNAL Detection Rate [kev -1 ton -1 year -1 ]

33. BNB Experiment Layout 33R.L. Cooper