Robert Cooper

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

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

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

Physics Cases for CENNS 5R.L. Cooper Bentz et al., Phys Lett B 693 (2010) see also Scholberg, Phys Rev D 73 (2006) 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

Physics Cases for CENNS 6R.L. Cooper Bentz et al., Phys Lett B 693 (2010) see also Scholberg, Phys Rev D 73 (2006) 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

Physics Cases for CENNS 7R.L. Cooper Ar-C data + models Patton et al., arXiv/ 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

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

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

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)  ee constraints in Ne & Xe 100 kg / yr, 20 m from SNS

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), SNS Stopped Pion Energy Spectrum

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

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

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

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 ]

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

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

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 m from BNB at 32 kW and 30 keV threshold

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

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

Typical Sources of Uncertainty Duty factor (~ ) 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

Typical Sources of Uncertainty Duty factor (~ ) 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

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

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 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

PINCH HITTERS (BACKUPS) 25R.L. Cooper

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) , astro-ph/ Never been observed! SM tests: measure sin 2  W Form factors Supernova physics Non-standard Interactions Irreducible dark matter background

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

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

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), , hep-ph/ at 20 m

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

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

Background Rejection in Signal Beam duty factor ~ 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 ]

BNB Experiment Layout 33R.L. Cooper