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Nuclear Science & the New Standard Model: Neutrinos & Fundamental Symmetries in the Next Decade The Nuclear next physics decade studies presents ofNP ns & with a historic fundamental opportunity symmetries to buildplayed on thisan legacy essential in developing role in developing the “new & Standard confirming Model” the Standard Model Fifty years of PV in nuclear physics The Our value role has of our been contribution broadly will be broadly recognized recognized within and outside beyond the NP field Solar ns & the neutrino revolution Michael Ramsey-Musolf, APS April, 2007 Community Input • Pre-Town Meetings: Santa Fe Nov 2006 (~ 50 participants) Caltech Dec 2006 (~ 50 participants) • DNP Town Meeting Chicago Jan 2007 (~ 370 participants) • White paper (merging two) Substantial work by the organizing committee Primary Recommendation: New Standard Model Initiative Scientific Questions, Achievements & Challenges Primary Scientific Questions • What are the masses of neutrinos and how have they shaped the evolution of the universe? 0nbb decay, q13, b decay,… • Why is there more matter than antimatter in the present universe? EDM, DM, LFV, 0nbb, q13 … • What are the unseen forces that disappeared from view as the universe cooled? Weak decays, PVES, gm-2,… Tribble report Scientific Achievements • Discovery of flavor oscillations in solar neutrinos; Solution of the solar neutrino problem; 1300+ citations • Discovery of flavor oscillations in reactor neutrinos; Identification of LMA solution; over 1000 citations • World’s most precise measurement of (gm-2) Possible first indications of supersymmetry; over 1000 citations • Most precise measurement of sin2qW off the Z0 resonance using PV Moller scattering; constrains new physics at the TeV scale (Z’, RPV SUSY…) Scientific Achievements • Definitive test of large Dm2 oscillations by MiniBoone experiment (April 2007! ) • Definitive determinations of strange quark contributions to nucleon EM form factors using PV electron-proton & electron-nucleus scattering; confirmed theoretical estimates of hadronic effects in electroweak radiative corrections • Quark-lepton universality tested to 0.05% using superallowed nuclear b-decay, yielding most precise value of any CKM matrix element (Vud) 2006 Bonner Prize in Nuclear Physics recognizing work of Towner & Hardy Scientific Achievements • Completion of a comprehensive set of computations of supersymmetric effects in lowenergy electroweak observables; 2005 Dissertation Award in Nuclear Physics to A. Kurylov • Reduction in the theoretical hadronic uncertainty in extraction of Vud from neutron and nuclear b-decay • New theoretical breakthroughs in simulating neutrino flavor transformation in supernovae; modeling n flavor transformation effects nucleosynthesis with SN’s; understanding weak interaction effects in SN shock dynamics Scientific Achievements • 2007 Bonner Prize (S.J. Freedman*) and Dissertation Award in Nuclear Physics (K. Milknaitis) for experimental work in neutrinos • Four Bonner Prizes (Bowman, McDonald, Hardy/Towner, Freedman ) • Three Dissertation Awards (Heeger, Kurylov, Miknaitis) * Also weak decays Technological Achievements & Investments b-decay: Neutrino Mass KATRIN, NexTex, MARE… Total Lepton Number & Neutrino Mass Term QuickTime™ and a TIFF (Uncompressed) decompressor are needed to see this picture. Majorana 0nbb-decay QuickTime™ and a TIFF (LZW) decompressor are needed to see this picture. CUORE EXO GERDA Technological Achievements & Investments QuickTime™ and a TIFF (Uncompressed) decompressor are needed to see this picture. Fundamental Neutron Physics Beamline at SNS QuickTime™ and a TIFF (Uncompressed) decompressor are needed to see this picture. 1.4 MW , 1 GeV Hbeam on L Hg Also new capabilities at LANSCE, NIST… Quic kTime™ and a TIFF ( Unc ompres s ed) dec ompr es s or are needed to s ee this pic ture. CEBAF 12 GeV Up-grade QuickTime™ and a TIFF (Uncompressed) decompressor are needed to see this picture. Muon storage ring at BNL QuickTime™ and a TIFF (Uncompressed) decompressor are needed to see this picture. ISAAC, RIBF…. Technological Achievements & Investments DUSEL Multi-purpose Facility Site selection process proceeding at NSF Challenges: What role can low energy studies play in the LHC era ? (and beyond!) Two frontiers in the search for new physics Collider experiments (pp, e+e-, etc) at higher energies (E >> MZ) Large Hadron Collider Indirect searches at lower energies (E < MZ) but high precision Ultra cold neutrons CERN High energy physics Particle, nuclear & atomic physics Scientific Opportunities • • • Major Discovery Potential: 0nbb-decay & EDM Precision measurements Neutrino mixing & hierarchy Weak decays, PVES, gm-2 Electroweak probes of QCD PVES, Hadronic PV, nN scatt… The Origin of Matter & Energy Electroweak symmetry breaking: Higgs ? WIMPy D.M.: Related to baryogenesis? Leptogenesis: discover the ingredients: LN- & CPviolation in neutrinos Weak scale baryogenesis: test experimentally: EDMs Baryogenesis: When? CPV? SUSY? Neutrinos? “New gravity”? Lorentz violation? Grav baryogen ? ? Nuclear Science mission: explain the origin, evolution, & structure of SM symmetry (broken) Beyond the SM “KnownEnergy Unknowns” Cosmic Budget the baryonic component 0nbb-Decay: LNV? Mass Term? Dirac Majorana b-decay Long baseline Theory Challenge: matrix e e elements+ mechanism ? 1000 EFF mW n De ge ne rate Effective bb Mass (meV) 100 Inve r te d Nor m al m Ue1 = 0.866 1 Ue2 = 0.5 m 2 2 atm s ol 2 = 70 meV = 2000 meV Ue3 = 0 2 0.1 2 1 ? 3 4 5 6 7 2 3 4 5 6 7 10 100 Minimum Neutrino Mass (meV) 2 3 4 5 6 7 1000 u AZ,N d e W u u e˜ d W k e nM W 2 e 10 n MUek mk e2i e 0 e˜ u AdZ 2,N 2 d EDMs: New CPV? f˜ Electron ˜0 f˜ Improvements of 102 to 103 f f˜ ˜0 Neutron ˜ 0 f˜ g p q˜ f q˜ q QCD q˜ ˜ N e q q˜ ˜ 0 g q˜ QCD Deuteron g q˜ 0 n Neutral Atoms q QCD Baryogenesis: EDMs & Colliders Theory progress & challenge: refined computations of baryon asymmetry & EDMs baryogenesis LHC reach LEP II excl Present de ILC reach dn similar Prospective de Precision Probes of New Symmetries Electroweak symmetry New Symmetries breaking: Higgs ? 1. 2. 3. 4. Origin of Matter Unification & gravity Weak scale stability Neutrinos ? nm ne n˜ m W ˜ 0 m m˜ e QuickT ime™ and a T IFF (Uncompressed) decompressor are needed to see this picture. QuickTime™ and a TIFF(Uncompressed) decompressor are needed to see this picture. Qu ickT ime ™ a nd a TIF F (U nco mpre sse d) de com pres sor are nee ded to s ee th is pi cture . Quic kTime™ and a TIFF (Uncompres sed) dec ompressor ar e needed to see this picture. Beyond the SM Qui ckT ime™ and a T IFF (Uncompressed) decompressor are needed to see this picture. SM symmetry (broken) Precision Neutrino Property Studies Mixing, hierarchy, & CPV Daya Bay U e1 U e2 U e 3 U U m1 U m 2 U m 3 U1 U 2 U 3 1 0 0 cosq13 0 ei CP sin q13 cosq12 sin q12 0 1 0 0 i / 2 0 cosq 23 sin q23 0 1 0 0 sin q12 cosq12 0 0 e i CP i / 2ib cosq13 0 0 1 0 0 e 0 sin q 23 cosq 23 e sin q13 0 • proton s nSNS Long baseline site oscillation studies: CPV? Normal or Inverted ? Mini Boone SNS Hall Precision Neutrino Property Studies High energy solar ns Solar Neutrinos DM + EWB Ice Cube EM vs. n luminosity: MNSP KamLAND Borexino unitarity? Solar model? SNO+ LENS Weak decays & new physics SUSYCorrelations models Vud u c t Vcd Vtd d u e n e s u e n e b u e n e nm ne n˜ m ˜ m m˜ ˜ 0 ne d SUSY CKM, (g-2)m, MW, Mpt pe pMn M dW 1 a m˜ L q˜L A n E e En e Ee e u˜ O ~ 0.001 OSM 0 u W Vus Vub d Vcs Vcb s Vts Vtb b ˜ n˜ e e SUSY Non (V-A) x probes (V-A) of Similarly unique Vud from neutron interactions: me/E new physics in muon and decay: LANSCE, pion decay SNS, NIST TRIUMF &RIA? PSI SNS, NIST, LANSCE, Weak Mixing in the Standard Model Parity-violating electron scattering SLAC Moller JLab Future Z0 pole tension Scale-dependence of Weak Mixing Probing SUSY with PV Electron Scattering RPV: No SUSY DM Majorana n s 12 GeV QWP, SUSY / QWP, SM SUSY Loops QuickTime™ and a TIFF (LZW) decompressor are needed to see this picture. E158 QWe, SUSY / QWe, SM 6 GeV gm-2 Muon Anomalous Magnetic Moment m QED m Z Weak Future goal Had VP Had LbL SM Loops QuickTime™ and a TIFF (LZW) decompressor are needed to see this picture. SUSY Loops Quic kTime™ and a TIFF ( LZW) dec ompres sor are needed to s ee this pic ture. New Standard Model Initiative A Road Map • A robust neutrino program: DUSEL (+ exp) & immediate 0nbb • An EDM program: nEDM (SNS), atomic, 2H R&D • Precision Electroweak: PVES, b-decay, gm-2 • Supernova simulation & observation • Cross-disciplinary research support: q13 , DM, CLV • Theory: focus on problems & junior theorists Resources & Benefits Equivalent to a major new initiative: • • • “New Standard Model Initiative” (NSMI) ~ $750m over 10+ years (~$185m non DUSEL) One major new facility (DUSEL) Targeted program at other facilities Benefits to NP: • Make NP a major player in era of historic discovery potential; we can help write the textbook on the new SM • Builds on substantial achievements since 2002 LRP & development of strong groups • Attractive to junior scientists • Economy of resources & synergy with other NP facilities Resources Project Funding for Neutrinos and Fundamental Symmetries Non DUSEL: $184m Total: $748m DUSEL Const: $250m 1 ton 0nbb