Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014 Dark Matter Axion Dark Matter Georg G. Raffelt, Max-Planck-Institut für Physik, München Physics Colloquium, University of Sydney, 3 March 2014

Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014 Axions as Cold Dark Matter of the Universe Dark Energy ~ 70% Dark Energy ~ 70% (Cosmological Constant) (Cosmological Constant) Neutrinos Neutrinos 0.1  2% 0.1  2% Dark Matter ~ ~ 25% ~ Ordinary Matter ~ 5% (of this only about 10% luminous)

Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014 Neutron Proton Gravitation (Gravitons?) Weak Interaction (W and Z Bosons) Periodic System of Elementary Particles Electromagnetic Interaction (Photon) Strong Interaction (8 Gluons) Down Strange Bottom Electron Muon Tau e-Neutrino  -Neutrino  -Neutrino   e e   d s b 1 st Family 2 nd Family 3 rd Family Up Charm Top u c t QuarksLeptons Charge  1/3 Down Charge  1 Electron Charge 0 e-Neutrino e ed Charge +2/3 Up u Higgs

Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014 Supersymmetric Extension of Particle Physics In supersymmetric extensions of the particle-physics standard model, every boson has a fermionic partner and vice versa SpinSuperpartner 0 1/2 3/2 Higgsino Gravitino 1/2 Leptons (e, e, …) Quarks (u, d, …) 1 Gluons W  Z 0 Photon (  ) 0 2 Higgs Graviton SpinStandard particle If R-Parity is conserved, the lightest SUSY-particle (LSP) is stable Most plausible candidate for dark matter is the neutralino, similar to a massive Majorana neutrino Neutralino = C 1 Photino + C 2 Zino + C 3 Higgsino

Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014 Laboratory Searches for WIMP Dark MatterEnergydeposition Recoil energy (few keV) is measured by Ionisation Scintillation Cryogenic Galactic dark matter particle (e.g. neutralino)

Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014 WIMP Searches (Underground Physics) COUPP PICASSO XENON LUX, ZEPLIN WARP, ArDM DEAP/CLEAN DAMA/LIBRA KIMS, XMASS DRIFT GERDA CDMS EDELWEISS CRESST ROSEBUD Heat Phonons ChargeLight

Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014 WIMP Cross Section Limits 2014 Klaus Eitel, 2014

Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014 High- and Low-Energy Frontiers in Particle Physics eV Planck mass GUT scale Electroweak scale QCD scale Cosmological constant WIMP dark matter (related to EW scale, perhaps SUSY) Axion dark matter (related to Peccei-Quinn symmetry) Accelerator Frontier CERN

Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014 Axion Physics in a Nut Shell CP conservation in QCD by Peccei-Quinn mechanism For f a ≫ f  axions are “invisible” and very light  Axions a ~  0 m  f   m a f a   a Particle-Physics Motivation Axions thermally produced in stars, e.g. by Primakoff production Limits from avoiding excessive energy drain Solar axion searches (CAST, Sumico) a  Solar and Stellar Axions In spite of small mass, axions are born non-relativistically (non-thermal relics) Cold dark matter candidate m a ~ 10  eV (or much smaller or larger) CosmologySearch for Axion Dark Matter S N  a B ext Microwave resonator (1 GHz = 4  eV) Primakoff conversion ADMX-LF (UW Seattle) ADMX-HF (Yale)

Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014 CP Violation in Particle Physics Physics Nobel Prize 2008 Discrete symmetries in particle physics C – Charge conjugation, transforms particles to antiparticles violated by weak interactions P – Parity, changes left-handedness to right-handedness violated by weak interactions T – Time reversal, changes direction of motion (forward to backward) CPT – exactly conserved in quantum field theory CP – conserved by all gauge interactions violated by three-flavor quark mixing matrix M. Kobayashi T. Maskawa  All measured CP-violating effects derive from a single phase in the quark mass matrix (Kobayashi-Maskawa phase), i.e. from complex Yukawa couplings  Cosmic matter-antimatter asymmetry requires new ingredients

Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014 The CP Problem of Strong Interactions Real quark mass Phase from Yukawa coupling Angle variable Remove phase of mass term by chiral transformation of quark fields

Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014 Neutron Electric Dipole Moment Violates time reversal (T) and space reflection (P) symmetries Natural scale Experimental limit Limit on coefficient

Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014 Strong CP Problem Equivalent

Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014 The Pool Table Analogy (Pierre Sikivie 1996) Gravity Symmetric relative to gravity Pool table New degree of freedom  Axion (Weinberg 1978, Wilczek 1978) Axis Symmetry dynamically restored (Peccei & Quinn 1977) Symmetry broken Floor inclined fafa

Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March Years of Axions

Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014 The Cleansing Axion Frank Wilczek “I named them after a laundry detergent, since they clean up a problem with an axial current.” (Nobel lecture 2004)

Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014 Axion Bounds and Searches [GeV] f a eVkeVmeV  eV mama neV Directsearches Too much CDM (misalignment) (misalignment) TelescopeExperiments Globular clusters (a-  -coupling) SN 1987A Too many events Too much energy loss Too much hot dark matter CAST ADMX (Seattle & Yale) Globular clusters (He ignition), WD cooling (a-e coupling) Too much cold dark matter (re-alignment with  i = 1) Classic region Anthropic region

Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014 Dark Energy ~ 70% Dark Energy ~ 70% (Cosmological Constant) (Cosmological Constant) Neutrinos Neutrinos 0.1  2% 0.1  2% Dark Matter ~ ~ 25% ~ Ordinary Matter ~ 5% (of this only about 10% luminous) Axions as Cold Dark Matter of the Universe

Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014 Creation of Cosmological Axions Axions are born as nonrelativistic, classical field oscillations Very small mass, yet cold dark matter

Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014 Axion Cosmology in PLB 120 (1983)

Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014 Killing Two Birds With One Stone Peccei-Quinn mechanism Solves strong CP problem Provides dark matter in the form of axions

Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014 Cosmic Axion Density Modern values for QCD parameters and temperature-dependent axion mass imply (Bae, Huh & Kim, arXiv: )

Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014 Axion Production by Domain Wall and String Decay

Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014 BEC Formation ~ 100 citations

Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014 High- and Low-Energy Frontiers in Particle Physics eV Planck mass GUT scale Electroweak scale QCD scale Cosmological constant WIMP dark matter (related to EW scale, perhaps SUSY) Axion dark matter (related to Peccei-Quinn symmetry) Accelerator Frontier CERN

Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014 Searching for Solar Axions Searching for Axion-Like Particles

Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014 Experimental Tests of Invisible Axions Pierre Sikivie: Macroscopic B-field can provide a large coherent transition rate over a big volume (low-mass axions) Axion helioscope: Look at the Sun through a dipole magnet Axion haloscope: Look for dark-matter axions with A microwave resonant cavity

Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014 Search for Solar Axions  a Sun Primakoff production Axion Helioscope (Sikivie 1983)  Magnet S N a Axion-Photon-Oscillation  Tokyo Axion Helioscope (“Sumico”) (Results since 1998, up again 2008)  CERN Axion Solar Telescope (CAST) (Data since 2003) Axion flux Alternative technique: Bragg conversion in crystal Experimental limits on solar axion flux from dark-matter experiments (SOLAX, COSME, DAMA, CDMS...)

Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014 Tokyo Axion Helioscope (“Sumico”) Moriyama, Minowa, Namba, Inoue, Takasu & Yamamoto PLB 434 (1998) 147 Inoue, Akimoto, Ohta, Mizumoto, Yamamoto & Minowa PLB 668 (2008) 93

Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014 CAST at CERN

Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014 Recent “shining-light-through-a-wall” or vacuum birefringence experiments: ALPS BMV BFRT GammeV LIPPS OSQAR PVLAS Photon Regeneration Experiments Ehret et al. (ALPS Collaboration), arXiv: (DESY, using HERA dipole magnet) (Laboratoire National des Champs Magnétiques Intens, Toulouse) (Brookhaven, 1993) (Fermilab) (Jefferson Lab) (CERN, using LHC dipole magnets) (INFN Trieste)

Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014 Shining TeV Gamma Rays through the Universe Figure from a talk by Manuel Meyer (Univ. Hamburg)

Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014 Parameter Space for Axion-Like Particles Invisible axion (DM) Axion Line Invisible axion (DM) Axion Line HB Stars Invisible axion (DM) Axion Line HB Stars CAST Solar Axions Invisible axion (DM) Axion Line HB Stars Laser Experiments CAST Solar Axions TeV  rays How to make progress?

Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014 Next Generation Axion Helioscope (IAXO) at CERN Irastorza et al.: Towards a new generation axion helioscope, arXiv: Armengaud et al.: Conceptual Design of the International Axion Observatory (IAXO), arXiv:

Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014 Searching for Axion Dark Matter Searching for Axion Dark Matter

Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014 Search for Galactic Axions (Cold Dark Matter) Power Frequency mama Axion Signal Thermal noise of cavity & detector Power of galactic axion signal Microwave Energies (1 GHz  4  eV) Dark matter axions Velocities in galaxy Energies therefore m a = 1  100  eV v a  10  3 c E a  (1  10  6 ) m a Axion Haloscope (Sikivie 1983) B ext  8 Tesla Microwave Resonator Q  10 5 Primakoff Conversion  a B ext Cavity overcomes momentum mismatch

Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014 Axion Dark Matter Experiment (ADMX), Seattle Adapted from Gianpaolo Carosi

Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014 SQUID Microwave Amplifiers in ADMX Adapted from Gianpaolo Carosi

Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014 Axion Dark Matter Searches 1. Rochester-Brookhaven- Fermilab, PRD 40 (1989) University of Florida PRD 42 (1990) US Axion Search ApJL 571 (2002) L27 4. CARRACK I (Kyoto) hep-ph/ Limits assuming axions are the galactic dark matter with standard halo KSVZ DFSZ ADMX-LF (Seattle) search range (2015+)

Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014 ADMX-HF at Yale (Steve Lamoreaux Group) Design of cavity & magnet Dilution refrigerator above & below deck ADMX-HF will also be a test-bed for innovative concepts, e.g. thin-film superconducting cavities Adapted from Karl van Bibber

Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014 WISPDMX at DESY and MPIfR 208 MHz microwave cavities H1 detector Microwave cavities: HERA – 50, 208, 500 MHz 208 MHz cavity: resonant modes at 199, 295, 433, 524, 579, 707, 765, 832 MHz Magnets: DESY H1 1.1 T (solenoid), HERA 5 T (dipole), Receiver technology: MPIfR, T n ~ 100 K Phase 1,2 – searches using available facilities Phase 3 – advanced searches with specially designed facilities

Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014 Broadband Approaches TOKAMAK Facility B [T] V [m 3 ] B 2 V [T 2 m 3 ] ToreSupra JET ITER MPP ASDEX TEXTOR Microwave cavity experiment B [T] V [m 3 ] B 2 V [T 2 m 3 ] ADMX WISPDMX Horns et al. 2013

Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014 Center for Axion and Precision Physics (CAPP) New Institute for Basic Science (IBS), Korea The plan is to launch a competitive Axion Dark Matter Experiment in Korea, participate in state- of-the-art axion experiments around the world, play a leading role in the proposed proton electric-dipole-moment (EDM) experiment and take a significant role in storage-ring precision physics involving EDM and muon g–2 experiments. 15 Oct 2013 Yannis Semertzidis

Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014 What if the axion is found?

Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March D Infall and the Folding of Phase Space

Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014 Fine Structure in the Axion Spectrum Axion distribution on a 3-dim sheet in 6-dim phase space Is “folded up” by galaxy formation Velocity distribution shows narrow peaks that can be resolved More detectable information than local dark matter density P.Sikivie & collaborators

Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014 Axion Bounds and Searches [GeV] f a eVkeVmeV  eV mama neV Directsearches Too much CDM (misalignment) (misalignment) TelescopeExperiments Globular clusters (a-  -coupling) SN 1987A Too many events Too much energy loss Too much hot dark matter CAST ADMX (Seattle & Yale) Globular clusters (He ignition), WD cooling (a-e coupling) Too much cold dark matter (re-alignment with  i = 1) Classic region Anthropic region

Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014 Oscillating Neutron EDM by Axion Dark Matter Oscillating axion field (DM) → Oscillating   term → Oscillating neutron EDM

Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014 Searching for Axions in the Anthropic Window Graham & Rajendran, arXiv: Budker, Graham, Ledbetter, Rajendran & Sushkov, arXiv: CASPEr experiment Precise magnetometry to measure tiny deviations from Larmor frequency

Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014 Cosmic Axion Spin Precession Experiment (CASPEr) Budker, Graham, Ledbetter, Rajendran & Sushkov, arXiv: Time-varying nucleon EDM caused by axion DM in Lead Titanate magnetometer Phase I Phase II Magnetometer noise limit

Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014 Helmholtz Institute Mainz (HIM) Building under construction New institute on Structure, symmetry and stability of matter and antimatter Dmitry Budker Moving from Berkeley to HIM Plans to pursue CASPEr

Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014 Dow Jones Index of Axion Physics inSPIRE: Citation of Peccei-Quinn papers or title axion (and similar)

Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014 Pie Chart of Dark Universe Dark Energy ~ 70% Dark Energy ~ 70% (Cosmological Constant) (Cosmological Constant) Neutrinos Neutrinos 0.1  2% 0.1  2% Dark Matter ~ ~ 25% ~ Ordinary Matter ~ 5% (of this only about 10% luminous)