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Weakly Interacting Slim Particles (Wisps) Weakly interacting slim particles (WISPs) Theory and phenomenology update Javier Redondo (LMU & MPP München) 1 Outline - MOTIVATION for WISPs ALPs, HPs, ... - GENERALITIES - WHAT’S NEW? 2 Beyond Standard model Universe transparency Flavor Dark Matterstructure Dark Energy Dark Strong CP Anomalous anomalousproblem muon g-2 EW Hierarchy Problem Neutrino masses Quantum Gravity 3 Beyond Standard model Universe transparency Flavor Dark MatterstructureTOP All problems at a time (O(?) New particles...) One problem atEnergy a timeDark Strong CP (O(1) New particles...) Anomalous anomalousproblem muon g-2 EW Hierarchy Problem BOTTOM Neutrino masses Quantum Gravity 3 Hidden Sectors Fields coupled through gravity or HE “messenger” fields... Massive Messengers Standard Model Hidden Sector e−, ν, q, γ, W ±, Z, g...H a, γ, ψMCP... String Theory, SUSY breaking, ... 4 Hidden Sectors can be quite complicated BIG guys Light guys (live in the mountains) (mass is protected by a symmetry) Goldstone Chiral Bosons fermions Gauge and more... Bosons hard to detect; not only as hidden they have suppressed interactions but as hidden, also heavy! light they have no thresholds and they can have maybe at LHC or ILC... coherent forces Let symmetry be our guide ! 5 Hidden Sectors can be quite complicated BIG guys Light guys (live in the mountains) (mass is protected by a symmetry) Goldstone Chiral Bosons WISPsfermions (very) weakly interacting slim Particles Gauge and more... Bosons hard to detect; not only as hidden they have suppressed interactions but as hidden, also heavy! light they have no thresholds and they can have maybe at LHC or ILC... coherent forces Let symmetry be our guide ! 5 There are ``WISPs’’ in the SM ... ! SM Planck scale γ physics g Gravitons γ EW W ± boson SM l ν Neutrinos 6 Symmetries and WISPs 1- Shift symmetries and Goldstone Bosons When a global symmetry is spontaneously broken in the vacuum (i.e. respected by the interactions but not by the vacuum) there appears a massless particle in the spectrum: a Goldstone boson (if it is slightly explicitly broken... then it acquires a little mass-> pseudo) 2- Local U(1)s : Hidden Photons Gauge invariance protects masses of gauge bosons (m=0 for non-abelian group, not for U(1)) Masses can be given by the Stückelberg mechanism Kinetic mixing with the photon is the stronger of all mediator mechanisms (discussed here) (Additional U(1)’s are ubiquitous in PBSM) 3- Chiral sym : Mini-charged Particles/sterile nu’s Chiral symmetries may forbid a mass term for fermions; or protect it. When these particles have interactions with a hidden U(1) that mixes with Photon they appear as mini-charged particles 7 Axion-like particles (ALPs) 0− pseudo Goldstone bosons MAJORONS Global continuous symmetry 0 η spontaneously broken at πη R-AXION FAMILONS high energy scale M a String ‘axions’ DILATONS RADION Sizes and deformations of extra dimensions, MODULI Axiverse! gauge couplings Supersymmetry/supergravity EACH GAUGE GROUP HAS ITS OWN AXION 8 Local U(1)’s: Hidden Photons & kinetic mixing Extra U(1) symmetries are ubiquitous BSM (for instance in String Theory) If the corresponding Hidden photon does not couple to SM particles -> HIDDEN PHOTON γ γ high mass messenger particles Kinetic mixing is the 1 µν most relevant interaction I = χFµν B L −2 at low energies 9 Mini-charged particles (MCPs) Low mass particles charged under the hidden U(1) appear as MCPs γ g Q = h χQh γ e Aternatively, SM charged particles couple directly to HPs γ e γ Qh = χQ gh 10 Generalities 1- stellar WISP emission (VOLUME) νs WISPS? γs (surface) - Stellar constraints are very strong -> very WISP - WISPs can help fitting theory and observations (WDs) 11 Generalities 2- coupling to photons Axion-like Particle α µν Fµν F φ SM Msn φ 8πM α g = γ 2πM γ Hidden Photon 1 χF Bµν −2 µν χ... - Very generic - Advantageous for experimental detection 12 Generalities 3- WISPy cold dark matter (any boson) V (φ) φ - WISPs don’t thermalize!!! - DM set by initial conditions (after Inflation) m φ 2 ρ ρ φ 0 , CDM measured × eV 4.8 1011 GeV F × - ALPs φ 0 π f φ ( M s ) ; HPs ... ?? - Isocurvature constraints 13 Beam Status on ALP searches (as of Jan 2013) Dump 6 LSW SN1987a 8 Solar Ν Helioscopes CAST Telescopes HB 10 1 SN Γburst ALPSII, REAPR IAXO GeV xion 12 Transparency hint YMCE WD cooling hint Coupling axion CDM ADMXHF Log 14 ALP CDM ADMX Haloscopes EBL 16 X axion Rays KSVZ 18 12 10 8 6 4 2 0 2 4 6 Log Mass eV 14 Beam Updates on ALP parameter space Dump 6 LSW SN1987a 8 Solar Ν Helioscopes CAST Telescopes HB 10 1 SN Γburst ALPSII, REAPR IAXO GeV xion 12 Transparency hint YMCE WD cooling hint Coupling axion CDM ADMXHF Log 14 ALP CDM ADMX Haloscopes EBL 16 X axion Rays KSVZ 18 12 10 8 6 4 2 0 2 4 6 Log Mass eV 15 Accumulated hints from White dwarfs (...) Axion emission can accelerate the WD cooling between neutrino and surface dominated cooling periods. a ν a γ , ? e ν¯ Ceme gae Z ≡ fa Period decrease of G117−B15A WD luminosity function Corsico et al. arXiv:1205.6180 Isern et al. arXiv:1204.3565 13 gae/10− 13 2.8 5.6 gae =0, 2.2, 4.5 (10− ) period decrease rate period decrease Number of & Luminosity WDs/ Vol Luminosity 16 Transparency of the universe: lower limits of g! Meyer et al, PRD87 (2013) Transparency of the universe to gamma rays and ALPs Photons can convert into ALPs in galactic or extra galactic magnetic fields and reconvert back close to us Points to ALP photon couplings 11 1 g 10− GeV− φγ ∼ B nG Requires very∼ small ALP masses mφ < neV Challenged by Magnetic-WD constraints! Gill et al. PRD84 (2011) 17 Status on HP searches (as of Jan 2013) 0 0 Jupiter Earth mwLSW Rydberg 3 Coulomb 3 CMB LSW Dark Radiation Sun HB 6 6 Nonzero FIterm Yale Helioscope mixing ADMX ALPSII UWA CERN Cosmology 9 TSHIPS 9 kinetic Cold Dark Matter I line Thermal Log Stückelberg isotropic ckelberg DM anisotropic Stü 12 DPB 12 Hidden Higgs mHh m' Haloscopes 15 15 15 12 9 6 3 0 3 6 Log Mass eV 18 Major updates on HP parameter space Lobanov et al. arXiv:1211.6268 0 0 Jupiter Earth mwLSW Rydberg 3 Coulomb 3 CMB LSW Dark Radiation Sun HB 6 6 Nonzero FIterm Yale Helioscope mixing ADMX ALPSII UWA CERN Cosmology 9 TSHIPS 9 kinetic Cold Dark Matter I line Thermal Log Stückelberg isotropic ckelberg DM anisotropic Stü 12 DPB 12 Hidden Higgs mHh m' DarkHaloscopes Matter 15 15 15 12 9 6 3 0 3 6 Log Mass eV 19 Solar HPs Ann et al. 1302.3884, Redondo & Raffelt (in prep) Production is proportional to photon’s 1 2 4 Γ(γ)=Im χ m K2 Π − 2 2 ReΠL = ωP ;ReΠL = ωP /ZL Ann et al. 1302.3884 ZL 2 4 Γ (γ)=Z ImΠ (γ) χ m L L L (ω2 ω2 )2 +(Z ImΠ )2 − P L K Forgotten renormalization factor is huge for small masses!! 2 2 2 2 ZL = ω /K = ω /m 20 Solar HPs Ann et al. 1302.3884, Redondo & Raffelt (in prep) Production is proportional to photon’s 1 2 4 Γ(γ)=Im χ m K2 Π − 2 2 ReΠL = ωP ;ReΠL = ωP /ZL Ann et al. 1302.3884 ZL 2 4 Γ (γ)=Γ (γ) χ m L L (ω2 ω2 )2 +(ωΓ (γ))2 − P L Forgotten renormalization factor is huge for small masses!! 2 2 2 2 ZL = ω /K = ω /m 21 Solar HPs Φ(γL) Φ(γT ) Boron Neutrino Flux 8 7 s 2 6 cm High Z 6 10 5 Measurements B8 LowZ 4 3 0 1 2 3 4 5 6 Χ m 1012eV Redondo & Raffelt (in prep) This changes many things in the meV range - Helioscopes looking for T-HPs - Dark Radiation - XENON10 Ionization 22 Solar HPs: XENON10 constraints Ann et all [1304.3461] Φ(γL) XENON10 Ionization 1104.3088 1039 1038 " 1037 s 2 1036 1 1035 keV cm 1034 2 2 33 m 10 2 eV Χ 1032 ! Φ Ω 1031 d d 1030 1029 1 10 102 103 104 Ω!eV" 23 Update: New Dark matter experiment proposed 24 Axion - photon mixing in a magnetic field Raffelt, PRD’88 - In a magnetic field one photon polarization Q-mixes with the axion g = aγ F F µν a = g B E a LI 4 µν − aγ · Not axions, nor photons are propagation eigenstates! - Equations of motion can be easily diagonalised 2 2 10 0 gaγ B ω A 0 (ω k ) + − |2 | || = . − 01 gaγ B ω m a 0 − | | a k - Dark matter solution v = ; ω m (1 + v2/2+...) ω a A χ || − exp( i(ωt kz)). a ∝ 1 − − DM ggaaγγ BB It has a small E field! χχ || || ∼∼ mmaa 25 Radiation from a magnetised mirror Horns et al , JCAP04(2013)016 Ea = ωaχ cos(ωat + kz). magnetic field Eγ + Ea =0 |z=zmirror E = ω χ cos(ω (t z)). γ − a γ − 2 Photons radiated from the mirror with ωγ = ωa = ma(1 + v /2) Note: measuring these photons, we measure the TOTAL DM energy, DM mass and the velocity distribution! also with directional sensitivity! 26 Cavity searches (haloscopes) Sikivie PRL ‘83 - Use two facing mirrors (simplistic resonant cavity in 1D) 10 resonant ωγ L π +2πn detector 5 ? 5 10 transmission coefficient t dark matter distribution 1/t 8 ∼ 2 δω v 6 10− 6 ω ∼ 2 ∼ δω t2 4 ω ∼ ωL chose out amplitude 2 maL = π large 2 4 6 8 10 1/t 2 6 ω[1/πL] t 10− ∼ 27 Dish antenna searches (broadband!) Horns et al , JCAP04(2013)016 nice shielding - Mirror radiation is perpendicular to the mirror’s surface (emitted coherently from the surface!) spherical dish - concentrate emission using a spherical dish antenna! ? background magnetic field Comparing both methods..
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