Theory and Phenomenology of WISPs

Transcription

1 Theory and Phenomenology of WISPs very weakly interacting Sub-eV particles Javier Redondo Deutsches Elektronen Synchrotron (DESY) A review of the accomplishments of SFB 676 C1 project Project Leader: Andreas Ringwald

2 step ahead: from `standard to BSM WISPs (WISP for weakly interacting sub-ev particle) Extremely energetic cosmic neutrinos Not merely a C project, A and B also present!

3 Hidden Sectors Extensions of SM often include Hidden Sectors Fields coupled to SM only through gravity or high energy messenger fields... This is the case in string theory (compactifications produce many particles, new gauge symmetries, and KKs) Desirable for SUSY Also in GUT theories... Massive Messengers Standard Model Hidden Sector e, ν, q, γ, W ±, Z, g...h a, γ, ψ MCP...

4 Hidden Sectors can be quite complicated we certainly don t know much! Hidden Sector BIG guys Light guys (live in the mountains) (mass is protected by a symmetry) Goldstone Bosons Chiral fermions Gauge Bosons and more... hard to detect; not only hidden, also heavy! maybe at LHC or ILC... as hidden they have suppressed interactions but as light they have no thresholds and they can have coherent forces study couplings to photons to exploit coherence

5 U(1) Symmetries and weakly interacting sub ev particles (WISPs) 1- Global U(1)s and ALPs (axion-like-particles) Standard Model Msn φ Hidden Sector F µν F µν 1 M φ SSB implies a massless Goldstone boson (small explicitly breaking implies small mass-> pseudo) F µν F µν 1 M φ dilaton-like coupled scalars have similar phenomenological aspects but generate 5th forces (not for chameleons) 2- Local U(1)s : Hidden Photons Masses can be given by the Stückelberg mechanism Kinetic mixing not med-mass suppressed (Additional U(1) s are ubiquitous in PBSM) Standard Photon Msn loop Hidden Photon 3- Chiral sym : Mini-charged Particles Particles in a a hidden sector charged under a hidden U(1) that mixes with Photon appear as mini-charged particles

6 Hidden Photons: photon oscillations and mod. Coulomb law 1 4 A µνa µν + ej µ A µ sin χ 2 A µνb µν A µ õ sin χb µ õ χb µ L. B. Okun. Sov. Phys. JETP, 56:502, B µνb µν m2 γ B µ B µ 1 4õνõν ej µ (õ χb µ ) Flavor eigenstate 1 4 B µνb µν m2 γ B µ B µ mass eigenstates Modified Coulomb potential V (r) = α r [ cos 2 χ + sin 2 χexp m γ r ] P A S = sin 2 2χ sin 2 m2 γ L 4ω photon-hidden photon Oscillation probability

7 C1 accomplishments Theory Brainstoming and Calculationshop: The physics case for the low energy frontier (11-14 June 2008, DESY Hamburg) White Paper in preparation: -The physics case for a low energy frontier of fundamental physics, S. Abel et al. - Kinetic Mixing of the Photon with Hidden U(1)s in String Phenomenology. A. Ringwald et at. JHEP 0807:124, Probing Hidden Sector Photons through the Higgs Window. Ahlers et al. Phys.Rev.D78:075005,2008. Astrophysics and Cosmology -Helioscope Bounds on Hidden Sector Photons. JCAP 0807:008, New Constraints on Hidden Photons using Very High Energy Gamma-Rays from the Crab Nebula. AIP Conf.Proc.1085: , Hidden gauginos of an unbroken U(1): Cosmological constraints and phenomenological prospects. JCAP 0901:003, Signatures of a hidden cosmic microwave background. Phys.Rev.Lett.101:131801, Microwave Background Constraints on Mixing of Photons with Hidden Photons. JCAP. -Massive hidden photons as lukewarm dark matter. JCAP 0902:005,2009. Laboratory experiments -Alpenglow - A Signature for Chameleons in Axion-Like Particle Search Experiments. Phys.Rev.D77:015018, Light from the hidden sector. Phys.Rev.D76:115005, Laser experiments explore the hidden sector. Phys.Rev.D77:095001, On search for ev hidden sector photons in Super- Kamiokande and CAST experiments. Phys.Lett.B664: , Searching Hidden-sector Photons inside a Superconducting Box. Europhys.Lett.84:31002,2008 -A Cavity Experiment to Search for Hidden Sector Photons. Phys.Lett.B659: ,2008 -Mixing of photons with massive spin-two particles in a magnetic field. Phys.Rev.D79:015012, The Discovery Potential of Laser Polarization Experiments. arxiv: [hep-ph]

8 Brainstorming and Calculationshop Bottom-up Top-bottom WISPs in BSM, (extra dimensions, string theory...)

9 Brainstorming and Calculationshop Bottom-up Top-bottom

10 Brainstorming and Calculationshop Bottom-up Top-bottom

11 Brainstorming and Calculationshop Bottom-up Top-bottom

12 Top-bottom Bottom-up Brainstorming and Calculationshop

13 Top-bottom Bottom-up Brainstorming and Calculationshop

14 Top-bottom Bottom-up Brainstorming and Calculationshop

15 Top-bottom Bottom-up Brainstorming and Calculationshop

16 Brainstorming and Calculationshop: upcoming White paper!

17 Phenomenology of Hidden Photons STATUS before C1 `a picture s worth more than 1000 words, `, `Un bon croquis vaut mieux qu'un long discours, etc... 1 Jupiter Earth Rydberg EW 3 Coulomb 5 Sun Log 10 Χ 7 9 LSW Log 10 m Γ' ev

18 Phenomenology of Hidden Photons STATUS after C1! `a picture s worth more than 1000 words, `, `Un bon croquis vaut mieux qu'un long discours, etc... 1 Jupiter Earth Rydberg EW 3 Coulomb Log 10 Χ CMB FIRAS hcmb CAST LSW Solar Lifetime HB ddm Log 10 m Γ' ev

19 Photon-Hidden Photon resonant oscillations in plasmas new bounds are based on photon-hidden photon oscillations in either stellar or primordial plasmas where the photon self-energy is modified by refraction and absorption phenomena are pretty similar to neutrino oscillations in dense matter, with the exception that here one of the oscillating flavors (the photon) interacts strongly with the plasma In particular Mikheev-Smirnov-Wolfenstein (MSW) transitions do occur m γ = m γ m γ1,2 The hidden photon mass determines the time/position of the production in the early universe or in a star photon `mass, plasma density Cosmological time Stellar radius

20 Phenomenology of Hidden Photons `a picture s worth more than 1000 words, `, `Un bon croquis vaut mieux qu'un long discours, etc kev HPs with 10^-12 mixing reproduce the correct DM abundance (are (are produced around just BBN) before -testable- BBN) 1 ev T [kev ] mev 1 mev mev HPs with 10^-6 mixing are produced between BBN and CMB decoupling χ CMB Γ H = 1 1 kev BBN 1 MeV

21 Phenomenology of Hidden Photons `a picture s worth more than 1000 words, `, `Un bon croquis vaut mieux qu'un long discours, etc... Log 10 Χ Jupiter Earth CMB Coulomb FIRAS hcmb CAST LSW Rydberg Solar Lifetime EW kev HPs with 10^-12 mixing reproduce the correct DM abundance (are (are produced around just BBN) before -testable- BBN) 1 ev T [kev ] HB ddm Log 10 m Γ' ev χ mev HPs with 10^-6 mixing are produced between BBN and CMB decoupling CMB 0.1 mev 1 mev Γ H = 1 1 kev BBN 1 MeV

22 Late cosmology the mev Valley: Hidden CMB! For low χ only resonance is relevant Oscillations transfer energy from photons to hidden photons x ρ γ ρ γ Photon temperature readjusted after T after = (1 x) 1/4 T before but standard neutrinos untouched so its temperature relative to photons is increased! Χ CMB decoupling H meV 0.1meV mev 10 mev Big Bang Nucleosynthesis Finally: N eff ν (x) = N ν 1 x x 1 x ( ) 4/ Our computation T kev x = χ 2 χ <

23 BBN results (PDG) Assume N ν = η BBN = CMB results (Steigman) (WMAP5+otherCMB+LSS+SN+HST) η CMB = N eff ν = CMB results (Hamann) (WMAP3+...+SDSS+Ly-alpha) N eff ν =

24 Cosmological Constraint on the Effective Number of Neutrino Species K. Ichikawa arxiv: v1 [astro-ph]

25 BBN results (PDG) Assume N ν = η BBN = CMB results (Steigman) (WMAP5+otherCMB+LSS+SN+HST) N eff < 4.8 ν η BBN > 0.75 η CMB η CMB = N eff ν = CMB results (Hamann) (WMAP3+...+SDSS+Ly-alpha) N eff ν = x < 0.2 x < 0.32

26 BBN results (PDG) Assume N ν = η BBN = CMB results (Steigman) (WMAP5+otherCMB+LSS+SN+HST) η CMB = N eff ν = CMB results (Hamann) (WMAP3+...+SDSS+Ly-alpha) N eff ν = values suggest 1.6 central x 0.1 Take it as the biggest surprise one can face!

27 massive Hidden photons and the mev Valley χ Coulomb BBNvsCMB CAST L γ L too much energy loss! FIRAS m γ [ev] 10 8

28 Experimental Opportunities at the mev Valley to explore further the parameter space, and in particular the suggestive mev we can arrange laboratory experiments: -Light-shining-through-walls (the ALPS experiment) -LSW with radio Cavities -Magnetic field leaking through Superconducting shielding -Solar Hidden photon searches: CAST, SK, SHIPS

29 Laboratory experiments: Light-Shinning-though-walls A µ S µ S µ A µ Laser as intense/controlled source: A pioneer experiment BFRT (BNL) in early 90 s and 2005 boom: ALPS (DESY), BMV (LNCMP), GammeV (FL), LIPPS (jlab), OSQAR (CERN) Axion Like Particle Search or better ``Any-light-particle-search Resonant cavity L 6 m, ω 2 ev P 300 Watt, B 20 mhz P 10 4 Watt, B 20 mhz photon regeneration LSW probability 16χ 4 sin 2 m2 γ L 1 m2γ L 2 4ω sin2 4ω

30 Laboratory experiments: Light-Shinning-though-walls Axion Like Particle Search or better ``Any-light-particle-search Resonant cavity L 6 m, ω 2 ev P 300 Watt, B 20 mhz P 10 4 Watt, B 20 mhz photon regeneration LSW probability to cover this region Χ 16χ 4 ( m 2 γ L 4ω ) 4 decrease ω enlarge L Coulomb ALPS sens BMV GammeV LIPSS ALPS prospects Sun & CAST m Γ' ev

31 Laboratory experiments: LSW with RF cavities Use Radio frequency cavities for emission and detection! Superconducting cavities boost the detection efficiency by a huge quality factor ( 10 11?!) Resonant cavity small frequency much smaller photon energy implies sensitivity to smaller masses!

32 Laboratory experiments: field through a wall `photon regeneration LSW probability 16χ 4 sin 2 m2 γ L 1 m2γ L 2 4ω sin2 4ω production χ 2 and detection χ 2 of real photons `field regeneration amplitude B e MLondond + χ 2 ( 1 e m B γ r ) Χ m Γ' ev

33 Solar Hidden Photons X

34 Solar Hidden Photons X

35 Solar Hidden Photon detection Shield absorbs the photon component B = S X χa A S(r) S(R ) = B S A oscillations

36 Solar Hidden Photons: CAST, SuperK and SHIPS Spectrum of mev mass solar Hidden Photons peaks at low energies (most of the emission comes from the external shells, just below the photosphere) χ 2 m 4 γ γ cm 2 s ev F Ω ev

37 Solar Hidden Photons: CAST, SuperK and SHIPS cern solar axion telescope, LHC dipole 10 m length, 9 T, tracking the Sun sunrise and sunset great sensitivity to kev photons CAST kev 10 5 Proposals: Coulomb LSW DONE Χ CASYeV parallel vacuum vessel, bigger aperture, visible photon detector -SuperK data, photon-hp oscillations inside the shadow PMTs 10 7 CAST ev SuperK SHIPS (SOLAR HIDDEN PHOTON SEARCH) m Γ' ev 10 8

38 Solar Hidden Photons: CAST, SuperK and SHIPS cern solar axion telescope, LHC dipole 10 m length, 9 T, tracking the Sun sunrise and sunset great sensitivity to kev photons Proposals: -CASYeV parallel vacuum vessel, bigger aperture, visible photon detector Χ Coulomb LSW CAST kev DONE SuperK data, photon-hp oscillations inside the shadow PMTs CAST ev -SHIPS (SOLAR HIDDEN PHOTON STERNWARTE (G. Wiedeman proposal) 10 7 SuperK m Γ' ev 10 8

39 Solar Hidden Photons: CAST, SuperK and SHIPS cern solar axion telescope, LHC dipole 10 m length, 9 T, tracking the Sun sunrise and sunset great sensitivity to kev photons... Proposals: -CASYeV parallel vacuum vessel, bigger aperture, visible photon detector Χ Χ Coulomb CAST CAST kev Coulomb 10 6 LSW LSW DONE SuperK data, photon-hp oscillations inside the shadow PMTs hcmb CAST ev SHIPS -SHIPS (SOLAR HIDDEN PHOTON STERNWARTE (G. Wiedeman proposal) m Γ' ev SuperK m Γ' ev 10 8

40 Conclusions -C1 -> Theory and phenomenology of WISPs -an A,B,C project -Enormous success in its first 1 1/2 year, in theory, phenomenology (cosmo and astro) -Experiments ongoing and more proposed