Science Case for / Physics Goals of ALPS-II.

Slides:



Advertisements
Similar presentations
The Higgs boson What it is: 1) barroom explanation 2) more, with some pictures 3) yet more, with some formulas Plus pictures related to the discovery John.
Advertisements

Kiwoon Choi PQ-invariant multi-singlet NMSSM
An intruder in the neutrino school and to finish...THE AXION CAST: The CERN Axion Solar Telescope Iñaki Ortega ISAPP 2013 LSC, Canfranc.
Dark Energy and Quantum Gravity Dark Energy and Quantum Gravity Enikő Regős Enikő Regős.
String theoretic QCD axions in the light of PLANCK and BICEP2 (QCD axion after BICEP2) Kiwoon KIAS, May 1, 2014 KC, K.S. Jeong and M.S. Seo, arXiv:
The minimal B-L model naturally realized at TeV scale Yuta Orikasa(SOKENDAI) Satoshi Iso(KEK,SOKENDAI) Nobuchika Okada(University of Alabama) Phys.Lett.B676(2009)81.
Higgs Boson Mass In Gauge-Mediated Supersymmetry Breaking Abdelhamid Albaid In collaboration with Prof. K. S. Babu Spring 2012 Physics Seminar Wichita.
Why we need Lab Experiments to search for Alps Joerg Jaeckel 1 E. Masso, J. Redondo 2 F. Takahashi, A. Ringwald 1 1 DESY 2 Universitat Autonoma de Barcelona.
Andreas Ringwald (DESY) HAP Dark Matter 2013, Universität Münster, Münster, Germany February 2013 Axions and Axion-Like Particles in the Dark Universe.
CMB Constraints on Mini-charged Particles Clare Burrage (DESY) arXiv: with J. Jaeckel, J. Redondo & A. Ringwald.
Dark Energy and Void Evolution Dark Energy and Void Evolution Enikő Regős Enikő Regős.
Andreas Ringwald, DESY 27 th DESY PRC Closed Session, DESY, Hamburg, 26 October 2011 Towards a comprehensive summary Physics Case for WISP Searches.
Richard Howl The Minimal Exceptional Supersymmetric Standard Model University of Southampton UK BSM 2007.
Chiral freedom and the scale of weak interactions.
The Ideas of Unified Theories of Physics Tareq Ahmed Mokhiemer PHYS441 Student.
Chiral freedom and the scale of weak interactions.
Searches for New Physics Motivations Examples Searches so far Setting scene for LHC 1/12.
1 New Frontiers in Particle Physics Jeff Forshaw University of Manchester.
Andreas Ringwald (DESY) PASCOS 2012, Merida, Mexico, 3-8 June 2012 Searching for axions and ALPs from string theory.
Quintessino model and neutralino annihilation to diffuse gamma rays X.J. Bi (IHEP)
Cosmological Vacuum Selection and Meta-Stable Susy Breaking Ioannis Dalianis IFT-University of Warsaw.
String theoretic QCD axions in the light of PLANCK and BICEP2 Kiwoon CosKASI Conference, April 16, 2014 KC, K.S. Jeong and M.S. Seo, arXiv:
A.F.Kord Sabzevar Tarbiat Moallem University (Iran) September 2011.
Relic Neutrinos as a Source of Dark Energy Neal Weiner New York University IDM04 R.Fardon, D.B.Kaplan, A.E.Nelson, NW What does dark energy have to do.
Center for theoretical Physics at BUE
 It would appear that there is more matter in the universe, called dark matter, than we see. We believe this because  The edges of galaxies are rotating.
Axel Lindner, DESY An experimental Expedition into a new Particle Habitat at smallest Masses Cosmology Meets Particle Physics, DESY Theory Workshop, 28.
Dark Matter and Dark Energy from the solution of the strong CP problem Roberto Mainini, L. Colombo & S.A. Bonometto Universita’ di Milano Bicocca Mainini.
Relic Neutrinos, thermal axions and cosmology in early 2014 Elena Giusarma arXiv: Based on work in collaboration with: E. Di Valentino, M. Lattanzi,
Low scale gravity mediation in warped extra dimensions and collider phenomenology on sector hidden sector LCWS 06, March 10, Bangalore Nobuchika.
24 Sep 2013 DaMaSC 2 Feng 1 DARK MATTER AND ITS PARTICLE PROPERTIES Jonathan Feng, UC Irvine Dark Matter in Southern California (DaMaSC 2) Keck Institute.
Axion and anomalous U(1) gauge symmetry Axion and anomalous U(1) gauge symmetry in string theory in string theory Kiwoon Choi (KAIST) ASK 2011 Apr.11 –
Supersymmetric Models with 125 GeV Higgs Masahiro Yamaguchi (Tohoku University) 17 th Lomonosov Conference on Elementary Particle Physics Moscow State.
The Universe  What do we know about it  age: 14.6 billion years  Evolved from Big Bang  chemical composition  Structures.
DARK MATTER CANDIDATES Cody Carr, Minh Nguyen December 9 th, 2014.
1 Supersymmetry Yasuhiro Okada (KEK) January 14, 2005, at KEK.
Low scale supergravity mediation in brane world scenario and hidden sector phenomenology Phys.Rev.D74:055005,2006 ( arXiv: hep-ph/ ) ACFA07 in Beijing:
Strong fields and recycled accelerator parts as a laboratory for fundamental physics Joerg Jaeckel † M. Ahlers *,H. Gies x, J. Redondo**, A. Ringwald **
Theoretical Issues in Astro Particle Physics J.W. van Holten April 26, 2004.
Large extra dimensions and CAST Biljana Lakić Rudjer Bošković Institute, Zagreb Joint ILIAS-CAST-CERN Axion Training, , CERN Joint ILIAS-CAST-CERN.
Neutrino mass and DM direct detection Daijiro Suematsu (Kanazawa Univ.) Erice Sept., 2013 Based on the collaboration with S.Kashiwase PRD86 (2012)
Cosmological mass bounds on hot-dark matter axions Alessandro MIRIZZI (MPI, Munich) NOW Neutrino Oscillation Workshop Conca Specchiulla, September.
CONSTRAINED MSSM AND RECENT ASTROPHYSICAL DATA Alexey Gladyshev (JINR, Dubna & ITEP, Moscow) SEMINAR AT KEK THEORY GROUP November 1, 2004.
Results and perspectives of the solar axion search with the CAST experiment Esther Ferrer Ribas IRFU/CEA-Saclay For the CAST Collaboration Rencontres de.
DYNAMICAL GENERATION OF FERMION MASSES AND ITS CONSEQUENCES Jiří Hošek Department of Theoretical Physics Nuclear Physics Institute Rez (Prague) Czech Republic.
Supersymmetric B-L Extended Standard Model with Right-Handed Neutrino Dark Matter Nobuchika Okada Miami Fort Lauderdale, Dec , 2010 University.
“Planck 2009” conference Padova May 2009 Facing Dark Energy in SUGRA Collaboration with C. van de Bruck, A. Davis and J. Martin.
J. KalinowskiDark matter in U(1) extended SUSY1 Dark matter in the U(1) extended supersymmetric model Jan Kalinowski S.Y. Choi, H.E. Haber and P.M. Zerwas,
Durmu ş Ali Demir İ zmir Institute of Technology Reasons for … Results from … Extra U(1) in SUSY.
Georg Raffelt, MPI Physics, Munich IAXO Workshop, INFN Frascati, 18–19 April 2016 Axion Landscape Solar Axions Supernova 1987A Dark Matter Long-Range Force.
Klein Particles in the Universe Oscar Klein Memorial Lecture 2008 Helen R. Quinn SLAC.
Any Light Particle Search – ALPS II Natali Kuzkova Ph.D. student, DESY PIER PhD seminar 20 th January, 2015.
Derek F. Jackson Kimball. Collaboration Dmitry Budker, Arne Wickenbrock, John Blanchard, Samer Afach, Nathan Leefer, Lykourgas Bougas, Dionysis Antypas.
New constraints on light bosons from the high energy universe Denis WOUTERS Service de Physique des Particules Supervisor: Pierre BRUN D. Wouters and P.
Andreas Ringwald (DESY) Physics of fundamental Symmetries and Interactions - PSI2013 Paul-Scherrer-Institut, Villigen, CH 8-12 September 2013 Fundamental.
Konstantinos Dimopoulos Lancaster University Work done with: Sam Cormack arXiv: [astro-ph.HE]
1-2 Mass Degeneration in the Leptonic Sector Hiroyuki ISHIDA (Tohoku University) Collaboration with : Takeshi ARAKI (MISC) Ref ; T. Araki and H.I. arXiv.
A model for large non-standard interactions of neutrinos leading to the LMA-dark solution Yasaman Farzan IPM, Tehran.
The CAST Experiment A search for Solar Axions Jaime Ruz Armendáriz, LFNAE, Zaragoza University On behalf of the CAST Collaboration CASTCAST.
Topics on Dark Matter Annihilation
Axion Electrodynamics
and now for something completely different...
The Dark Universe Susan Cartwright.
An interesting candidate?
dark matter Properties stable non-relativistic non-baryonic
The symmetry of interactions
The MESSM The Minimal Exceptional Supersymmetric Standard Model
Marco Roncadelli, INFN – Pavia (Italy)
Prospect after discoveries of Higgs/SUSY
Presentation transcript:

Science Case for / Physics Goals of ALPS-II.

Strong case for particles beyond the Standard Model Standard Model (SM) of particle physics describes basic proper-ties of known matter and forces SM not a complete and fundamental theory: No satisfactory explanation for values of its many parameters No quantum gravity

Strong case for particles beyond the Standard Model Standard Model (SM) of particle physics describes basic proper-ties of known matter and forces SM not a complete and fundamental theory: No satisfactory explanation for values of its many parameters No quantum gravity No explanation of the origin of dark energy and dark matter (wikipedia)

Strong case for particles beyond the Standard Model Standard Model (SM) of particle physics describes basic proper-ties of known matter and forces SM not a complete and fundamental theory: No satisfactory explanation for values of its many parameters No quantum gravity No explanation of the origin of dark energy and dark matter Leading dark matter candidates: Neutralinos and other Weakly Interac-ting Massive Particles (WIMPs) Axions and other very Weakly Interac-ting Slim (=ultra-light) Particles (WISPs) (Kim,Carosi 10)

Axion and axion-like particles: Theory Peccei-Quinn solution of strong CP puzzle: introduce axion field a(x) as dynamical theta parameter, enjoying a shift symmetry, broken only by anomalous couplings to gauge fields, Effective theta parameter has zero expectation value: no strong CP violation Elementary particle excitation of axion field: QCD axion (Weinberg 78; Wilczek 78) For large decay constant : prime example of a WISP . . . (Kim 79; Shifman et al 80; Zhitnitsky 80; Dine et al 81) Axion-like particles (ALPs) : more axion-like fields with shift symmetry and anomalous couplings to gauge bosons

Axion and axion-like particles: Theory

Axion and axion-like particles: Theory In field theoretic extensions of SM, axion and ALP fields realised as phase of complex SM singlet scalar fields whose vacuum expectation values break global anomalous chiral U(1) symmetries . (Peccei, Quinn 77) At energies much below the symmetry breaking, the low-energy effec-tive field theory is that of (pseudo-)Nambu-Goldstone bosons with decay constants In models, in which the global PQ symmetries are not imposed by hand, but in which they appear as automatic consequences of local gauge in-variance, renormalisability and pattern of gauge symmetry breakdown: . (Georgi, Hall, Wise 81) Big range of possibilities discussed in literature:

Axion and axion-like particles: Theory Particular strong motivation for the exi-stence of the axion and ALPs comes from string theory Low-energy effective field theory emer-ging from string theory predicts natural candidates for the QCD axion, often even an `axiverse´, containing many additional ALPs (Witten 84; Conlon 06; Svrcek, Witten 06; Arvanitaki et al 09; Acharya et al 10; Cicoli,Goodsell,AR 12) Number of ALPs = number of cycles of extra-dimensional manifold Big range of possibilities, since its vo-lume can take a range of values:

Axion and axion-like particles: Theory

Axion and axion-like particles: Astrophysics Strong bounds on axions/ALPs come from their effects on stellar evo-lution and on the propagation of SM particles through astrophysical en-vironments: (Raffelt 96) Non-observation of an anomalous energy loss of Horizontal Branch (HB) stars due to ALP emission: Absense of a gamma-ray burst due to axion/ALP-photon conversion in coincidence with neutrinos from SN 1987A: (Brockway et al 96; Grifols et al 96) Just behind the boundary of current bounds, there are intriguing hints suggesting existence of axions and ALPs (Isern et al 08;12) Evidence for a non-standard energy loss in white dwarfs, consistent with the existence of a sub keV mass axion or ALP with

Axion and axion-like particles: Astrophysics TeV photons from distant Active Galactic Nuclei (AGN) should show absorption features due to e+e- pair production at the Extragalactic Background Light (EBL)

Axion and axion-like particles: Astrophysics TeV photons from distant Active Galactic Nuclei (AGN) should show absorption features due to e+e- pair production at the Extragalactic Background Light (EBL) Not the case: (e.g. Horns,Meyer) Analysis of 50 spectra (HESS, MAGIC, Veritas): minimal EBL, absorption excluded by more than 4 sigma (Horns,Meyer 12)

Axion and axion-like particles: Astrophysics TeV photons from distant Active Galactic Nuclei (AGN) should show absorption features due to e+e- pair production at the Extragalactic Background Light (EBL) Not the case: (e.g. Horns,Meyer) Analysis of 50 spectra (HESS, MAGIC, Veritas): minimal EBL, absorption excluded by more than 4 sigma Possible explanation in terms of photon <-> ALP conversions in astrophysical magnetic fields (Roncadelli et al 07; Simet et al 08; Sanchez-Conde et al 09; Horns et al 12)

Axion and axion-like particles: Astrophysics

Axion and axion-like particles: Dark matter Axions and other bosonic WISPy cold dark matter may be produ-ced non-thermally via vacuum-realignment in form of classical, spatially coherent oscillating fields = coherent state of extre-mely non-relativistic dark matter (Preskill et al 83; Abbott,Sikivie 83; Dine,Fischler 83; Cadamuro et al 12)

Axion and axion-like particles: Dark matter Axions and other bosonic WISPy cold dark matter may be produ-ced non-thermally via vacuum-realignment in form of classical, spatially coherent oscillating fields = coherent state of extre-mely non-relativistic dark matter Axion (ALPs) can contribute signifi-cantly to cold dark matter for . (a wider range of parameters) Axion or ALP cold dark matter may form rethermalising Bose Einstein Condensate (BEC) (Sikivie,Yang 09; Erken et al. 12; Sikivie 12) Observational evidence for caustic rings of dark matter consistent with BEC, but not with WIMPy dark matter (Cadamuro et al. 12)

Axion and axion-like particles: Goals of ALPS-IIc Chart thus-far unexplored parameter space, surpassing, at low masses, even the limits from the CERN Axion Solar Telescope (CAST) Tackle regions which are favored by astrophysical hints, dark matter, and theory

Hidden photons: Theory Most extensions of standard model based on supergravity or super-strings predict “hidden sector” of particles which are very weakly cou-pled to the “visible sector” standard model particles Hidden-sector Abelian gauge bosons (hidden photons) provide a win-dow to the hidden sector since they can mix kinetically with the visible sector hypercharge U(1) gauge boson, Kinetic mixing generated at loop level via messenger exchange (Holdom 86; Dienes et al 97; Abel et al 08; Goodsell et al 09;12; Cicoli et al 11)

Hidden photons: Dark radiation For meV scale masses, photon <-> hidden photon oscillations occur resonantly after big bang nucleosynthesis, producing a hidden cosmic microwave background, leading to an increase of the cosmic energy density in invisible radiation at decoupling (dark radiation), often quoted as the effective number of neutrino species (Jaeckel,Redondo,AR 08) CMB observations seem to favour extra dark radiation: (Komatsu et al [WMAP] 10; Dunkley et al [Acatama Cosmology Telescope Collaboration] 10) Required parameters:

Hidden photons: Goals of ALPS-IIa/IIb Conclusive test of hidden photon dark radiation hypothesis Probe parameter region predicted in intermediate string scale scenarios Tackle a fraction of hidden photon dark matter parameter space

Summary Strong physics case for WISPs from theory: Solution of strong CP problem gives particularly strong motivation for existence of QCD axion In many UV completions of SM with a QCD axion, there occur also ALPs Hidden sectors are often exploited in supersymmetric extensions of the SM. In these sectors, hidden photons are very well motivated WISP candidates providing a window to the hidden sector. ALPs and hidden photons can solve puzzles in astrophysics and cos-mology: Anomalous energy loss of white dwarfs Anomalous transparency of the universe for TeV photons Extra dark radiation WISPy dark matter ALPS-II can tackle corresponding regions in WISPy parameter space!

Backup Study on ALP explanation of TeV transparency in progress (Horns,Meyer): ALPS-II covers fiducial region

Backup Projected axion/ALP sensitivities of other experiments: (Hewett et al 12)

Backup Projected hidden photon sensitivities of other experiments: (Hewett et al 12)