DOCSLIB.ORG

Wispy Cold Dark Matter Heidelberg University!

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Wispy Cold Dark Matter Heidelberg University! WISPy Cold Dark Matter Heidelberg University! ** J. Jaeckel † S. Abel , J. Berges**, B. Doebrichz, M. Goodsellxx, H. Gies0, F. Kahlhoefer*, S. Knirck**, † V. Khoze , A. Lobanovy, J. Redondox, A. Ringwald*, K. Schmidt-Hoberg* and The FUNK Collaboration ** † ITP Heidelberg, zCERN, IPPP Durham, *DESY, YMPIfR Bonn, xU. Zaragoza, xxParis LPTHE, 0ITP Jena What we know... Inventory of the Universe Heidelberg University! Dark Energy 68% Neutrinos 0.1-0.5% Ordinary matter 5% Dark Matter 27% Where does it hide? Where does it hide? Try to find me Exploring is (at least) 2 dimensional Heidelberg University! ν,Fixed target Can Dark Matter be WISPy? (Weakly Interacting Sub-eV Particley ) Slim Dark Matter Properties of Dark Matter Heidelberg University! • Dark matter is dark, i.e. it doesn‘t radiate! (and also doesn‘t absorb) è very, very weak interactions with light and with ordinary matter è Exactly the property of WISPs Exploring is (at least) 2 dimensional Heidelberg University! “dark” ν,Fixed target = weakly coupled A common prejudice Heidelberg University! • Dark Matter has to be heavy: • Prejudice based on thermal production! and/or fermionic DM! Both assumptions give v>vescape minimal velocity è(thermal/Fermi) galaxy, i.e. structure, formation inhibited! v<vescape Weakly interacting sub-eV DM Heidelberg University! • Has to be non-thermally (cold!!!) produced See misalignment mechanism • Bosonic! Axion(-like particles) Hidden Photons Dark matter has to be heavy… Heidelberg University! Dark matter has to be heavy Dark matter has to be heavy… Heidelberg University! Dark matter has to be heavy Example WISP: Axions in a nutshell A dirty little secret... Heidelberg University! • The θ-term violates time reversal (T=CP)! • Connected to strong interactions! Electric dipole moment of the neutron! Not found è µ~0!!! The axion solution to the strong CP problem Heidelberg University! • Make µ dynamical è it can change its value Classical potential With QCD quantum corrections The axion solution to the strong CP problem Heidelberg University! • Make µ dynamical è it can change its value initially Classical potential With QCD quantum corrections The axion solution to the strong CP problem Heidelberg University! • Make µ dynamical è it can change its value after some time Classical potential With QCD quantum corrections è QCD likes to be CP conserving (if we allow it) The axion solution to the strong CP problem Heidelberg University! • Make µ dynamical è it can change its value Classical potential With QCD quantum corrections è Can still move è new particle = axion Axions Heidelberg University! • Classical flatness from symmetry • Quantum corrections are small • New light particle: The Axion (it’s a Weakly Interacting Sub-eV Particle) Dark matter candidate Good motivation for axion/WISP experiments Axion also couples to two photons Heidelberg University! Coupling to two photons Very very weak Because: Very large Axion also couples to two photons Heidelberg University! “A” Physics J Coupling to two photons Very very weak Because: Very large Axion also couples to two photons Heidelberg University! Coupling to two photons Very very weak Because: Very large Axion-like Particles Heidelberg University! mass/energy 0 CDF LHC Yinv. LEP + - -3 e e inv.+ Beam LSW dump ] -6 1 - 0 SN1987a ¼ GeV [ CAST aBB -9 + g SUMICO HB stars 10 SN1987a Cosmology Log -12 Weaker interactionWeaker Intermediate string scale models -15 Axion band -18 -15 -12 -9 -6 -3 0 3 6 9 12 15 Log10 ma[eV] Axion-like Particles Heidelberg University! mass/energy 0 CDF LHC Yinv. LEP + - -3 e e inv.+ Beam LSW dump ] -6 1 - SN1987a GeV [ CAST aBB -9 + g SUMICO HB stars 750 GeV ALP 10 SN1987a Cosmology Log -12 Weaker interactionWeaker Intermediate string scale models -15 Axion band -18 -15 -12 -9 -6 -3 0 3 6 9 12 15 Log10 ma[eV] Looking for Axions/ALPs Light shining through walls Heidelberg University! X X Light shining through walls Heidelberg University! X X • Test • Enormous precision! • Study extremely weak couplings! Photons coming through the wall! Heidelberg University! • It could be Axion(-like particle)s! • Coupling to two photons: a a ALPS @ Hamburg Heidelberg University! 0 CDF LHC Yinv. LEP + - -3 e e inv.+ Beam ALPS-ILSW dump ] -6 1 ~104 GeV - SN1987a GeV [ CAST aBB -9 ALPS-II + g SUMICO HB stars 8 10 ~10 GeV SN1987a Cosmology Log -12 Intermediate string scale models -15 Axion band -18 -15 -12 -9 -6 -3 0 3 6 9 12 15 Log10 ma[eV] Going deeper Helioscopes Heidelberg University! CAST@CERN SUMICO@Tokyo SHIPS@Hamburg Sun Detector Ion Going to the future: IAXO Heidelberg University! The International Axion Observatory CAST + IAXO Heidelberg University! 0 CDF LHC Yinv. LEP + - -3 e e inv.+ Beam ALPS-ILSW dump ] -6 1 - SN1987a GeV [ CAST aBB -9 + g SUMICO HB stars 10 SN1987a Cosmology 9 Log IAXO ~10 GeV -12 Intermediate string scale models -15 Axion band -18 -15 -12 -9 -6 -3 0 3 6 9 12 15 Log10 ma[eV] Dark Matter(s) The axion has no clue where to start Heidelberg University! Can sit anywhere Early times High T>TQCD The axion has no clue where to start Heidelberg University! Early times High T>TQCD t&10µs Low T<TQCD Can start moving… The axion solution to the strong CP problem Heidelberg University! Classical potential With QCD quantum corrections è Oscillations contain energy è behave like non-relativistic particles (T=0) Why Cold? Inflation! Heidelberg University! Field value space Axion(-like particle) Dark Matter Heidelberg University! ~107 GeV ~1012 GeV Detecting WISPy DM Use a plentiful source of axions Heidelberg University! • Photon Regeneration Photon (amplified in resonator) axion (dark matter) Signal: Total energy of axion Heidelberg University! RF Receiver Virial velocity in galaxy halo! An extremely sensitive probe!!! Heidelberg University! Electricity from Dark Matter ;-). Heidelberg University! • Photon Regeneration Photon (amplified in resonator) axion (dark matter) Really sustainable Energy Heidelberg University! • Galaxy contains (6-30)x1011 solar masses of DM è (3-15)x1043 TWh @100000 TWh per year (total world today) è 1038 years J DM power ½*v~300 MeV/cm3*300km/s~10 W/m2 compared to 2W/m2 for wind A discovery possible any minute! Heidelberg University! Beam Encircling the axion… Heidelberg Dump University! -6 LSW ALPS-I SN1987a -8 Solar n HelioscopesH CASTL YMCE Telescopes HB D -10 1 TeV ALPS-II - SN g-burst Transparency H L REAPR GeV @ IAXO xion -12 WD cooling hint Coupling Dish axion CDM Antenna Haloscopes ADMX-HF Log -14 ALP CDM ADMX Intermediate string scale EBL -16 X axion - Rays KSVZ -18 -12 -10 -8 -6 -4 -2 0 2 4 6 Log Mass eV @ D Beyond ALPs Also for hidden photons!!! Heidelberg University! • There are other very light DM candidates • E.g extra (hidden) U(1) bosons=hidden photons!!! @ DESY + Bonn: WISPDMX Heidelberg University! New Results! Broadband Search Strategy Dark Matter Antenna Heidelberg University! Antenna converts axion->photon Radiation concentrated in center Detector B Probes here; very sensitive!! The FUNK Experiment Heidelberg University! Recycle Auger mirror Detector First Results Heidelberg University! Upgrade: The PMT 9000(+107) Heidelberg University! Discovery Potential J!!! A Dream for Astrology ehhm Astronomy Heidelberg University! • Emission from moving dark matter VDM =0 VDM≠0= • A picture of the DM-velocity distribution Screen Going Monodromic Axion Monodromy Heidelberg University! • Allows for extended field range Advantages Heidelberg University! • Allows to start with higher energy density è More DM vs Models in this region! Interesting Phenomena?? Heidelberg University! Could get stuck here Oscillations like DM! Interesting Phenomena?? Heidelberg University! Overdense region? Could get stuck here Interesting Phenomena?? Heidelberg University! Regions with “negative mass” Instability è Particle Production with p≠0?!? Running through walls A WISPy Domain Wall Heidelberg University! Potential with two minima Domain wall from side 1 To side 2 A WISPy Domain Wall Heidelberg University! Potential with two minima Domain wall from side 1 To side 2 v aLIGO Heidelberg University! • Has detected gravitational waves!! • Is an Interferometer Interference pattern Causing a phase shift Heidelberg University! • Interaction inside wall creates photon mass aLIGO Heidelberg University! • Has detected gravitational waves!! • Is an Interferometer Interference pattern changed Signal shapes Heidelberg University! Signal shapes Heidelberg University! How to distiguish from grav waves? Heidelberg University! • velocity<<c • v~10-3 è Time difference between two sites ~few seconds è Need careful analysis strategies Conclusions Conclusions Heidelberg University! • Good Physics Case for Axions and WISPs explore `The Low Energy Frontier’ • Low energy experiments complementary to accelerators! • Dark Matter may be WISPy J è New Search opportunities! è Searches ongoing! è Crazy things to explore! X .
Load more

Recommended publications
  • CERN Courier–Digital Edition
    CERNMarch/April 2021 cerncourier.com COURIERReporting on international high-energy physics WELCOME CERN Courier – digital edition Welcome to the digital edition of the March/April 2021 issue of CERN Courier. Hadron colliders have contributed to a golden era of discovery in high-energy physics, hosting experiments that have enabled physicists to unearth the cornerstones of the Standard Model. This success story began 50 years ago with CERN’s Intersecting Storage Rings (featured on the cover of this issue) and culminated in the Large Hadron Collider (p38) – which has spawned thousands of papers in its first 10 years of operations alone (p47). It also bodes well for a potential future circular collider at CERN operating at a centre-of-mass energy of at least 100 TeV, a feasibility study for which is now in full swing. Even hadron colliders have their limits, however. To explore possible new physics at the highest energy scales, physicists are mounting a series of experiments to search for very weakly interacting “slim” particles that arise from extensions in the Standard Model (p25). Also celebrating a golden anniversary this year is the Institute for Nuclear Research in Moscow (p33), while, elsewhere in this issue: quantum sensors HADRON COLLIDERS target gravitational waves (p10); X-rays go behind the scenes of supernova 50 years of discovery 1987A (p12); a high-performance computing collaboration forms to handle the big-physics data onslaught (p22); Steven Weinberg talks about his latest work (p51); and much more. To sign up to the new-issue alert, please visit: http://comms.iop.org/k/iop/cerncourier To subscribe to the magazine, please visit: https://cerncourier.com/p/about-cern-courier EDITOR: MATTHEW CHALMERS, CERN DIGITAL EDITION CREATED BY IOP PUBLISHING ATLAS spots rare Higgs decay Weinberg on effective field theory Hunting for WISPs CCMarApr21_Cover_v1.indd 1 12/02/2021 09:24 CERNCOURIER www.
    [Show full text]
  • Axions and Other Similar Particles
    1 91. Axions and Other Similar Particles 91. Axions and Other Similar Particles Revised October 2019 by A. Ringwald (DESY, Hamburg), L.J. Rosenberg (U. Washington) and G. Rybka (U. Washington). 91.1 Introduction In this section, we list coupling-strength and mass limits for light neutral scalar or pseudoscalar bosons that couple weakly to normal matter and radiation. Such bosons may arise from the spon- taneous breaking of a global U(1) symmetry, resulting in a massless Nambu-Goldstone (NG) boson. If there is a small explicit symmetry breaking, either already in the Lagrangian or due to quantum effects such as anomalies, the boson acquires a mass and is called a pseudo-NG boson. Typical examples are axions (A0)[1–4] and majorons [5], associated, respectively, with a spontaneously broken Peccei-Quinn and lepton-number symmetry. A common feature of these light bosons φ is that their coupling to Standard-Model particles is suppressed by the energy scale that characterizes the symmetry breaking, i.e., the decay constant f. The interaction Lagrangian is −1 µ L = f J ∂µ φ , (91.1) where J µ is the Noether current of the spontaneously broken global symmetry. If f is very large, these new particles interact very weakly. Detecting them would provide a window to physics far beyond what can be probed at accelerators. Axions are of particular interest because the Peccei-Quinn (PQ) mechanism remains perhaps the most credible scheme to preserve CP-symmetry in QCD. Moreover, the cold dark matter (CDM) of the universe may well consist of axions and they are searched for in dedicated experiments with a realistic chance of discovery.
    [Show full text]
  • Axions –Theory SLAC Summer Institute 2007
    Axions –Theory SLAC Summer Institute 2007 Helen Quinn Stanford Linear Accelerator Center Axions –Theory – p. 1/?? Lectures from an Axion Workshop Strong CP Problem and Axions Roberto Peccei hep-ph/0607268 Astrophysical Axion Bounds Georg Raffelt hep-ph/0611350 Axion Cosmology Pierre Sikivie astro-ph/0610440 Axions –Theory – p. 2/?? Symmetries Symmetry ⇔ Invariance of Lagrangian Familiar cases: Lorentz symmetries ⇔ Invariance under changes of coordinates Other symmetries: Invariances under field redefinitions e.g (local) gauge invariance in electromagnetism: Aµ(x) → Aµ(x)+ δµΩ(x) Fµν = δµAν − δνAµ → Fµν Axions –Theory – p. 3/?? How to build an (effective) Lagrangian Choose symmetries to impose on L: gauge, global and discrete. Choose representation content of matter fields Write down every (renormalizable) term allowed by the symmetries with arbitrary couplings (d ≤ 4) Add Hermitian conjugate (unitarity) - Fix renormalized coupling constants from match to data (subtractions, usually defined perturbatively) "Naturalness" - an artificial criterion to avoid arbitrarily "fine tuned" couplings Axions –Theory – p. 4/?? Symmetries of Standard Model Gauge Symmetries Strong interactions: SU(3)color unbroken but confined; quarks in triplets Electroweak SU(2)weak X U(1)Y more later:representations, "spontaneous breaking" Discrete Symmetries CPT –any field theory (local, Hermitian L); C and P but not CP broken by weak couplings CP (and thus T) breaking - to be explored below - arises from quark-Higgs couplings Global symmetries U(1)B−L accidental; more? Axions –Theory – p. 5/?? Chiral symmetry Massless four component Dirac fermion is two independent chiral fermions (1+γ5) (1−γ5) ψ = 2 ψ + 2 ψ = ψR + ψL γ5 ≡ γ0γ1γ2γ3 γ5γµ = −γµγ5 Chiral Rotations: rotate L and R independently ψ → ei(α+βγ5)ψ i(α+β) i(α−β) ψR → e ψR; ψL → e ψL Kinetic and gauge coupling terms in L are chirally invariant † ψγ¯ µψ = ψ¯RγµψR + ψ¯LγµψL since ψ¯ = ψ γ0 Axions –Theory – p.
    [Show full text]
  • The WISP Paradigm
    The WISP Paradigm Javier Redondo Max Planck Institut (Werner Heisenberg Institut) Munich MPI 14/12/2009 Hidden Sectors in PBSM 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, ψMCP... Hidden Sectors can be quite complicated we certainly don’t know! Hidden Sector 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 ! Hidden Sectors can be quite complicated we certainly don’t know! Hidden Sector BIG guys Light guys (live in the mountains) (mass is protected by a symmetry) Goldstone Chiral Bosons WISPsfermions (very) weakly interacting sub-eV 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 ! Axion-like-Particles and Axions 1 µν Axions are GB of a color anomalous U(1) Tr Gµν G a 4fa { } The color anomalous term creates a potential with CP conserving minimum Solution to Strong CP which gives the axion a mass m f 10 10GeV 1 m π π 0.6 meV − − .
    [Show full text]
  • Axions & Wisps
    FACULTY OF SCIENCE AXIONS & WISPS STEPHEN PARKER 2nd Joint CoEPP-CAASTRO Workshop September 28 – 30, 2014 Great Western, Victoria 2 Talk Outline • Frequency & Quantum Metrology Group at UWA • Basic background / theory for axions and hidden sector photons • Photon-based experimental searches + bounds • Focus on resonant cavity “Haloscope” experiments for CDM axions • Work at UWA: Past, Present, Future A Few Useful Review Articles: J.E. Kim & G. Carosi, Axions and the strong CP problem, Rev. Mod. Phys., 82(1), 557 – 601, 2010. M. Kuster et al. (Eds.), Axions: Theory, Cosmology, and Experimental Searches, Lect. Notes Phys. 741 (Springer), 2008. P. Arias et al., WISPy Cold Dark Matter, arXiv:1201.5902, 2012. [email protected] The University of Western Australia 3 Frequency & Quantum Metrology Research Group ~ 3 staff, 6 postdocs, 8 students Hosts node of ARC CoE EQuS Many areas of research from fundamental to applied: Cryogenic Sapphire Oscillator Tests of Lorentz Symmetry & fundamental constants Ytterbium Lattice Clock for ACES mission Material characterization Frequency sources, synthesis, measurement Low noise microwaves + millimetrewaves …and lab based searches for WISPs! Core WISP team: Stephen Parker, Ben McAllister, Eugene Ivanov, Mike Tobar [email protected] The University of Western Australia 4 Axions, ALPs and WISPs Weakly Interacting Slim Particles Axion Like Particles Slim = sub-eV Origins in particle physics (see: strong CP problem, extensions to Standard Model) but become pretty handy elsewhere WISPs Can be formulated as: Dark Matter (i.e. Axions, hidden photons) ALPs Dark Energy (i.e. Chameleons) Low energy scale dictates experimental approach Axions WISP searches are complementary to WIMP searches [email protected] The University of Western Australia 5 The Axion – Origins in Particle Physics CP violating term in QCD Lagrangian implies neutron electric dipole moment: But measurements place constraint: Why is the neutron electric dipole moment (and thus θ) so small? This is the Strong CP Problem.
    [Show full text]
  • Rare Event Physics WG1
    Rare event physics WG1 Our ambitious mission : ● Show the state of the art of the physics of rare events ● Cover for both experimental and theoretical aspects ● Provide hints for the exploration of next generation experiments (link with WG5) ● Provide a guideline for experimental and technological efforts, like constraints for low cosmo- and radio-purity techniques(WG2), for detection methods (WG3) and analysis tools (WG4) ● Being inclusive to any other scientific field that would profit of deep underground sites Christine Marquet, CENBG Mariangela Settimo, Subatech May 31, 2021 - visioconference Luca Scotto Lavina, LPNHE Two major axes 1. Dark Matter WG1 We will keep a particular eye on direct search of dark matter : ● Scoping the whole zoology of models (WIMP, WISP, axions, …), nucleo- or lepto-philic ● Exploring a wide (and experimentally accessible) range of masses/energies ( >GeV, sub-GeV, down to μeV) ● Looking for any trace of daily and seasonal modulation ● Using a plethora of targets and combinations of energy losses ● Complementarity with colliders (new particles) and indirect evidences (annihilation) Christine Marquet, CENBG Mariangela Settimo, Subatech May 31, 2021 - visioconference Luca Scotto Lavina, LPNHE Two major axes 2. Neutrinoless double beta decay WG1 We will keep an eye on the search for the intimate nature of neutrinos : ● Nature of neutrino (Majorana/Dirac) ● Fixing the neutrino mass scale and possible mass scenarii ● Proof of a lepton number violation ● Neutrino hierarchy ● Impact on baryon asymmetry of the Universe
    [Show full text]
  • Evidence for a New 17 Mev Boson
    PROTOPHOBIC 8Be TRANSITION EVIDENCE FOR A NEW 17 MEV BOSON Flip Tanedo arXiv:1604.07411 & work in progress SLAC Dark Sectors 2016 (28 — 30 April) with Jonathan Feng, Bart Fornal, Susan Gardner, Iftah Galon, Jordan Smolinsky, & Tim Tait BART SUSAN IFTAH 1 flip . tanedo @ uci . edu EVIDENCE FOR A 17 MEV NEW BOSON 14 week ending A 6.8σ nuclear transitionPRL 116, 042501 (2016) anomalyPHYSICAL REVIEW LETTERS 29 JANUARY 2016 shape of the resonance [40], but it is definitelyweek different ending pairs (rescaled for better separation) compared with the PRL 116, 042501 (2016) PHYSICAL REVIEW LETTERS 29 JANUARY 2016 from the shape of the forward or backward asymmetry [40]. simulations (full curve) including only M1 and E1 con- Therefore, the above experimental data make the interpre- tributions. The experimental data do not deviate from the Observation of Anomalous Internal Pairtation Creation of the in observed8Be: A Possible anomaly Indication less probable of a as Light, being the normal IPC. This fact supports also the assumption of the Neutralconsequence Boson of some kind of interference effects. boson decay. The deviation cannot be explained by any γ-ray related The χ2 analysis mentioned above to judge the signifi- A. J. Krasznahorkay,* M. Csatlós, L. Csige, Z. Gácsi,background J. Gulyás, M. either, Hunyadi, since I. Kuti, we B. cannot M. Nyakó, see any L. Stuhl, effect J. Timár, at off cance of the observed anomaly was extended to extract the T. G. Tornyi,resonance, and Zs. where Vajta the γ-ray background is almost the same. mass of the hypothetical boson. The simulated angular Institute for Nuclear Research, Hungarian Academy ofTo Sciences the best (MTA of Atomki), our knowledge, P.O.
    [Show full text]
  • Supersymmetry and Stationary Solutions in Dilaton-Axion Gravity" (1994)
    University of Massachusetts Amherst ScholarWorks@UMass Amherst Physics Department Faculty Publication Series Physics 1994 Supersymmetry and stationary solutions in dilaton- axion gravity R Kallosh David Kastor University of Massachusetts - Amherst, [email protected] T Ortín T Torma Follow this and additional works at: https://scholarworks.umass.edu/physics_faculty_pubs Part of the Physical Sciences and Mathematics Commons Recommended Citation Kallosh, R; Kastor, David; Ortín, T; and Torma, T, "Supersymmetry and stationary solutions in dilaton-axion gravity" (1994). Physics Review D. 1219. Retrieved from https://scholarworks.umass.edu/physics_faculty_pubs/1219 This Article is brought to you for free and open access by the Physics at ScholarWorks@UMass Amherst. It has been accepted for inclusion in Physics Department Faculty Publication Series by an authorized administrator of ScholarWorks@UMass Amherst. For more information, please contact [email protected]. SU-ITP-94-12 UMHEP-407 QMW-PH-94-12 hep-th/9406059 SUPERSYMMETRY AND STATIONARY SOLUTIONS IN DILATON-AXION GRAVITY Renata Kallosha1, David Kastorb2, Tom´as Ort´ınc3 and Tibor Tormab4 aPhysics Department, Stanford University, Stanford CA 94305, USA bDepartment of Physics and Astronomy, University of Massachusetts, Amherst MA 01003 cDepartment of Physics, Queen Mary and Westfield College, Mile End Road, London E1 4NS, U.K. ABSTRACT New stationary solutions of 4-dimensional dilaton-axion gravity are presented, which correspond to the charged Taub-NUT and Israel-Wilson-Perj´es (IWP) solu- tions of Einstein-Maxwell theory. The charged axion-dilaton Taub-NUT solutions are shown to have a number of interesting properties: i) manifest SL(2, R) sym- arXiv:hep-th/9406059v1 10 Jun 1994 metry, ii) an infinite throat in an extremal limit, iii) the throat limit coincides with an exact CFT construction.
    [Show full text]
  • Axion Dark Matter from Higgs Inflation with an Intermediate H∗
    Axion dark matter from Higgs inflation with an intermediate H∗ Tommi Tenkanena and Luca Visinellib;c;d aDepartment of Physics and Astronomy, Johns Hopkins University, 3400 N. Charles Street, Baltimore, MD 21218, USA bDepartment of Physics and Astronomy, Uppsala University, L¨agerhyddsv¨agen1, 75120 Uppsala, Sweden cNordita, KTH Royal Institute of Technology and Stockholm University, Roslagstullsbacken 23, 10691 Stockholm, Sweden dGravitation Astroparticle Physics Amsterdam (GRAPPA), Institute for Theoretical Physics Amsterdam and Delta Institute for Theoretical Physics, University of Amsterdam, Science Park 904, 1098 XH Amsterdam, The Netherlands E-mail: [email protected], [email protected], [email protected] Abstract. In order to accommodate the QCD axion as the dark matter (DM) in a model in which the Peccei-Quinn (PQ) symmetry is broken before the end of inflation, a relatively low scale of inflation has to be invoked in order to avoid bounds from DM isocurvature 9 fluctuations, H∗ . O(10 ) GeV. We construct a simple model in which the Standard Model Higgs field is non-minimally coupled to Palatini gravity and acts as the inflaton, leading to a 8 scale of inflation H∗ ∼ 10 GeV. When the energy scale at which the PQ symmetry breaks is much larger than the scale of inflation, we find that in this scenario the required axion mass for which the axion constitutes all DM is m0 . 0:05 µeV for a quartic Higgs self-coupling 14 λφ = 0:1, which correspond to the PQ breaking scale vσ & 10 GeV and tensor-to-scalar ratio r ∼ 10−12. Future experiments sensitive to the relevant QCD axion mass scale can therefore shed light on the physics of the Universe before the end of inflation.
    [Show full text]
  • The International Axion Observatory IAXO
    Letter of Intent to the CERN SPSC The International Axion Observatory IAXO IAXO Collaboration August 7, 2013 CERN-SPSC-2013-022 / SPSC-I-242 08/08/2013 Version: 1.0 IAXO The International Axion Observatory Letter of Intent Date: August 7, 2013 Page 3 of 80 Letter of Intent to the CERN SPSC The International Axion Observatory IAXO E. Armengaud1, F. T. Avignone2, M. Betz3, P. Brax4, P. Brun1, G. Cantatore5, J. M. Carmona6, G. P. Carosi7, F. Caspers3, S. Caspi8, S. A. Cetin9, D. Chelouche10, F. E. Christensen11, A. Dael1, T. Dafni6, M. Davenport3, A.V. Derbin12, K. Desch13, A. Diago6, B. Dobrich¨ 14, I. Dratchnev12, A. Dudarev3, C. Eleftheriadis15, G. Fanourakis16, E. Ferrer-Ribas1, J. Galan´ 1, J. A. Garc´ıa6, J. G. Garza6, T. Geralis16, B. Gimeno17, I. Giomataris1, S. Gninenko18, H. Gomez´ 6, D. Gonzalez-D´ ´ıaz6, E. Guendelman19, C. J. Hailey20, T. Hiramatsu21, D. H. H. Hoffmann22, D. Horns23, F. J. Iguaz6, I. G. Irastorza6;∗, J. Isern24, K. Imai25, A. C. Jakobsen11, J. Jaeckel26, K. Jakovciˇ c´27, J. Kaminski13, M. Kawasaki28, M. Karuza29, M. Krcmarˇ 27, K. Kousouris3, C. Krieger13, B. Lakic´27, O. Limousin1, A. Lindner14, A. Liolios15, G. Luzon´ 6, S. Matsuki30, V. N. Muratova12, C. Nones1, I. Ortega6, T. Papaevangelou1, M. J. Pivovaroff7, G. Raffelt31, J. Redondo31, A. Ringwald14, S. Russenschuck3, J. Ruz7, K. Saikawa32, I. Savvidis15, T. Sekiguchi28, Y. K. Semertzidis33, I. Shilon3, P. Sikivie34, H. Silva3, H. ten Kate3, A. Tomas6, S. Troitsky18, T. Vafeiadis3, K. van Bibber35, P. Vedrine1, J. A. Villar6, J. K. Vogel7, L. Walckiers3, A.
    [Show full text]
  • WISP Dark Matter Theory
    WISP Dark Matter Theory. Andreas Ringwald (DESY) Latest Results in Dark Matter Searches Stockholm, Sweden 12-14 May 2014 Introduction > Plenty of dark matter (DM) candi- dates spanning huge parameter range in masses and couplings > Two classes stand out because of their convincing physics case and the variety of experimental and observational probes: § Weakly Interacting Massive Particles (WIMPs), such as neutralinos § Very Weakly Interacting Slim (=ultra- light) Particles (WISPs), such as axions, axion-like particles and hidden photons [Kim,Carosi `10] Andreas Ringwald | WISP Dark Matter Theory, Latest Results in Dark Matter Searches, Stockholm, 12-14 May 2014 | Page 2 Theoretically favored WISP candidates > Pseudo Nambu-Goldstone bosons: § “Axion-Like Particles” (ALPs) arising from breaking of global U(1) symmetries at high energy scale f a ; angular part of complex SM singlet Higgs-like field • Low energy effective field theory has shift symmetry a ( x ) a ( x ) + const . , forbidding 2 2 explicit mass terms, m a a ( x ) , in the Lagrangian ! • Effective couplings to/ SM particles suppressed by powers of high energy scale f a , e.g. coupling to photons, ↵ a C F F˜µ⌫ aγ µ⌫ L ⊃−8⇡ fa • Examples: • Axion from breaking of global chiral symmetry; axion field acts as dynamical theta parameter, [Peccei,Quinn 77; Weinberg 78; Wilczek 78] spontaneously relaxing to zero, (thus CP conserved in strong interactions) • mass due to chiral symmetry breaking, • Majoron from breaking of global lepton number symmetry [Chikashige et al. 78] • high scale
    [Show full text]
  • The Many Faces of the Inflaton Field
    The many faces of the inflaton field Tommi Tenkanen in collaboration with T. Alanne, F. Sannino, K. Tuominen, and V. Vaskonen Queen Mary University of London Talk based on arXiv: 1606.06063, 1607.01379, 1611.04932 University of Helsinki 8/3/2017 E-mail: [email protected] Tommi Tenkanen The many faces of the inflaton field 8/3/2017 1 / 30 Open problems in cosmology Tommi Tenkanen The many faces of the inflaton field 8/3/2017 2 / 30 Evidence for Dark Matter Great deal of evidence for the existence of dark matter: rotational velocity curves of galaxies, Bullet Cluster1, acoustic peaks in the Cosmic Microwave Background (CMB) radiation spectrum... Still the nature of dark matter is unknown 1 Image: Chandra X-ray Observatory Tommi Tenkanen The many faces of the inflaton field 8/3/2017 3 / 30 What is Dark Matter? What is the correct explanation for the invisible matter content observed in the universe? Does the dark matter particle exist? Or are there many dark matter particles? Are they WIMP’s, FIMP’s, SIMP’s, GIMP’s, PIDM’s, WISP’s, ALP’s, Wimpzillas, or sterile neutrinos? Or should gravity be modified? How can we tell which model is the correct one (if any)? Tommi Tenkanen The many faces of the inflaton field 8/3/2017 4 / 30 Search for Dark Matter Many on-going experiments exist2 Yet no conclusive detection. 2 Original image: Max-Planck-Institut Für Kernphysik Tommi Tenkanen The many faces of the inflaton field 8/3/2017 5 / 30 Matter–antimatter asymmetry Why is there more matter than antimatter? How and at what point in the history of the universe was this asymmetry generated? Electroweak baryogenesis remains as a viable candidate for explaining the origin of this asymmetry.
    [Show full text]