Auf der Suche nach ultraleichten Teilchen jenseits des Standardmodells

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1 Auf der Suche nach ultraleichten Teilchen jenseits des Standardmodells 77. Jahrestagung der DPG und DPG-Frühjahrstagung Dresden Axel Lindner, DESY Outline > Physics beyond the Standard Model > Keys to BSM physics and WISPy particles > WISP experiments Laboratory bases Helioscopes Haloscopes > International activities and summary Axel Lindner WISPs beyond the SM March 7 th 2013 Page 2 1

2 Physics beyond the standard model Axel Lindner WISPs beyond the SM March 7 th 2013 Page 3 There is physics beyond the SM > Dark matter and dark energy: (Credit Queens Univ) Even if one neglects dark energy: 83% of the matter are of unknown constituents. Axel Lindner WISPs beyond the SM March 7 th 2013 Page 4 2

3 There is physics beyond the SM > Dark matter and dark energy candidate constituents: (Credit Queens Univ) > Very weak interaction with SM matter > Very weak interaction among themselves > Stable on cosmological times > Non-relativistic Axel Lindner WISPs beyond the SM March 7 th 2013 Page 5 There is physics beyond the SM > Dark matter and dark energy candidate constituents: (Credit Queens Univ) > Very weak interaction with SM matter > Very weak interaction among themselves > Stable on cosmological times > Non-relativistic > Extremely lightweight scalar particle Axel Lindner WISPs beyond the SM March 7 th 2013 Page 6 3

4 There might be physics beyond the SM > Puzzles from astrophysics: Example: TeV photons should be absorbed in the intergalactic space, Center of mass energy about 1 MeV! M. Meyer, 7th Patras Workshop on Axions, WIMPs and WISPs, 2011 Axel Lindner WISPs beyond the SM March 7 th 2013 Page 7 There might be physics beyond the SM > Puzzles from astrophysics: but this seems to be in conflict with observations. D. Horns, M. Meyer, JCAP 1202 (2012) 033 > If physics beyond the SM is involved, it happens below the MeV scale! Axel Lindner WISPs beyond the SM March 7 th 2013 Page 8 4

5 There might be physics beyond the SM > CP-conservation in QCD: why does the static electromagnetic dipole moment of the neutron vanish? Why do the wave functions of the three quarks exactly cancel out any observable static charge distribution in the neutron? Why does QCD conserve CP? In principle QCD would allow for CP violation parameterized by an overall phase Θ of the quark mass matrix. Axel Lindner WISPs beyond the SM March 7 th 2013 Page 9 There might be physics beyond the SM > CP-conservation in QCD: F. Wilczek at Vistas in Axion Physics, Seattle, 26 April 2012 (see The overall phase of the quark mass matrix is physically meaningful. In the minimal standard model, this phase is a free parameter, theoretically. Experimentally it is very small. This is the most striking unnaturality of the standard model, aside from the cosmological term. It does not seem susceptible of anthropic explanation. In QCD a free parameter Θ could have any value between 0 and 2π. Experimentally, Θ < Axel Lindner WISPs beyond the SM March 7 th 2013 Page 10 5

6 Physics beyond the standard model > > > No clue on energy scale of BSM physics from DM. If confirmed, energy scale well below the TeV regime. Not only the TeV-scale arguments! Axel Lindner WISPs beyond the SM March 7 th 2013 Page 11 Outline > Physics beyond the Standard Model > Keys to BSM physics and WISPy particles > WISP experiments Laboratory bases Helioscopes Haloscopes > International activities and summary Axel Lindner WISPs beyond the SM March 7 th 2013 Page 12 6

7 Keys to beyond SM physics Symmetry magazin, August 2006 Axel Lindner WISPs beyond the SM March 7 th 2013 Page 13 Supersymmetry > Very viable option, also in context with dark matter! > Will not be covered here! Nature 471, (2011) doi: /471013a Axel Lindner WISPs beyond the SM March 7 th 2013 Page 14 7

8 Supersymmetry at the end of 2012 an internet joke Axel Lindner WISPs beyond the SM March 7 th 2013 Page 15 Supersymmetry at the end of 2012 an internet joke However, this statement is not even wrong! Axel Lindner WISPs beyond the SM March 7 th 2013 Page 16 8

9 Supersymmetry at the end of 2012 an old joke T 3.2 Do 9:10 9:50 HSZ-01, Martin Wessels: Needles in a Haystack Beyond the Standard Model Searches at the LHC T 3.3 Do 9:50 10:30 HSZ-01, Tilman Plehn: New Physics, Where Art Thou Axel Lindner WISPs beyond the SM March 7 th 2013 Page 17 SM extension: µev or/and TeV? > Also very lightweight, very weakly interacting new particles might show the way to physics beyond the Standard Model. 15 orders of magnitude: looking for atoms instead of planets? Axel Lindner WISPs beyond the SM March 7 th 2013 Page 18 9

10 Introducing the axion > CP-conservation in QCD: S. Hannestaad, presentation at 5th Patras Workshop on Axions, WIMPs and WISPs, 2009 A dynamic explanation for Θ < 10-9 predicts the axion, which couples very weakly to two photons. Peccei-Quinn 1977 T f a T GeV Wilczek and Weinberg 1978 Axel Lindner WISPs beyond the SM March 7 th 2013 Page 19 The Search for Axions, Carosi, van Bibber, Pivovaroff, Contemp. Phys. 49, No. 4, 2008 Introducing the axion Javier Redondo s talk at last year s DPG meeting: Axel Lindner WISPs beyond the SM March 7 th 2013 Page 20 10

11 Introducing the axion Javier Redono s talk at last year s DPG meeting: Axel Lindner WISPs beyond the SM March 7 th 2013 Page 21 Properties of the axion > The QCD axion: light, neutral pseudoscalar boson. > The QCD axion: the light cousin of the π 0. Mass and the symmetry breaking scale f a are related: m a = 0.6eV (10 7 GeV / f a ) The coupling strength to photons is g aγγ = α g γ / (π f a ), where g γ is model dependent and O(1). Note: g aγγ = α g γ / (π GeV) m a The axion abundance in the universe is Ω a / Ω c (f a / GeV) 7/6. f a < GeV m a > µev The Search for Axions, Carosi, van Bibber, Pivovaroff, Contemp. Phys. 49, No. 4, 2008 Axel Lindner WISPs beyond the SM March 7 th 2013 Page 22 11

12 Properties of the axion > The QCD axion: light, neutral pseudoscalar boson. > The QCD axion: the light cousin of the π 0. Mass and the symmetry breaking scale f a are related: m a = 0.6eV (10 7 GeV / f a ) The coupling strength to photons is g aγγ = α g γ / (π f a ), where g γ is model dependent and O(1). Note: g aγγ = α g γ / (π GeV) m a The axion abundance in the universe is Ω a / Ω c (f a / GeV) 7/6. f a < GeV m a > µev The Search for Axions, Carosi, van Bibber, Pivovaroff, Contemp. Phys. 49, No. 4, 2008 Axel Lindner WISPs beyond the SM March 7 th 2013 Page 23 Axions are perfect cold DM candidates > Axions with µev mass are perfect cold dark matter candidates. > They would interact extremely weakly with SM constituents. > Similar to SUSY-WIMPs axions would solve two puzzles in one go: Dark matter CP conservation in QCD. 52 orders of magnitude 52 orders of magnitude H. Baer, presentation at 5th Patras Workshop on Axions, WIMPs and WISPs, 2009 Axel Lindner WISPs beyond the SM March 7 th 2013 Page 24 12

13 Properties of the axion > The QCD axion: the light cousin of the π 0. > Therefore the Primakoff effect will also work for the axion! Axel Lindner WISPs beyond the SM March 7 th 2013 Page 25 Properties of the axion > The QCD axion: the light cousin of the π 0. > Therefore the Primakoff effect will also work for the axion! > Axions could be produced (detected) by sending a light beam (them) through a magnetic field: γ π 0 / a Axel Lindner WISPs beyond the SM March 7 th 2013 Page 26 13

14 Axions at the end of 2012 probably the only axion spotted so far at CERN Axel Lindner WISPs beyond the SM March 7 th 2013 Page 27 Sakurai prize 2013: H. Quinn & R. Peccei 2010: P.W. Higgs and others! Axel Lindner WISPs beyond the SM March 7 th 2013 Page 28 14

15 More general: WISPy particles Weakly Interacting Slim Particles (WISPs): > Axions and axion-like particles (ALPs, pseudoscalar or scalar bosons) > Hidden photons (neutral vector bosons) > Mini-charged particles > Chameleons (self-shielding scalars), massive gravity scalars Axel Lindner WISPs beyond the SM March 7 th 2013 Page 29 Such WISPs are expected by theory > Axions, ALPs and other WISPs occur naturally in string theory inspired extensions of the standard model as components of a hidden sector. DOI: /JHEP10(2012)146 > Their weak interaction might be related to very heavy messenger particles. Thus WISPs may open up a window to particle physics at highest energies. Axel Lindner WISPs beyond the SM March 7 th 2013 Page 30 15

16 ALPs and cosmic TeV photons > Axion-like particles might explain the apparent transparency of the Universe for TeV photons: M. Meyer, 7th Patras Workshop on Axions, WIMPs and WISPs, 2011 Axel Lindner WISPs beyond the SM March 7 th 2013 Page 31 ALPs and cosmic TeV photons > Axion-like particles might explain the apparent transparency of the Universe for TeV photons: M. Meyer, 7th Patras Workshop on Axions, WIMPs and WISPs, 2011 TeV photons may hide as ALPs: Axel Lindner WISPs beyond the SM March 7 th 2013 Page 32 16

17 ALPs and cosmic TeV photons > Axion-like particles might explain the apparent transparency of the Universe for TeV photons: Two photon coupling > g aγ GeV -1, m a < 10-7 ev have to be probed! ALP mass M. Meyer, D. Horns, M. Raue, arxiv: [astro-ph.he], accepted by PRD Axel Lindner WISPs beyond the SM March 7 th 2013 Page 33 The big picture: ALPs excluded Two photon coupling Astrophysics hints excluded QCD axion range Excluded by WISP experiments Excluded by astronomy (ass. ALP DM) Excluded by astrophysics / cosmology Axions or ALPs being cold dark matter WISP hints from astrophysics ALP mass Axel Lindner WISPs beyond the SM March 7 th 2013 Page 34 17

18 The big picture: ALPs DOI: /j.dark e-print: arxiv: [hep-ph] QCD axion range Excluded by WISP experiments Excluded by astronomy (ass. ALP DM) Excluded by astrophysics / cosmology Axions or ALPs being cold dark matter WISP hints from astrophysics Sensitivity of next generation WISP exp. Particular interesting: > ALP-photon couplings around GeV -1, masses below 1 mev. This can be probed by the next generation of experiments. Axel Lindner WISPs beyond the SM March 7 th 2013 Page 35 The big picture: ALPs DOI: /j.dark e-print: arxiv: [hep-ph] ALP predictions from large volume scenarios of type IIB string theory. QCD axion range Excluded by WISP experiments Excluded by astronomy (ass. ALP DM) Excluded by astrophysics / cosmology Axions or ALPs being cold dark matter WISP hints from astrophysics Sensitivity of next generation WISP exp. Particular interesting: > ALP-photon couplings around GeV -1, masses below 1 mev. Such ALPs are predicted by string theory. Axel Lindner WISPs beyond the SM March 7 th 2013 Page 36 18

19 The big picture: ALPs ALP predictions from large volume scenarios of type IIB string theory. 10 TeV 10 5 TeV 10 9 TeV Energy scale of new physics Particular interesting: > ALP-photon couplings around GeV -1, masses below 1 mev. Physics at a scale of 10 5 TeV will be probed. Axel Lindner WISPs beyond the SM March 7 th 2013 Page 37 The big picture: hidden photons DOI: /j.dark e-print: arxiv: [hep-ph] Excluded by WISP experiments Excluded by astronomy Excluded by astrophysics and cosmology Dark radiation in the CMB epoch Hidden photons as dark matter Sensitivity of next generation WISP exp. Axel Lindner WISPs beyond the SM March 7 th 2013 Page 38 19

20 Unexplained physics phenomena might hint a Weakly Interacting Slim Particles (WISPs). > Axions and axion-like particles (ALPs, pseudoscalar or scalar bosons) > Hidden photons (neutral vector bosons) > Mini-charged particles > Chameleons (self-shielding scalars) Phenomenon WISPy explanation Solar phenomena Chameleon, ALP White dwarf cooling Axion, ALP TeV transparency ALP CMBR neutrino number HP, Chameleon (?) Dark matter Axion, ALP, HP Dark energy Chameleon to be confirmed! Axel Lindner WISPs beyond the SM March 7 th 2013 Page 39 Unexplained physics phenomena might hint a Weakly Interacting Slim Particles (WISPs). > Axions and axion-like particles (ALPs, pseudoscalar or scalar bosons) > Hidden photons (neutral vector bosons) > Mini-charged particles > Chameleons (self-shielding scalars) Phenomenon WISPy explanation WIMPy explanation Solar phenomena Chameleon, ALP White dwarf cooling Axion, ALP TeV transparency ALP CMBR neutrino number HP, Chameleon (?) Dark matter Axion, ALP, HP LSP Dark energy Chameleon to be confirmed! Axel Lindner WISPs beyond the SM March 7 th 2013 Page 40 20

21 Outline > Physics beyond the Standard Model > Keys to BSM physics and WISPy particles > WISP experiments Laboratory bases Helioscopes Haloscopes > International activities and summary Axel Lindner WISPs beyond the SM March 7 th 2013 Page 41 Directly looking for WISPs Mudie, A Popular Guide to the Observation of Nature (1836, p.144). Axel Lindner WISPs beyond the SM March 7 th 2013 Page 42 21

22 Basics of WISP experiments (I) Weakly Interacting Slim Particles (WISPs) are searched for by converting WISPs to photons (and vice versa) via > kinetic mixing (hidden photons) > the Primakoff effect (axion-like particles) photon + (virtual) photon ALP ALP + (virtual) photon photon A virtual photon can be provided by an electromagnetic field. The Search for Axions, Carosi, van Bibber, Pivovaroff, Contemp. Phys. 49, No. 4, 2008 Axel Lindner WISPs beyond the SM March 7 th 2013 Page 43 Basics of WISP experiments (II) > Basic idea: due to their very weak interaction WISPs may traverse any wall opaque to Standard Model constituents (except ν and gravitons). WISP could transfer energy out of a shielded environment WISP could convert back into detectable photons behind a shielding. > Shining-through-a-wall Okun 1982, Skivie 1983, Ansel m 1985, Van Bibber et al steel wall, cryostat, earth s atmosphere, stellar body, intergalactic background light,. Axel Lindner WISPs beyond the SM March 7 th 2013 Page 44 22

23 Three kinds of WISP searches Weakly Interacting Slim Particles (WISPs) are searched for by > Purely laboratory experiments ( light-shining-through-walls ) optical photons, > Helioscopes (WISPs emitted by the sun), X-rays, > Haloscopes (looking for dark matter constituents), microwaves. Axel Lindner WISPs beyond the SM March 7 th 2013 Page 45 Three kinds of WISP searches Weakly Interacting Slim Particles (WISPs) are searched for by > Purely laboratory experiments ( light-shining-through-walls ) optical photons, > Helioscopes (WISPs emitted by the sun), X-rays, > Haloscopes (looking for dark matter constituents), microwaves. Energy (mass) converted to photons, no scattering experiments possible for µev WISPs Axel Lindner WISPs beyond the SM March 7 th 2013 Page 46 23

24 Three kinds of WISP searches Weakly Interacting Slim Particles (WISPs) are searched for by > Purely laboratory experiments ( light-shining-through-walls ) optical photons, g aγ, J P, m (estimation) > Helioscopes (WISPs emitted by the sun), X-rays, flux g aγ, J, m (estimation) > Haloscopes (looking for dark matter constituents), microwaves. flux g aγ, J P, m Axel Lindner WISPs beyond the SM March 7 th 2013 Page 47 Three kinds of WISP searches Weakly Interacting Slim Particles (WISPs) are searched for by > Purely laboratory experiments ( light-shining-through-walls ) optical photons, Dark matter candidates > Helioscopes (WISPs emitted by the sun), X-rays, Possible DM candidates > Haloscopes (looking for dark matter constituents), microwaves. Dark matter Axel Lindner WISPs beyond the SM March 7 th 2013 Page 48 24

25 Three kinds of WISP searches Weakly Interacting Slim Particles (WISPs) are searched for by > Purely laboratory experiments ( light-shining-through-walls ) optical photons, > Helioscopes (WISPs emitted by the sun), X-rays, WISP flux > Haloscopes (looking for dark matter constituents), microwaves. Axel Lindner WISPs beyond the SM March 7 th 2013 Page 49 Three kinds of WISP searches Weakly Interacting Slim Particles (WISPs) are searched for by > Purely laboratory experiments ( light-shining-through-walls ) optical photons, > Helioscopes (WISPs emitted by the sun), X-rays, Sensitivity > Haloscopes (looking for dark matter constituents), microwaves. Axel Lindner WISPs beyond the SM March 7 th 2013 Page 50 25

26 Three kinds of WISP searches Weakly Interacting Slim Particles (WISPs) are searched for by > Purely laboratory experiments ( light-shining-through-walls ) optical photons, Make the WISPs yourself > Helioscopes (WISPs emitted by the sun), X-rays, Rely on astrophysics > Haloscopes (looking for dark matter constituents), microwaves. Astrophysics + cosmology Axel Lindner WISPs beyond the SM March 7 th 2013 Page 51 Three kinds of WISP searches Weakly Interacting Slim Particles (WISPs) are searched for by > Purely laboratory experiments ( light-shining-through-walls ) optical photons, > Helioscopes (WISPs emitted by the sun), X-rays, > Haloscopes (looking for dark matter constituents), microwaves. Theoretical uncertainty Axel Lindner WISPs beyond the SM March 7 th 2013 Page 52 26

27 WISP experiments worldwide An incomplete selection of (mostly) small-scale experiments: Experiment Type Location Status ALPS-II DESY construction BMV Laboratory Toulouse running CERN microwave experiments, CERN running cavity experiment light-shiningthrough-a-wall CERN OSQAR running REAPR FNAL Proposed CAST CERN running IAXO? proposed Helioscopes SUMICO Tokio running TSHIPS Hamburg started ADMX Seattle, NH running Haloscope WISPDMX DESY in HH first thoughts Axel Lindner WISPs beyond the SM March 7 th 2013 Page 53 WISP experiments worldwide An incomplete selection of (mostly) small-scale experiments: Experiment Type Location Status ALPS-II DESY construction BMV Laboratory Toulouse running CERN microwave experiments, CERN running cavity experiment light-shiningthrough-a-wall CERN OSQAR running REAPR FNAL proposed CAST CERN running IAXO? proposed Helioscopes SUMICO Tokio running TSHIPS Hamburg started ADMX Seattle, NH running Haloscope WISPDMX DESY first thoughts Axel Lindner WISPs beyond the SM March 7 th 2013 Page 54 27

28 DESY in Hamburg MPI PETRA III-Extension CSSB European XFEL PETRA III CFEL FLASH ALPS-I ALPS-II in the HERA tunnel? PETRA III-Extension Axel Lindner WISPs beyond the SM March 7 th 2013 Page 55 ALPS-I at DESY in Hamburg Any Light Particle DESY: ALPS-I concluded in 2010 Axel Lindner WISPs beyond the SM March 7 th 2013 Page 56 28

29 ALPS-I results (PLB Vol. 689 (2010), 149, or > The most sensitivity WISP search experiment in the laboratory (still). > Unfortunately, no light was shining through the wall! laser hut HERA dipole detector /s < /s Axel Lindner WISPs beyond the SM March 7 th 2013 Page 57 Prospects for DESY laser hut HERA dipole detector > Laser with optical cavity to recycle laser power, switch from 532 nm to 1064 nm, increase effective power from 1 to 150 kw. > Magnet: upgrade to straightened HERA dipoles instead of ½+½ used for ALPS-I. > Regeneration cavity to increase WISP-photon conversions, single photon counter (superconducting transition edge sensor?). Axel Lindner WISPs beyond the SM March 7 th 2013 Page 58 All set up in a clean environment! 29

30 The ALPS-II reach Three orders of magnitude gain in ALP coupling and two orders of magnitude in HP mixing! Axel Lindner WISPs beyond the SM March 7 th 2013 Page 59 ALPS-II essentials: laser & optics ALPS-I: basis of success was the optical resonator in front of the wall. > ALPS-IIa Optical resonator to increase effective light flux by recycling the laser power Optical resonator to increase the conversion probability WISP γ Axel Lindner WISPs beyond the SM March 7 th 2013 Page 60 30

31 ALPS-II essentials: laser & optics Production cavity, infrared Wall Regeneraton cavity, locked with green light. Axel Lindner WISPs beyond the SM March 7 th 2013 Page 61 ALPS-II essentials: laser & optics > Optical design based on well established techniques used in the field of gravitational wave detectors. > Several prototype stages to test / demonstrate new challenges and mitigate risk before large investments. > Encouraging first results! Production cavity, infrared Wall Regeneraton cavity, locked with green light. Axel Lindner WISPs beyond the SM March 7 th 2013 Page 62 31

32 ALPS-II will be realized in stages ALPS-I > ALPS-IIa > ALPS-IIb > ALPS-IIc Axel Lindner WISPs beyond the SM March 7 th 2013 Page 63 ALPS-II will be realized in stages ALPS-I > ALPS-IIa Hidden photon search: no magnets > ALPS-IIb > ALPS-IIc Hidden photon search: no magnets Axion-like particle search with magnets Axel Lindner WISPs beyond the SM March 7 th 2013 Page 64 32

33 ALPS-II schedule (rough) ALPS-IIa ALPS-IIb ALPS-IIc installation data runs Any Light Particle Search II -- Technical Design Report arxiv: [physics.ins-det], submitted to JINST Albert Einstein Institute, Hannover DESY in Hamburg University of Hamburg Axel Lindner WISPs beyond the SM March 7 th 2013 Page 65 Sketch of the ALPS-II sensitivity > ALPS-IIc will surpass present day direct and indirect limits. > ALPS-IIc will probe the parameter region proposed by astrophysics phenomena and theory (strings, dark matter). Axel Lindner WISPs beyond the SM March 7 th 2013 Page 66 33

34 The ALPS-II collaboration Axel Lindner WISPs beyond the SM March 7 th 2013 Page 67 The ALPS-II collaboration ALPS-II is a joint effort of > DESY: Babette Döbrich, Jan Dreyling-Eschweiler, Samvel Ghazaryan, Reza Hodajerdi, Friederike Januschek, Ernst-Axel Knabbe, Axel Lindner, Dieter Notz, Andreas Ringwald, Jan Eike von Seggern, Richard Stromhagen, Dieter Trines > Hamburg university: Dieter Horns > AEI Hannover: Robin Bähre, Benno Willke with strong support from > LZH Hannover / neolase: Maik Frede, Bastian Schulz Theory Exp. Particle physics Accelerator physics Surface physics Astronomy Astroparticle physics Laser physics Engineer Axel Lindner WISPs beyond the SM March 7 th 2013 Page 68 34

35 More on ALPS-II > Jan Dreyling-Eschweiler: Aufbau und erste Ergebnisse eines supraleitenden Detektors zum Nachweis einzelner infraroter Photonen für das ALPSII Experiment, T 74.6 Mi 18:00 GER-052 > Jan Eike von Seggern: The ALPS-II Experiment, T 78.8 Do 18:30 WIL-C133 Axel Lindner WISPs beyond the SM March 7 th 2013 Page 69 Helioscopes Axel Lindner WISPs beyond the SM March 7 th 2013 Page 70 35

36 CAST: the dominating helioscope > LHC prototype magnet pointing to the sun. Axions or ALPs from the center of the sun would come with X-ray energies. New J. Phys. 11 (2009) Axel Lindner WISPs beyond the SM March 7 th 2013 Page 71 CAST: the dominating helioscope > LHC prototype magnet pointing to the sun. (courtesy of I. Irastorza) > Most sensitive experiment searching for axion-like particles. Unfortunately no hint for WISPs yet. If an ALP is found, it would be compatible with known solar physics! > However, CAST does not strictly meet the no excuse theorem. CAST has to assume ALP production in the sun. Axel Lindner WISPs beyond the SM March 7 th 2013 Page 72 36

37 More on CAST > Christoph Krieger: An InGrid based Detector for the CAST Experiment, T Di 18:45 HSZ-103 Axel Lindner WISPs beyond the SM March 7 th 2013 Page 73 IAXO proposal > The International Axion Observatory CAST principle with dramatically enlarged aperture Use of a toroid magnet similar to ATLAS arxiv: v3 [hep-ex] Axel Lindner WISPs beyond the SM March 7 th 2013 Page 74 37

38 IAXO proposal > The International Axion Observatory CAST principle with dramatically enlarging the aperture Use of toroid magnet similar to ATLAS X-ray optics similar to satellite experiments. M. Pivovaroff (LLNL), presentation at Fundamental Physics at the Intensity Frontier, Rockville, 2011 Axel Lindner WISPs beyond the SM March 7 th 2013 Page 75 IAXO proposal > The International Axion Observatory ALPS-I CAST principle with dramatically enlarging the aperture Use of toroid magnet similar to ATLAS? > IAXO could reach deep into the region where astrophysical phenomena might indicate the existence of ALPs. arxiv: v3 [hep-ex] ALPS-II (but m < 0.2meV) ALPS-III dream (but m < 0.1meV) Axel Lindner WISPs beyond the SM March 7 th 2013 Page 76 38

39 Haloscopes Axel Lindner WISPs beyond the SM March 7 th 2013 Page 77 Searches for WISPy cold dark matter > Due to their low mass WISPy cold dark matter can not be detected by recoil techniques. > WISPy dark matter particles have to convert into photons in a thoroughly shielded environment. > The mass of the dark matter particle determines the energy to be detected. For axions it is in the microwave range. > The resonance frequency of the cavity is to be tuned to the WISP mass to be probed. This is a time consuming process! Axel Lindner WISPs beyond the SM March 7 th 2013 Page 78 The Search for Axions, Carosi, van Bibber, Pivovaroff, Contemp. Phys. 49, No. 4,

40 ADMX > Existing experiment at Washington university. The Search for Axions, Carosi, van Bibber, Pivovaroff, Contemp. Phys. 49, No. 4, 2008 > ADMX-HF in preparation at Yale. > Both experiments could probe a large part of the parameter space for dark matter axions! G. Carosi (LLNL), presentation at Fundamental Physics at the Intensity Frontier, Rockville, 2011 Axel Lindner WISPs beyond the SM March 7 th 2013 Page 79 New possibilities by combining forces > Dark matter searched for by particle physicists and radio astronomers MPIfR (A. Lobanov, R. Keller, M. Kramer) DESY (A.L.,A. Lobanov, W.-D. Möller, A. Ringwald, J. Sekutowicz,D, Trines, A. Westphal) ITP Heidelberg (J. Jaeckel) > Combine accelerator cavities, detector magnets with receivers from radio astronomy? Axel Lindner WISPs beyond the SM March 7 th 2013 Page

41 A new way of broadband DM seaches? DESY , MPP , arxiv: [hep-ph] > The photonic component of a WISP excites electromagnetic radiation emitted by a conducting surface. > This radiation is emitted perpendicular to the surface and can be focused onto a detector. > This works for a broad range of WISP masses, given by the mirror reflectivity. > A lacking resonance enhancement (ADMX) can be compensated for by a large mirror surface. Axel Lindner WISPs beyond the SM March 7 th 2013 Page 81 A new way of broadband DM seaches? > The cold DM WISP em. radiation is focused in the center of a spherical mirror. > Already a 1 m 2 dish could allow to reach high sensitivities. Axel Lindner WISPs beyond the SM March 7 th 2013 Page 82 41

42 Outline > Physics beyond the Standard Model > Keys to BSM physics and WISPy particles > WISP experiments Laboratory bases Helioscopes Haloscopes > International activities and summary Axel Lindner WISPs beyond the SM March 7 th 2013 Page 83 International activities > Input to the discussion on the future European strategy on particle physics: sid=0&confid= Document written by international authors! Axel Lindner WISPs beyond the SM March 7 th 2013 Page 84 42

43 Activities (selected) in the US > November 2011: Fundamental Physics at the Intensity Frontier (Rockville) > April 2012: Vistas in Axion Physics (Seattle) > Snowmass 2013: (Snowmass on the Mississippi) Minneapolis, July 29 Aug. 6, 2013, see Among others: Working group on the Intensity Frontier including a sub-group New Light, Weakly Coupled particles Axel Lindner WISPs beyond the SM March 7 th 2013 Page 85 Patras workshop series > Workshop on WIMPs and WISPs! Workshop 2014: CERN Axel Lindner WISPs beyond the SM March 7 th 2013 Page 86 43

44 Keys to beyond SM physics WISPs Symmetry magazin, August 2006 Axel Lindner WISPs beyond the SM March 7 th 2013 Page 87 Summary > Weakly Interacting Slim Particles might explain puzzles from cosmology, astrophysics and particle physics. > With the recent developments in theory and astrophysics phenomena we know where to go for axion-like particles and hidden photons. > Next generation experiments are being constructed or prepared with sensitivities allowing to probe these predictions. > One should exploit carefully new options provided by high power pulsed laser systems, large existing magnets or new approaches for dark matter searches for example. > Small scale and short term WISP experiments offer a fascinating complement to accelerator based big science. > There is plenty of room for new ideas and quick experiments having the potential to change the (particle physicist s) world! Axel Lindner WISPs beyond the SM March 7 th 2013 Page 88 44

45 Backup slides Axel Lindner WISPs beyond the SM March 7 th 2013 Page 89 ALPs in LSW experiments > The production (and re-conversion) of WISPs takes place in a coherent fashion. For ALPs (Φ): q = p γ p Φ l: length of B field With P γ Φ =P Φ γ = P 1/2 : g = (P) 1/4 2 / (L B) / F 1/2 P = (photon flux behind wall) / (flux before wall) / (power built-up in cavity behind wall) Axel Lindner WISPs beyond the SM March 7 th 2013 Page 90 45

46 Hidden photons in LSW experiments > The production (and re-conversion) of WISPs takes place in a coherent fashion. With P γ γ =P γ γ = P 1/2 : χ = (P) 1/4 P = (photon flux behind wall) / (flux before wall) / (power built-up in cavity behind wall) Axel Lindner WISPs beyond the SM March 7 th 2013 Page 91 ALPS-II essentials: detector Transition Edge Sensor (TES) > Very high quantum efficiency, also at 1064 nm. > Very low noise. > Difficult to operate around 100 mk. Axel Lindner WISPs beyond the SM March 7 th 2013 Page 92 46

47 ALPS-II essentials: detector > Refrigerator: ADR (Adiabatic Demagnetisation Refrigerator) > Sensors from NIST and AIST Axel Lindner WISPs beyond the SM March 7 th 2013 Page 93 ALPS-II essentials: magnets The aperture of the magnets determines the lenghts of the optical cavities: > The laser beam diverges and clipping is to be avoided to not spoil the power built-up in the cavities. Eff. dipole aperture Max. # of dipoles B L (Tm) HERA LHC HERA LHC 35 mm (HERA) mm (LHC) mm 55 mm (HERA almost straight) (HERA straight) HERA dipoles are competitive with LHC dipoles, if one could get them straight! > Challenge: develop (cheap) straigthening procedure for HERA dipole magnets! Axel Lindner WISPs beyond the SM March 7 th 2013 Page 94 47

48 ALPS-II essentials: magnets Axel Lindner WISPs beyond the SM March 7 th 2013 Page 95 ALPS-II essentials: magnets Axel Lindner WISPs beyond the SM March 7 th 2013 Page 96 48

49 ALPS-II essentials: magnets Axel Lindner WISPs beyond the SM March 7 th 2013 Page 97 ALPS-II essentials: magnets > The first test of the procedure was already a full success! > Presently the straightening procedure is being revised and improved. Axel Lindner WISPs beyond the SM March 7 th 2013 Page 98 49

50 Beyond ALPS-II > On the longer run one could strive for an ALPS-III : New dipoles based on developments for LHC energy upgrade: B = 13T, aperture 100 mm: gain in B L by a factor of about 10. Increasing the cw laser power to a few MW. Reach for ALP couplings down to GeV -1! However, only light ALPs with masses below 0.1 mev could be searched for! Axel Lindner WISPs beyond the SM March 7 th 2013 Page 99 Beyond ALPS-II > Crucial parameters: Experiment Photon flux (1/s) Photon E (ev) B (T) L (m) B L (Tm) Mass reach (ev) ALPS-I ALPS-II ALPS-III European XFEL < PW laser /pulse ALPS-III would improve the sensitivity in g aγ of ALPS-II by a factor 25. It would be a real European enterprise. Axel Lindner WISPs beyond the SM March 7 th 2013 Page

51 TSHIPS Telescope for Solar Hidden Photon Search DESY Hamburger University (observatory Bergedorf) Axel Lindner WISPs beyond the SM March 7 th 2013 Page 101 TSHIPS-I potential Significant improvement compared to present experimental sensitivities! Axel Lindner WISPs beyond the SM March 7 th 2013 Page

52 TSHIPS-I status previously now > Hope for first light soon! > For more details see: Axel Lindner WISPs beyond the SM March 7 th 2013 Page 103 Exploit the possibilties of other magnets DOI: /PhysRevD , arxiv: v1 [physics.ins-det] Experiments with toroid (IAXO),dipole and wiggler magnets could complement ADMX (using a solenoid). Axel Lindner WISPs beyond the SM March 7 th 2013 Page

53 Options with Tore Supra > Use large magnetic volume equipped with microwave cavities to search for dark matter ALPs and axions. Experiment B (T) V (m 3 ) B 2 V (T 2 m 3 ) ADMX Tore Supra > However, Tore Supra cannot be (easily) cooled down to a few K. > Questions Is the electromagnetic noise within the magnet tolerable? Is it possible to use the magnet as a cavity at its fundamental resonance at about 145 MHz (0.6 µev)? What is the Q value here? Is it possible to assemble a number of smaller cavities inside the magnet? Does a broad spectral range search for dark matter make sense (Q=1)? Axel Lindner WISPs beyond the SM March 7 th 2013 Page 105 Axel Lindner WISPs beyond the SM March 7 th 2013 Page

54 WI(S)P searches at LHC IPPP/12/94; DCPT/12/188 arxiv: [hep-ph] HP ALP > LHC can probe couplings much weaker than the typical values of the visible sector. > However, there is hardly any sensitivity for lightweight particles, which are of cosmological relevance. Axel Lindner WISPs beyond the SM March 7 th 2013 Page 107 Input to the discussion on the future European strategy on particle physics: > In searches for WISPs as a Dark Matter component a variety of new experimental approaches have recently emerged and deserve serious attention, as they may yield an experimental program complementary to and competitive with the leading US Axion Dark Matter search experiment (ADMX). > In searches for WISPs emitted by the sun the proposal for an International AXion Observatory (IAXO) stands out as a larger scale follow-up of the successful CAST helioscope at CERN. > In purely laboratory based WISP searches the proposal for Any Light Particle Search (ALPS-II) at DESY offers leading prospects for this technique worldwide. Although significant challenges remain, the rewards of exploring the lowenergy frontier of particle physics could be enormous. Looking through the low-energy window may reveal fundamental insights on the underlying structure of nature and shed light on such important mysteries as the origin of Dark Matter and Dark Energy. Axel Lindner WISPs beyond the SM March 7 th 2013 Page

55 A new way of broadband DM seaches? > The spatial distribution of photons in a CCD detector would allow to determine our relative movement with respect to the dark matter. Simulation by J. Jaeckel Axel Lindner WISPs beyond the SM March 7 th 2013 Page