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K. Zioutas University of Patras / Greece

Cross - disciplinary axion ↔ chameleon detection + ID. DM. DE. Equipment / people. > novel concept … a by-product. K. Zioutas University of Patras / Greece + O.K. Baker, A. Lindner, Y.K. Semertzidis, A. Upadhye.

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K. Zioutas University of Patras / Greece

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  1. Cross-disciplinary axion↔chameleon detection+ID DM DE Equipment / people >novel concept … a by-product K. Zioutas University of Patras / Greece + O.K. Baker, A. Lindner, Y.K. Semertzidis, A. Upadhye Benefitted from: CERN, CAST + M. Betz, P. Brax, F. Caspers, J. Harris, M. Tsagri, J.-C. Vallet at al. / Tore Supra, L. Walckiers, … Vistas in Axion Physics: A Roadmap for Theoretical and Experimental Axion Physics through 2025 UW,Seattle / USA April 23-26, 2012 1

  2. Related work … • CAST search for sub-eV mass solar axions with 3He buffer gas. • The CAST Collaboration, S. Aune et al, Phys. Rev. Lett.107 (2011) 261302 • “Results from CAST … searches”, T. Papaevangelou, Moriond (March 2012): • http://indico.in2p3.fr/getFile.py/access?contribId=70&sessionId=11&resId=0&materialId=slides&confId=6001 • Prospects for Searching Axion-like Particle Dark Matter • with Dipole, Toroidal and Wiggler Magnets • O.K. Baker, M. Betz, F. Caspers, J. Jaeckel, A. Lindner, • A. Ringwald, Y. Semertzidis, P. Sikivie, K. Zioutas, Phys. Rev. D85 (2012) 035018 • Detection prospects for solar and terrestrial chameleons • P. Brax, A. Lindner, K. Zioutas, Phys. Rev. D85 (2012) 043014. • A chameleon helioscope • O.K. Baker, A. Lindner, A. Upadhye, K. Zioutas, arXiv:1201.0079v1 • Detection of radiation pressure from solar chameleons • O.K. Baker, A. Lindner, Y.K. Semertzidis, A. Upadhye, K. Zioutas, arXiv:1201.6508v1 … and ref’s therein 2

  3. Axion,Chameleons,WISPstosolveastrophysical puzzles • =>γ↔ALP oscillations? • Dark energy mCHameleon = f(density) • Dark matter maxion~1-1000μeV/c2 • HE -transparency mALP< 10-10eV/c2 / gaγγ ~ 10-12 GeV-1 • Chameleon instead?! • WD fast cooling maxion~10 meV/c2 • Solar corona heating maxion~17 meV/c2 • ~transparency • SN1987Amaxion ≤10 meV/c2 “Open questions”  new physics?! 3

  4. >> Motivation – encouragement for: • Telescopes: solar / relics • + Natural T. •  @ work => direct signatures! •  copy their workings • RECYCLING  gain: time, $$, R&D, people (collaborators) •  accelerating science cost efficiently, • e.g., CAST 4

  5. CAST:axionhelioscope+… CASTA superconducting LHC test-dipole tracks the Sun 2x1.5hours @ Sunrise/Sunset. Operation at T=1.8 K, I=13,000A, B=9T, L=9.26m, 4x14.5 cm2 A difficult experiment: the only moving telescope @ 1.8K (!?) Expected signal X-Ray excess during tracking @1-10 keV Axion flux on earth Ea=4.2 keV CAST sensitivity per detector 0.3 counts/hour for gaγγ= 10-10 GeV-1 and A = 14.5 cm2 5 More see in http://indico.in2p3.fr/getFile.py/access?contribId=70&sessionId=11&resId=0&materialId=slides&confId=6001

  6. CAST: Solar axion / chameleon ID » Signal / Noise Signal + background rare! The recycled CAST XRTelescope With CCD at focal plane expected axion signal

  7. … 2012 run CAST preliminary results for ma>0.64 eV/c2 2012 CAST 2012 10 trackings per density step, starting @ 0.4 eV (≈15.5 mbar) improved sensitivity 9

  8. … tbd CAST:also ~axionhaloscope+… …CHameleonhelioscope(+haloscope?) • Relics • CAST  Tore Supra / Tokamak • Need: MW antenna/cavitiesinsideB  ma≈0.1–100 μeV/c2 …tbd • Solar axions(CAST) • Need: « X-raybckg. det’s + XRTsbestlimitfor ma<0.02 eV/c2 • Solar Chameleons • CAST Tore Supra new ! • Need:~eV-keVthresholddet’sbestsensitivity 10

  9. CDM axion search ALPS / DESY CAST ADMX CDM axions / ALPs

  10. >>experimental Challenge!! Alternative magnets as haloscopes CAST DESY ATLAS  IAXO Tore Supra Dipole Toroidal magnets L. Walckiers / CERN Wiggler 1st exploratory meeting on Tore Supra, CERN, 19/3/2012 TE – modes couple to axions 12

  11. … tbd Expected sensitivity Existing bounds for axionlike particles. The QCD-axion region is marked as the hatched band. In the orange region, axions are a natural candidate for DM. In the lighter shaded orange area, axions can still be DM, but with decreasing mass, this requires an increasing amount of fine tuning. Axion-like particles can be dark matter in a large part of the so-far untested parameter space. The right green (red) regions are the conservatively (realistically) expected sensitivity of a dipole or wiggler search for axion-like particle DM. The left green/red region shows the masses and couplings that could be probed in a setup with a toroidal magnet. OK Baker, et al., PRD85 (2012)035018 13

  12. F. Caspers / CERN Box-in-the-box principle (3 GHz) Table-top particle physics! E2-field suppression ~300dB ~10-30 M. Betz, F. Caspers CERN 14 See M. Betz, in PATRAS2011http://axion-wimp2011.desy.de/e102694/e102699/e118290/Betz-M.pdf

  13. >> Tore Supra RF cavities inside toroidal magnets JC Vallet • Tore Supra = one of the largest Tokamaks FREE NOW!! • V = 30m3& B = 4.5 T • RF Heating Systems: • - 47-54 MHz : 12 MW x40s • - 3.7 GHz :       8 MW cw • - 118 GHz :       1 MW x 5s • ITER~2018 completion, start torus pump-down • ~10x F. Caspers / CERN: “Either with single big cavities for low axion mass ma or with an array of smaller cavities for larger axion masses >> it’s delicate: each cavity has to be controlled individually, +in terms of its resonance frequency, independently” >>> tbd  15

  14. Tokamak, as relics haloscope Tore Supra The magnetic field converts relic axions to MW photons, which excite the TE011 mode. axions Photons Test signal The inner walls might have to be covered by copper sheets, to achieve higher Q factors and better EMI shielding A test signal is required in order to proof that for zero result the detector was working properly. This test signal is recommended to be used during the whole run; it should be near the res-frq but not at resonance. The microwave signal is coupled out by a small antenna and amplified. A commercial spectrum analyzer can be used to detect the axion signal. 16 M. Betz, F. Caspers / CERN

  15. Tore Supra as relics haloscope Preliminary simulation results E–field of TE011 mode (ECAV) in TS cavity • Inner radius: 0.8m, outer radius: 2.4m • TE011 = H011 mode, f = 145.601MHz  Most sensitive to axions with ma=6∙10-7eV Static magnetic field of superconducting coils (B0) 17

  16. Tore Supra as relics haloscope M. Betz / CERN Expected sensitivity With the rather conservative parameters on the left (QL=1000 &Pdet=5.5∙10-22W),in 9h one could reach: gaγγ=7∙10-16 GeV-1 18

  17. Tore Supra as relics haloscope • [ADMX]: ~1m3(low frequency cavity), 7.6T; B2V ~50T2m3 near quantum limit! • Torre Supra: ~35m3, 4T; B2V~500T2m3 Low frequency cavity @ ~150MHz NEW Without cavity mode? F. Caspers / CERN Higher axion rest mass, in a large volume (Lcoh~10–100m) lose a factor of Q~105 in production rate, but wideband! Y.K. Semertzidis / BNL outcome? 19

  18. Yannis Semertzidis, BNL Tore Supra’… … relics sensitivity first estimate ALPS / DESY CAST  ADMX 300K 3K 30mK 20

  19. Chameleons … to explain DE Khoury, Weltman 2004 … solar CHameleons! 23

  20. In CAST: Converted Solar Chameleons: CAST, …, space Vacuum:  CH γ~10-13 axionγ ~10-17 vacuum 0.1 mbar [keV] CH conversion in vacuum with: BL=90Tm & βm=106 / βγ=1010.32. LE saturation! The analogue spectrum [h-1 keV-1] of regenerated photons as predicted to be seen by CAST: βm=106, B=30T in a shell of width 0.01Rsolar around the tachocline (~0.7Rsolar). [keV]  Low energy threshold: MM, CCD, …?! + vacuum The effective mass of the chameleon inside the CAST pipe in vacuum is: mch = 40μeV/c2 24

  21. XRT: Chameleon helioscope ~100-1000x enhanced ΦCH!! Tore Supra  double measurement!! enter βγ & βm CAST Eγ,CH>50–100eVX-Ray Telescope = Chameleon telescope Eγ,CH<10–50eV~any Telescope= Chameleon telescope 27 O.K. Baker, A. Lindner, A. Upadhye, K. Zioutas, arXiv:1201.0079v1 [astro-ph.SR]

  22. Detection of radiation pressure from solar chameleons ..on a foil arXiv:1201.6508v1 [astro-ph.IM] Equipment? … Finally, optomechanical experiments might be the mostly sensitive devices to react on an additional external radiation pressure component like that from solar chameleons. For example, the measured frequency drifts or the temporally observed irregularities in Figure 5.9 of [14] are of potential interest to be followed further; in particular, in case the observed behaviour resembles solar diurnal behaviour or other solar activity during the time period this measurement was performed. Therefore, such or other experiments being sensitive to external radiation pressure, when performed over longer time periods, i.e. at least one day, a correlation to solar activity should be searched for. Last but not least, the highest sensitivity of Gravitational Waves antennas might be of potential interest, provided their unprecedented sensitive performance is re-considered following the reasoning of this work about an ubiquitous dark radiation pressure. . A new concept! 28

  23. Optical cavity Massm &FrequencyωΜ 10-50 nm Membrane, ~50ngram … with a movable end mirror ~pendulum. Pcirc ~2-3 mm (r1,t1) Cavity length L ~7mm (r2,t2) 31

  24. RT force threshold≈10-16N ≈ 20nW nanogram - nanometers 6nN=1W ?some overlooked signal? Sensitivity ~ 20nW/cm2@RTJack Harris / Yale U. ΦsolarCHam.<15mW/cm2  “Contigency” ~106 32

  25. Resonant frequency drift … of the membrane in 1h run. origin?? “repeatedly” [Jack Harris/Yale U.] Solar / celectial CHs!!? B.M. Zwickl, Progress Toward Observation of Radiation Pressure Shot Noise, PhD-thesis, Yale University (2011) ( http://www.yale.edu/harrislab/docs/Zwickl_Thesis.pdf ) . 33

  26. Cosmic CHameleons same spectrumwith ΦCH ≤ 0.3Φγ-CR Optical IR O.K. Baker, K.Z. …the total probability to ALPs saturates to 1/3, which is the maximum (theoretical) attenuation. Chameleons http://www.aanda.org/index.php?option=com_article&access=standard&Itemid=129&url=/articles/aa/full/2006/20/aa4446-05/aa4446-05.right.html H. Dole et al., A&A 451 (2006) 417 36

  27. Thanks Sun!! 37

  28. Back-up slides

  29. Tore Supra as relics haloscope Can we improve with B2V~500T2m3? • Lose a factor of Q~105 in production rate; overall lose a factor of 3x102 in S/N (for same total integration time). We gain a factor of 10 in B2V. Hence S/N loss ~30. • If the receiver noise is 103 times higher (102 from temperature and 10 from frequency range) Another S/N loss of ~30. • Then the overall lost factor in S/N is 103. The coupling is worse by 30-100. • Overall the expected sensitivity is ~10-13GeV-1@~10GHz axion mass range. 19 March 2012 Yannis Semertzidis, BNL 19a

  30. Yannis Semertzidis, BNL Tore Supra… Opportunities on both sides, low + high frequency axions. see O.K. Baker, et al., PRD D85 (2012) 035018 19b

  31. Maximum energy at which a chameleon particle can be focused by an X-ray mirror with density 10g/cm3 (≈ the density of a Ni-coated X-ray telescope) and grazing angle ε, for several different chameleon models. The dotted horizontal and vertical lines illustrate one example of a 600 eV chameleon incident on a mirror of focusing angle 30', which is, for example, equal to the field-of-view of XMM/Newton. The chameleon will be focused by this mirror if n=4 and βm=106, but will pass through the mirror if n=1 and βm=104. K. Baker, A. Lindner, A. Upadhye, K. Zioutas, arXiv:1201.0079v1 [astro-ph.SR]

  32. Minimum chameleon energy ω required for transmission through the atmosphere to the Earth’s surface. The atmosphere has at sea level a density of ρm ≈1.2·10−3g/cm3. (left) The minimum energy at normal incidence is the chameleon mass in the atmosphere, shown as a function of βmand n. (right) Chameleons at nonzero incident angles θ require greater energies for transmission, i.e., when the chameleons hit the plane of the denser surface less and less perpendicularly, more and more energetic chameleons can be reflected K. Baker, A. Lindner, A. Upadhye, K. Zioutas, arXiv:1201.0079v1 [astro-ph.SR]

  33. Take for sure B ~0.1pTesla  BL ~ 109Tm ~ 107xCAST http://axion-wimp2010.desy.de/e80839/e80847/e92594/100706_montanino.pdf …the total probability saturates to 1/3  33% of the photons can convert into ALPs, which is the maximum (theoretical) attenuation.  Chameleons E.g.,A. Mirizzi, G. G. Raffelt, P. Serpico, Phys. Rev. D 76, 023001 (2007); M. A. SANCHEZ-CONDE et al., PHYSICAL REVIEW D 79, 123511 (2009) http://prd.aps.org/pdf/PRD/v79/i12/e123511 34

  34. although it is well established that the ultimateenergy source is the coronal magnetic field, the question of how the magnetic energy is transformed to heat the coronal plasma is still to be solved. ... one important issue is whether theheating is released gradually + continuously or in the form of discrete, rapid and intensepulses. http://xxx.lanl.gov/pdf/1204.0041.pdfApril 2012

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