k. zioutas university of patras / greece + + o.k. baker, a. lindner, y.k. semertzidis, a. upadhye...
TRANSCRIPT
K. ZioutasUniversity 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
Equipment / people DE
Cross-disciplinary axion ↔↔ chameleon detection ++ IDDM
>> novel concept … a by-product
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• 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
Related work …
… and ref’s therein
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=> γ↔ALP oscillations?
• Dark energy mCHameleon = f(density)
• Dark matter maxion ~1 - 1000 μeV/c2
• HE - transparency mALP < 10-10 eV/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?!
Axion, Chameleons, WISPs to solve astrophysical puzzles
• 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
>>>> Motivation – encouragement for:
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CAST sensitivity per detector
0.3 counts/hour forgaγγ= 10-10 GeV-1 and A = 14.5
cm2
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
2
GeV10
g110
aγ
Ea=4.2 keV
Axion flux on earth
CAST: axion helioscope ++ …
More see in http://indico.in2p3.fr/getFile.py/access?contribId=70&sessionId=11&resId=0&materialId=slides&confId=6001 5
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» Signal / NoiseSignal ++ background
With CCD at focal plane
rare! expected
axion signal
The recycled CAST XRTelescope
CAST: Solar axion / chameleon ID
CAST preliminary results for ma > 0.64 eV/c2
10 trackings per density step, starting @ 0.4 eV (≈15.5 mbar) improved sensitivity
2012
CAST 2012
… 2012 run
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CAST: also ~axion haloscope ++ …
…… CHameleon helioscope (++ haloscope ?)?)
• Relics CAST Tore Supra / Tokamak Need: MW antenna/cavities inside B ma ≈ 0.1 – 100 μeV/c2 …tbd
• Solar axions (CAST) Need: « X-ray bckg. det’s + XRTs best limit for ma <0.02
eV/c2
• Solar Chameleons
CAST Tore Supra new !
Need: ~eV-keV threshold det’s best sensitivity
… tbd
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ALPS / DESY
CAST
ADMX
CDM axion search
CDM axions / ALPsCDM axions / ALPs
Alternative magnets as haloscopes
DipoleWiggler Toroidal magnets
L. Walckiers / CERN
CAST DESY ATLAS IAXO Tore Supra
1st exploratory meeting on Tore Supra, CERN, 19/3/2012
>> experimental Challenge!!
TE – modes couple to axions
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Expected sensitivity
OK Baker, et al., PRD85 (2012)035018
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.
… tbd
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Box-in-the-box principle (3 GHz)
Table-top particle physics!!
See M. Betz, in PATRAS2011 http://axion-wimp2011.desy.de/e102694/e102699/e118290/Betz-M.pdf
F. Caspers / CERN
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E2-field suppression ~300dB ~10-30
M. Betz, F. Caspers CERN
RF cavities inside toroidal magnets
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
>> >> Tore Supra
JC Vallet
• Tore Supra = one of the largest Tokamaks FREE NOW!!
• V = 30 m3 & B = 4.5 T
RF Heating Systems:
-- 47-54 MHz : 12 MW x 40s -- 3.7 GHz : 8 MW cw -- 118 GHz : 1 MW x 5s
• ITER ~2018 completion, start torus pump-down ~10x
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axions
The magnetic field converts relic axions to MW photons, which excite the TE011 mode.
Photons
Test signal
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 inner walls might have to be covered by copper sheets, to achieve higher Q factors and better EMI shielding
The microwave signal is coupled out by a small antenna and amplified. A commercial spectrum analyzer can be used to detect the axion signal.
Tore Supra Tokamak, as relics haloscope
M. Betz, F. Caspers / CERN 16
Preliminary simulation results
• Inner radius: 0.8m, outer radius: 2.4m
• TE011 = H011 mode, f = 145.601 MHz
Most sensitive to axions with
ma = 6∙10-7 eV
Wall material Conductivity
Unloaded Q
Stainless steel 9.8e+5 S/m
19271
Copper 5.8e+7 S/m
148250
Tore Supra as relics haloscope
E–field of TE011 mode (ECAV) in TS cavity Static magnetic field ofsuperconducting coils (B0)
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Expected sensitivityWith 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
Tore SupraCavity volume V 30300 lMagnetic field B 4.5 TAxion density pa 3.00E+02 Mev/cm^3
Geometry factor C 0.39 Geometry factorAxion mass ma 6.00E-07 eV
Loaded Q factor Q 1.00E+03Desired signal/noise SNR 2.0System noise temp. Tn 300 KCoupling parameter gayy 7.00E-16 GeV^-1
Relic axion velocity spread Qa 1.00E+06
Minimum meas. Time t 3.18E+04 st 8.8 h
Tore Supra as relics haloscope M. Betz / CERN
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• [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 – 100 m) lose a factor of Q ~
105 in production rate, but wideband! Y.K. Semertzidis / BNL
outcome?
Tore Supra as relics haloscope
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Yannis Semertzidis, BNL19 March 2012
Tore Supra’… … relics sensitivity first estimate
ALPS / DESY
CAST
ADMX
300K300K3K 30mK
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Khoury, Weltman 20042004
Chameleons … to explain DE
… solar CHameleons!
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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).
The effective mass of the chameleon inside the CAST pipe in vacuum is: mch = 40 μeV/c2
[keV]
vacuum 0.1 mbar
[keV]
Converted Solar Chameleons: CAST, …, space
Vacuum:
CH γ ~10~10-13-13
axion γ ~10-17
In CAST: Low energy threshold: MM, CCD, …?! ++ vacuum
CH conversion in vacuum with: BL=90Tm & βm=106 / βγ=1010.32.
LE saturation!
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XRT: Chameleon helioscope
O.K. Baker , A. Lindner , A. Upadhye , K. Zioutas, arXiv:1201.0079v1 [astro-ph.SR]
enter βγ & βm
Tore Supra
CAST
double measurement!!
~100-1000x enhanced ΦCH !!
Eγ,CH > 50 – 100 eV X-Ray Telescope = Chameleon telescope
Eγ,CH < 10 – 50 eV ~any Telescope = Chameleon telescope
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..on a foil
A new concept!
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.
.
Detection of radiation pressure from solar chameleons
Optical cavity … with a movable end mirror ~pendulum.
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Pcirc
Mass m & Frequency ωΜ
10-50 nm Membrane, ~50 ngram
(r1,t1)
Cavity length L ~7mm
(r2,t2)
~2-3 mm
? some overlooked signal?
RT force threshold ≈ 10-16N ≈ 20nW
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Sensitivity ~ 20 nW/cm2 @@ RT Jack Harris / Yale U.
ΦsolarCHam. <15 mW/cm2 “Contigency” ~106
6nN=1W
nanogram - nanometers
Resonant frequency drift
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 ) .
… of the membrane in 1 h run.
origin??
“repeatedly” [Jack Harris/Yale U.]
Solar / celectial CHs!!?!!?
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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
Cosmic CHameleons
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O.K. Baker, K.Z.
…the total probability to ALPs saturates to 1/3, which is the maximum (theoretical) attenuation. Chameleons
same spectrum with
ΦCH ≤ 0.3Φγ-CR
IROptical
Thanks Sun!!
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Back-up slides
• 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.
Can we improve with B2V~500T2m3?
Tore Supra as relics haloscope
Yannis Semertzidis, BNL19 March 201219a
Opportunities on both sides, low + high frequency axions.
see O.K. Baker, et al., PRD D85 (2012) 035018
Yannis Semertzidis, BNL
Axion range coverage
Central frequency[GHz]
Quality factor Q
Receiver noise T [K]
Axion coupling[GeV-1]
5GHz/y 0.150 103 300 2x10-15
5GHz/y 0.150 103 3 2x10-16
5GHz/y 0.150 103 0.03 2x10-17
5GHz/y 10 1 300 10-13
5GHz/y 10 1 3 10-14
5GHz/y 10 1 0.03 10-15
19 March 2012
Tore Supra…
19b
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Maximum energy at which a chameleon particle can be focused by an X-ray mirror with density 10 g/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]
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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 βm and 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]
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
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although it is well established that the ultimate energy 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 the heating is released gradually + continuously or in the form of discrete, rapid and intense pulses.
http://xxx.lanl.gov/pdf/1204.0041.pdf April 2012