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

1

• 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

2

3

=> 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:

4

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

7

» 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

9

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

10

11

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

12

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

13

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

14

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

15

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)

17

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

18

• [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

19

Yannis Semertzidis, BNL19 March 2012

Tore Supra’… … relics sensitivity first estimate

ALPS / DESY

CAST

ADMX

300K300K3K 30mK

20

Khoury, Weltman 20042004

Chameleons … to explain DE

… solar CHameleons!

23

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!

24

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

27

28

..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.

31

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

32

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!!?!!?

33

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

36

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!!

37

31

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

13

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]

14

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

34

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