New experiment for axion dark matter

New experiment for axion dark matter J. Redondo and J. Jaeckel Feb 27th 2014

Outline - x-summary of Axion and ALP DM - Axion DM waves in Magnetic fields - Dish experiment - Understanding cavity experiments

QCD axion DM f - strong CP problem - Peccei Quinn - a - a - m a axion mass m a =6meV 109 GeV f a coupling to two photons Lg aγ B E a α g aγ = c γ 2πf a - Axion CDM from initial misalignment + decay of topological defects All throughout this talk = c = k B =1 1

QCD axion cold dark matter (two scenarios) f a GeV 10 14 10 13 10 12 10 11 10 10 10 9 10 8 10 7 10 6 10 5 10 4 10 3 10 2 10 1 1 String decay 2.0 Misalignment postinflation PQ 1.5 Cold DM (realignment+cosmic strings+dws) 1.0 preinflation PQ 0.5 WD cooling hint (only realignment) 0.0 ADMX ADMX II Burst Duration g ae Hot DM CMB BBN Random Telescope conditions EBL SK Globular Clusters g aγ White Dwarfs g ae Same a 1 g ae a 1 ( πf a,πf a ) Solar Neutrino flux g aγ SN1987A everywhere but which? IAXO Helioscopes Beam Dump 0.5 10 7 10 6 10 5 10 4 10 3 10 2 10 1 1 10 10 2 10 3 10 4 10 5 10 6 10 7 m a ev

+ Bounds on axions (and prospects) f a GeV 10 14 10 13 10 12 10 11 10 10 10 9 10 8 10 7 10 6 10 5 10 4 10 3 10 2 10 1 1 2.0 String decay Hot DM CMB BBN Misalignment postinflation PQ 1.5 Cold DM (realignment+cosmic strings+dws) 1.0 preinflation PQ 0.5 WD cooling hint (only realignment) 0.0 ADMX ADMX II Burst Duration g ae Telescope EBL SK SN1987A Globular Clusters g aγ White Dwarfs g ae g ae Solar Neutrino flux g aγ IAXO Helioscopes Beam Dump 0.5 10 7 10 6 10 5 10 4 10 3 10 2 10 1 1 10 10 2 10 3 10 4 10 5 10 6 10 7 m a ev

+ Bounds on axions (and prospects) f a GeV 10 14 10 13 10 12 10 11 10 10 10 9 10 8 10 7 10 6 10 5 10 4 10 3 10 2 10 1 1 String decay 2.0 Misalignment postinflation PQ 1.5 Cold DM (realignment+cosmic strings+dws) 1.0 preinflation PQ 0.5 WD cooling hint (only realignment) 0.0 ADMX ADMX II Burst Duration g ae Hot DM CMB BBN Excluded Telescope EBL by experiments SK and Globular Clusters g aγ White Dwarfs g ae SN1987A stellar evolution g ae Solar Neutrino flux g aγ IAXO Helioscopes Beam Dump 0.5 10 7 10 6 10 5 10 4 10 3 10 2 10 1 1 10 10 2 10 3 10 4 10 5 10 6 10 7 m a ev

+ Bounds on axions (and prospects) f a GeV 10 14 10 13 10 12 10 11 10 10 10 9 10 8 10 7 10 6 10 5 10 4 10 3 10 2 10 1 1 Excluded(?) String decay 2.0 postinflation Misalignment PQ Ω 1.5 (realignment+cosmic cdm h 2 > 0.11 strings+dws) 1.0 Cold DM preinflation PQ 0.5 WD cooling hint (only realignment) 0.0 ADMX ADMX II Burst Duration g ae Hot DM CMB BBN Excluded Telescope EBL by experiments SK and Globular Clusters g aγ White Dwarfs g ae SN1987A stellar evolution g ae Solar Neutrino flux g aγ IAXO Helioscopes Beam Dump 0.5 10 7 10 6 10 5 10 4 10 3 10 2 10 1 1 10 10 2 10 3 10 4 10 5 10 6 10 7 m a ev

+ Bounds on axions (and prospects) f a GeV 10 14 10 13 10 12 10 11 10 10 10 9 10 8 10 7 10 6 10 5 10 4 10 3 10 2 10 1 1 2.0 Excluded(?) postinflation Misalignment PQ Ω 1.5 (realignment+cosmic cdm h 2 > 0.11 strings+dws) 1.0 Cold DM ADMX String decay preinflation PQ 0.5 0.0 WD cooling hint (only realignment) ADMX II Classical axion window Burst Duration g ae Hot DM CMB BBN Telescope EBL SK Globular Clusters g aγ White Dwarfs g ae g ae Excluded by experiments and Solar Neutrino flux g aγ SN1987A stellar evolution IAXO Helioscopes Beam Dump 0.5 10 7 10 6 10 5 10 4 10 3 10 2 10 1 1 10 10 2 10 3 10 4 10 5 10 6 10 7 m a ev

Bounds and prospects in more detail Ν GHz 10 1 1 10 10 2 coupling to two photons g aγ = c γ α 2πf a m a = m a (f a ) 10 2 BFRT IAXO - Lab. Bounds - Exp. Prospects - Axion models - Ω acdm h 2 =0.12 c γ CΓ 10 ADMX ADMXII ADMXHF KSVZ ρ CDM =0.3GeV/cm 3 1 ADMX DFSZ HS HKS postinflation PQ 10 1 Antropic Θ 0 1 Θ 0 1 DS preinflation PQ 10 7 10 6 10 5 10 4 10 3 m a ev

General Axion-like particles (ALPs) - Mass and coupling unrelated g = α O(1) 2πf a 9 CAST Sumico EBL x ion HB Τ - Scenario 1 f a <H I (realignment+cosmic strings, DWs..) Log 10 g GeV 1 12 Optical EBL 15 X Rays 5 2 1 4 Log 10 m Φ ev

General Axion-like particles (ALPs) - Mass and coupling unrelated g = α O(1) 2πf a 9 CAST Sumico EBL x ion HB Τ - Scenario 2 (anthropic) f a >H I (realignment mechanism) Log 10 g GeV 1 12 Optical EBL - Isocurvature constraints!! 15 X Rays 5 2 1 4 Log 10 m Φ ev

Experiments to detect axion DM - Dish antenna DM a photon to detect! B-field - Cavity experiments DM a amplify and detect B-field - Light propagation E B x - Oscillating EDM

DM around us ρ CDM 0.3 GeV cm 3 velocities in the galaxy phase space density = m an a v 300 km/s 10 3 c n a 4πp 3 3 10 29 µev m a 4 occupation number is HUGE! behaves like a classical NR field! Fourier-transform a(x) ω m a (1 + v 2 /2+...) δω = m av 2 2 δω ω 10 6 ω m a

Axion - photon mixing in a magnetic field Raffelt, PRD 88 - In a magnetic field one photon polarization Q-mixes with the axion L I = g aγ 4 F µν F µν a = g aγ B E a Not axions, nor photons are propagation eigenstates! Axion-photon oscillations in a magnetic field, basis for - light shining through walls (LSW): ALPS @ DESY, GammeV,... - Helioscopes as CAST and SUMICO - Astrophysical anomalies? TeV transparency... and... - Haloscope DM detection

Axion - photon mixing in a magnetic field Raffelt, PRD 88 - Equations of motion for a plane wave A a exp( i(ωt kz)). (ω 2 k 2 1 0 ) 0 1 + 0 g aγ B ω g aγ B ω m 2 a A a = 0 0. axion mixes with A-component PARALLEL to the external B-field - Dark matter solution v = k ω ; ω m a(1 + v 2 /2+...) A a DM χa 1 exp( i(ωt kz)).

DM axions in a magnetic field ω, k, a 0 E a = ωχa 0 ω m a k B ext B a = k E a ω kχa 0

DM axions in a magnetic field E a = ωχa 0 ω, k = 0,a 0 B a =0 B ext

DM axions in a magnetic field ω, k, a 0 E a = ωχa 0 B ext B a = k E a ω kχa 0

DM axions in a magnetic field ω, k, a 0 E a = ωχa 0 B a =0 B ext

DM axions entering a magnetic field ω, k, a 0 B ext =0 B ext =0 sharp boundary

DM axions entering a magnetic field E a = ωχa 0 ω, k, a 0 B ext =0 B ext =0 sharp boundary

DM axions entering a magnetic field E a = ωχa 0 ω, k, a 0 transmitted photon wave ω, ωn, E a 2 reflected photon wave E a ω, ωn, 2 B ext =0 B ext =0 sharp boundary

DM axions changing medium Jaeckel and JR arxiv:1308.1103 B ext = B 2 B ext = B 1 index of refraction n 2 index of refraction n 1 χ 1 = gb 1 1 χ 2 = gb 2 1 m m a n 2 a n 2 2 1 E a = ωχ 1 a 0 ω, k, a 0 sharp boundary dω 1

DM axions changing medium Jaeckel and JR arxiv:1308.1103 B ext = B 2 B ext = B 1 index of refraction n 2 index of refraction n 1 χ 1 = gb 1 1 χ 2 = gb 2 1 m m a n 2 a n 2 2 1 E a = ωχ 2 a 0 E a = ωχ 1 a 0 ω, k, a 0 sharp boundary dω 1

DM axions changing medium Jaeckel and JR arxiv:1308.1103 B ext = B 2 B ext = B 1 index of refraction n 2 index of refraction n 1 χ 1 = gb 1 1 χ 2 = gb 2 1 m m a n 2 a n 2 2 1 E a = ωχ 2 a 0 E a = ωχ 1 a 0 ω, k, a 0 transmitted photon wave reflected photon wave ω, ωn 2, (χ 1 χ 2 ) n 1 n 2 ωa 0 ω, ωn 1, (χ 2 χ 1 ) ωa 0 n 1 + n 2 n 1 + n 2 sharp boundary dω 1

Radiation from a magnetised mirror Horns at al JCAP04(2013)016 E a = ω a χ cos(ω a (t + vz)). magnetic field Radiated photon wave

Radiation from a magnetised mirror Horns at al JCAP04(2013)016 E a = ω a χ cos(ω a (t + vz)). magnetic field E γ + E a z=zmirror =0 Radiated photon wave

Radiation from a magnetised mirror Horns at al JCAP04(2013)016 E a = ω a χ cos(ω a (t + vz)). magnetic field E γ + E a z=zmirror =0 Radiated photon wave E γ = ω a χ cos(ω γ (t z)).

Radiation from a magnetised mirror Horns at al JCAP04(2013)016 E a = ω a χ cos(ω a (t + vz)). magnetic field E γ + E a z=zmirror =0 Radiated photon wave E γ = ω a χ cos(ω γ (t z)). whose frequency is ω γ = ω a = m a (1 + v 2 /2)

3D situation ω, k, a 0 k 1 k E a = ωχa 0 k 2

3D situation ω, k, a 0 k 1 k k 2 E γ E a

3D situation ω, k, a 0 k 1 k k 2 k µ γ =(ω, k 1,k 2, ω 2 k 2 ω) E γ E a

3D situation ω, k, a 0 k 1 k k 2 E γ E a k µ γ =(ω, k 1,k 2, k µ γ (ω, 0, 0,ω) ω 2 k 2 ω)

3D situation ω, k, a 0 - emitted wave perpendicular to the surface k 1 - up to O(k/w) corrections ~ 0.001 - polarized ~ along the magnetic field k k 2 E γ E a k µ γ =(ω, k 1,k 2, k µ γ (ω, 0, 0,ω) ω 2 k 2 ω)

Simplest experiment Horns at al JCAP04(2013)016 light rays are focused in the dish center... up to an angle of order O(k /ω) spherical reflecting dish

Small electric field: how small? - Recall that for QCD axions m a = 6 mev(10 9 GeV/f a ) χ a g aγb m a 10 15 B 10 Tesla c γ 2 The small component does not depend on axion mass! - We know the typical axion amplitude -> typical electric field ρ CDM = 1 2 m2 aa 2 0 =0.3 GeV cm 3 E 2 m a χ a a 0 2 2χ 2 aρ CDM =2χ 2 a (2300 V/m) 2 E 10 12 V m B 5Tesla c γ

Signal size Horns et al, JCAP04(2013)016 spherical dish? detector center sph. P center E a 2 A dish χ 2 ρ CDM A dish 10 26 B 5T c γ 2 2 A 1m 2 Watt

Signal size Horns et al, JCAP04(2013)016 spherical dish? detector center sph. P center E a 2 A dish χ 2 ρ CDM A dish 10 26 B 5T c γ 2 2 A 1m 2 Watt broadband! :-) δω ω O(1) measure 1/octave of a decade with the same detector at the same time

Signal to noise S N = P signal P noise P signal T S measurement dominated by background S N =8 10 2 5K T S Area 10 m 2 B time Bandwidth 5T c γ 2 2 time 1 year (P noise T S ω) (T Sq.lim. = ω) 10 6 ω/ω 10 µev m a but we can do better... up to the quantum limits (one can even do better...) S N = 14T Sq.lim T S Area 10 m 2 B 10 T c γ 2 2 time 1 year 10 6 ω/ω 10 µev m a 3/2

Cavity searches II: ADMX and relatives Ν GHz 10 1 1 10 10 2 10 2 BFRT DISH IAXO - Lab. Bounds - Exp. Prospects - Axion models - Ω acdm h 2 =0.12 c aγγ ρcdm 0.3GeV/cm 3 CΓ 10 ADMX ADMXII ADMXHF KSVZ 1 ADMX DFSZ HS HKS postinflation PQ 10 1 Antropic Θ 0 1 Θ 0 1 DS preinflation PQ 10 7 10 6 10 5 10 4 10 3 m a ev

Limitations: Diffraction r R λ R r Better for small lambda

Limitations: momentum distribution k R λ R r

Limitations: momentum distribution k R R k ω R k ω 10 3 R

Limitations: momentum distribution and Earth s motion with respect to DM k R center of the distribution biased an amount Rv,Earth DM --------- > Daily modulation

Detecting the velocity distribution of DM! k At fist order rays from different parts of the surface end up in the same spot in a CCD d R k m a Rv Measuring Intensity I(d x,d x ) we measure velocity distribution of DM!!! Disclaimer: - 1 - Integrated over - 2 - aberrations of order so make r/r small v d = O(rv )

Conclusions - Axion DM - well motivated - underrepresented (getting better) - testable - key targets not covered - New experiment: dish antenna - a little short for axions - ideal for Hidden Photons and ALPs - directional detection - New understanding of the old experiments - More experiments needed!, some on the go! - ADMX-II, HF

First moves in the visible - Tokyo U. (moving to the MW)

First moves in the visible - DESY (Dark matter: a light move aftermath)