georg raffelt, max-planck-institut für physik, münchen, germany pont davignon, 21-25 april 2008,...

Georg Raffelt, Max-Planck-Institut für Physik, München, Germany PONT d‘Avignon, 21-25 April 2008, Avignon, France

AxionsAxionsGeorg G. Raffelt, Max-Planck-Institut fGeorg G. Raffelt, Max-Planck-Institut für Physik, Münchenür Physik, München

Motivation, Limits and SearchesMotivation, Limits and SearchesAxionsAxions

PONT d’Avignon, 21-25 April 2008, Avignon, FrancePONT d’Avignon, 21-25 April 2008, Avignon, France


Axion Physics in a Nut ShellAxion Physics in a Nut Shell

CosmologyCosmology

CosmiCosmicc

StringString

In spite of small mass, axionsIn spite of small mass, axions are born are born non-relativisticallynon-relativistically (“non-thermal relics”)(“non-thermal relics”)

““Cold dark matter”Cold dark matter” candidate candidate

mmaa ~ 1 ~ 1--1000 1000 eVeV

Search for Axion Dark MatterSearch for Axion Dark Matter

SS

NN

aa

BBextext

Microwave resonatorMicrowave resonator (1 GHz (1 GHz == 4 4 eV)eV)

PrimakoffPrimakoff conversionconversion

Particle-Physics MotivationParticle-Physics Motivation

CP conservation in QCD byCP conservation in QCD by Peccei-Quinn mechanismPeccei-Quinn mechanism

For fFor faa ≫≫ f f axions are “invisible” axions are “invisible”

and very lightand very light

AxionsAxions a a ~ ~ 00

mmff m maaffaa

aa

Solar and Stellar AxionsSolar and Stellar Axions

Axions thermally produced in stars,Axions thermally produced in stars, e.g. by Primakoff productione.g. by Primakoff production

• Limits from avoiding excessiveLimits from avoiding excessive energy drainenergy drain• SearchSearch forfor solarsolar axionsaxions (CAST, Sumico)(CAST, Sumico)

aa


StandardStandard QCD LagrangianQCD Lagrangian containscontains a CP violating terma CP violating term

GG~Tr)Mdetarg(

8L

20

qs

CP

GG~Tr)Mdetarg(

8L

20

qs

CP

The CP Problem of Strong InteractionsThe CP Problem of Strong Interactions

Induces a neutronInduces a neutron electric dipole momentelectric dipole moment (EDM) much in excess(EDM) much in excess of experimental limitsof experimental limits

cme10310

cme10d 26n2

16n

cme10310

cme10d 26n2

16n

Characterizes degenerateCharacterizes degenerateQCD ground state (QCD ground state ( vacuum) vacuum)

Phase of Quark Phase of Quark Mass MatrixMass Matrix

1010 1010 Why so smallWhy so small ??≲≲


Dynamical SolutionDynamical Solution

Peccei & Quinn 1977 - Wilczek 1978 - Weinberg 1978Peccei & Quinn 1977 - Wilczek 1978 - Weinberg 1978

Re-interpret asRe-interpret as a dynamical variable a dynamical variable (scalar field)(scalar field)

af)x(a

af

)x(a

Peccei-Quinn scale,Peccei-Quinn scale,Axion decay constantAxion decay constant

Pseudo-scalar axion fieldPseudo-scalar axion field

aff

couplings&

massPion~

couplings&

massAxion

aff

couplings&

massPion~

couplings&

massAxion

MeV93f MeV93f Pion decay constantPion decay constant

)G~G(Tr8

L sCP

)G~G(Tr8

L sCP

)G~G(Trf

)x(a8

La

sCP

)G~G(Tr

f)x(a

8L

a

sCP

Axions generically coupleAxions generically couple to gluons and mix with to gluons and mix with 00

gluongluon

aagluongluon

aa

V(a)V(a)

0 0

Potential (mass term)Potential (mass term)induced by Linduced by LCP CP drivesdrives

a(x) to CP-conservinga(x) to CP-conservingminimumminimum

CP-symmetry CP-symmetry dynamically restoreddynamically restored


Peccei-Quinn Mechanism Proposed in 1977Peccei-Quinn Mechanism Proposed in 1977


GravityGravitySymmetricSymmetricrelativerelativeto gravityto gravity

Pool Pool tabletable

New degree New degree of freedomof freedom AxionAxion

__

(Weinberg 1978, Wilczek 1978)(Weinberg 1978, Wilczek 1978)

AxisAxis

SymmetrySymmetrydynamicallydynamicallyrestoredrestored

(Peccei & Quinn 1977)(Peccei & Quinn 1977)

The Pool Table AnalogyThe Pool Table Analogy

P.Sikivie, Physics Today, Dec. 1996, pg. 22P.Sikivie, Physics Today, Dec. 1996, pg. 22

SymmetrySymmetrybrokenbroken

FloorFloor inclinedinclined

ffaa


30 Years of Axions30 Years of Axions


The Cleansing AxionThe Cleansing Axion

““I named them after a laundryI named them after a laundry detergent, since they clean updetergent, since they clean up a problem with an axial current.”a problem with an axial current.”(Nobel lecture 2004, written version)(Nobel lecture 2004, written version)

Frank WilczekFrank Wilczek


Windows of OpportunityWindows of Opportunity

AxionsAxions AlternativesAlternatives

• Cosmic cold dark matter candidateCosmic cold dark matter candidate• Direct detection possibleDirect detection possible

• Supersymmetric particlesSupersymmetric particles• Superheavy particlesSuperheavy particles• Sterile Neutrinos Sterile Neutrinos • Many others … Many others … (but usually not experimentally(but usually not experimentally accessible)accessible)

Search for new physics at E Search for new physics at E ≫≫ TeV TeV in low-energy experimentsin low-energy experiments (Axions Nambu-Goldstone boson of(Axions Nambu-Goldstone boson of spontaneously broken symmetry)spontaneously broken symmetry)

• Neutrino masses (see-saw)Neutrino masses (see-saw)• Proton decayProton decay• Neutron electric dipole momentNeutron electric dipole moment• Deviation from Newton’s LawDeviation from Newton’s Law (e.g. large extra dimensions)(e.g. large extra dimensions)

Solve strong CP problemSolve strong CP problem by Peccei-Quinnby Peccei-Quinn dynamical symmetry restorationdynamical symmetry restoration

• Massless up-quarkMassless up-quark• Spontaneous CP violationSpontaneous CP violation• set at some high energy scaleset at some high energy scale (no radiative corrections)(no radiative corrections)

0 0


Axions as a Research TopicAxions as a Research Topic

0

20

40

60

80

100

120

140

160

1977 1980 1983 1986 1989 1992 1995 1998 2001 2004 2007

Papers in SPIRES that cite one of the two original Peccei and Quinn papers orPapers in SPIRES that cite one of the two original Peccei and Quinn papers or Weinberg’s or Wilczek’s paper or with “axion” or “axino” in their titleWeinberg’s or Wilczek’s paper or with “axion” or “axino” in their title (total of 3186 papers up to 2007) (total of 3186 papers up to 2007)


Axions as Pseudo Nambu-Goldstone BosonsAxions as Pseudo Nambu-Goldstone Bosons

• The realization of the Peccei-Quinn mechanism involves a new chiral The realization of the Peccei-Quinn mechanism involves a new chiral

U(1) symmetry, spontaneously broken at a scale fU(1) symmetry, spontaneously broken at a scale faa

• Axions are the corresponding Nambu-Goldstone modeAxions are the corresponding Nambu-Goldstone mode

E E f faa

• UUPQPQ(1) spontaneously (1) spontaneously

broken broken • Higgs field settles in Higgs field settles in “ “Mexican hat”Mexican hat”

aa

V(a)V(a)

E E QCD QCD ≪≪ f faa

• UUPQPQ(1) explicitly broken (1) explicitly broken

by instanton effects by instanton effects • Mexican hat tiltsMexican hat tilts• Axions acquire a massAxions acquire a mass

aa

V(a)V(a)

=0=0__


From Standard to Invisible AxionsFrom Standard to Invisible Axions

Standard ModelStandard Model Standard AxionStandard AxionWeinberg 1978, Wilczek 1978Weinberg 1978, Wilczek 1978

Invisible AxionInvisible Axion

Kim 1979, Shifman,Kim 1979, Shifman,Vainshtein, Zakharov 1980,Vainshtein, Zakharov 1980,Dine,Dine, Fischler,Fischler, SrednickiSrednicki 19811981Zhitnitsky 1980Zhitnitsky 1980

All Higgs degrees ofAll Higgs degrees offreedom are used upfreedom are used up

• Peccei-Quinn scale fPeccei-Quinn scale faa = =

electroweak scale felectroweak scale few ew

• Two Higgs fields,Two Higgs fields, separately giving massseparately giving mass to up-type quarks andto up-type quarks and down-type quarksdown-type quarks

• Additional Higgs withAdditional Higgs with

ffaa ≫≫ f fewew

• Axions very light andAxions very light and and very weaklyand very weakly interactinginteracting

No room for axionsNo room for axions Axions quickly ruled outAxions quickly ruled outexperimentally andexperimentally andastrophysicallyastrophysically

• New scale requiredNew scale required• Axions can beAxions can be cold dark mattercold dark matter• Can be detectedCan be detected


Axion PropertiesAxion Properties

MassMassa7

aa f

fm

GeV10/f

eV6.0m

a7a

a ffm

GeV10/f

eV6.0m

Nucleon couplingNucleon coupling(axial vector)(axial vector)

af2

CL NN

a

NaN 5

af2

CL NN

a

NaN 5

NN

NNaa

Electron couplingElectron coupling(optional)(optional)

af2

CL ee

a

eae 5

af2

CL ee

a

eae 5

ee

eeaa

Gluon couplingGluon coupling(Generic property)(Generic property)

aG~Gf8

La

saG

aG~G

f8L

a

saG

aa

GG

GG

Photon couplingPhoton couplingaBEgaF~F

4

gL a

aa

aBEgaF~F

4

gL a

aa

92.1NE

f2g

aa

92.1NE

f2g

aa

aa

Pion couplingPion coupling a...)(ff

CL 0

a

aa

a...)(

ffC

L 0

a

aa

aa


Supernova 1987A Energy-Loss ArgumentSupernova 1987A Energy-Loss Argument

NeutrinoNeutrinospheresphere

NeutrinoNeutrino diffusiondiffusion

Late-time signal most sensitive observableLate-time signal most sensitive observable

Emission of very weakly interactingEmission of very weakly interactingparticles would “steal” energy from theparticles would “steal” energy from theneutrino burst and shorten it.neutrino burst and shorten it.(Early neutrino burst powered by accretion,(Early neutrino burst powered by accretion, not sensitive to volume energy loss.)not sensitive to volume energy loss.)

Volume emissionVolume emission of novel particlesof novel particles

SN 1987A neutrino signalSN 1987A neutrino signal


Axions as Pseudo Nambu-Goldstone BosonsAxions as Pseudo Nambu-Goldstone Bosons

• The realization of the Peccei-Quinn mechanism involves a new chiral The realization of the Peccei-Quinn mechanism involves a new chiral

U(1) symmetry, spontaneously broken at a scale fU(1) symmetry, spontaneously broken at a scale faa

• Axions are the corresponding Nambu-Goldstone modeAxions are the corresponding Nambu-Goldstone mode

E E f faa

• UUPQPQ(1) spontaneously (1) spontaneously

broken broken • Higgs field settles in Higgs field settles in “ “Mexican hat”Mexican hat”

aa

V(a)V(a)

E E QCD QCD ≪≪ f faa

• UUPQPQ(1) explicitly broken (1) explicitly broken

by instanton effects by instanton effects • Mexican hat tiltsMexican hat tilts• Axions acquire a massAxions acquire a mass

aa

V(a)V(a)

=0=0__


Series of Papers on Axion Cosmology in PLB Series of Papers on Axion Cosmology in PLB 120 (1983)120 (1983)

Page 127



Page 133



Page 137


Killing Two Birds with One StoneKilling Two Birds with One Stone

Peccei-Quinn mechanismPeccei-Quinn mechanism• Solves strong CP problemSolves strong CP problem• May provide dark matterMay provide dark matter in the form of axionsin the form of axions


Production of Cold Axion Population in the Production of Cold Axion Population in the Early UniverseEarly Universe

Approximate axionApproximate axion cold dark matter densitycold dark matter density

6/7

a

6/7

12a

a meV1

4GeV10

f5.0

6/7

a

6/7

12a

a meV1

4GeV10

f5.0

Inflation after PQ symmetry breaking Inflation after PQ symmetry breaking

Homogeneous mode oscillates afterHomogeneous mode oscillates after T T ≲ ≲ QCDQCD

Dependence on initial misalignmentDependence on initial misalignmentangleangle ia ia

Reheating restores PQ symmetry Reheating restores PQ symmetry

• Cosmic strings of broken UCosmic strings of broken UPQPQ(1)(1)

form by Kibble mechanismform by Kibble mechanism• Radiate long-wavelength axionsRadiate long-wavelength axions

• aa independent of initial conditions independent of initial conditions

Inhomogeneities of axion field large,Inhomogeneities of axion field large,self-couplings lead to formation of self-couplings lead to formation of mini-clustersmini-clustersTypical propertiesTypical properties• Mass Mass ~ 10~ 101212 M Msunsun

• Radius ~ 10Radius ~ 101010 cm cm• Mass fraction up to several 10%Mass fraction up to several 10%

• Isocurvature fluctuations from largeIsocurvature fluctuations from large quantum fluctuations of masslessquantum fluctuations of massless axion field created during inflationaxion field created during inflation• Strong CMBR bounds on isocurvature Strong CMBR bounds on isocurvature fluctuationsfluctuations• Scale of inflation required to beScale of inflation required to be very small very small II ≲≲ 10 101313 GeV GeV[Beltrán, García-Bellido & Lesgourgues[Beltrán, García-Bellido & Lesgourgues hep-ph/0606107]hep-ph/0606107]


Strings form by Kibble mechanism Strings form by Kibble mechanism after break-down of Uafter break-down of UPQPQ(1)(1)

Small loops form by self-intersectionSmall loops form by self-intersection

Axions from Cosmic StringsAxions from Cosmic Strings

Paul ShellardPaul Shellard


Axion Mini ClustersAxion Mini Clusters

The inhomogeneities of the axion field are large, leading to bound objects,The inhomogeneities of the axion field are large, leading to bound objects,““axion mini clusters”axion mini clusters”. [Hogan & Rees, PLB 205 (1988) 228.] . [Hogan & Rees, PLB 205 (1988) 228.] Self-coupling of axion field crucial for dynamics.Self-coupling of axion field crucial for dynamics.

Typical mini cluster properties:Typical mini cluster properties:

Mass ~ 10Mass ~ 101212 M Msunsun

Radius ~ 10Radius ~ 101010 cm cmMass fraction up to several 10Mass fraction up to several 10%%

Potentially detectable with Potentially detectable with gravitational femtolensinggravitational femtolensing

Distribution of axion energy density. Distribution of axion energy density. 2-dim slice of comoving length 0.25 pc2-dim slice of comoving length 0.25 pc[Kolb & Tkachev, ApJ 460 (1996) L25][Kolb & Tkachev, ApJ 460 (1996) L25]


Inflation, Axions, and the Anthropic PrincipleInflation, Axions, and the Anthropic Principle

Late inflation scenario of axion cosmologyLate inflation scenario of axion cosmology

• Initial misalignment angle constant in our patch of the universeInitial misalignment angle constant in our patch of the universe

• Dark matter density determined by the initial random number Dark matter density determined by the initial random number i i

• Is different in different patches of the universeIs different in different patches of the universe• Dark matter fraction not calculable from first principlesDark matter fraction not calculable from first principles• Random number chosen by process of spontaneous symmetry breakingRandom number chosen by process of spontaneous symmetry breaking

Natural case for applying anthropic reasoning for the observed darkNatural case for applying anthropic reasoning for the observed darkmatter density relative to baryonsmatter density relative to baryons

• Linde, “Inflation and Axion Cosmology,” PLB 201:437, 1988Linde, “Inflation and Axion Cosmology,” PLB 201:437, 1988• Tegmark, Aguirre, Rees & Wilczek,Tegmark, Aguirre, Rees & Wilczek, “ “Dimensionless constants, cosmology and other dark matters,”Dimensionless constants, cosmology and other dark matters,” PRD 73, 023505 (2006) [arXiv:astro-ph/0511774]PRD 73, 023505 (2006) [arXiv:astro-ph/0511774]


Axion Hot Dark Matter from Thermalization Axion Hot Dark Matter from Thermalization after after QCDQCD

Freeze-out temperatureFreeze-out temperature

Cosmic thermal degrees ofCosmic thermal degrees offreedom at axion freeze-outfreedom at axion freeze-out

Cosmic thermal degrees ofCosmic thermal degrees offreedom freedom

a)2

(ff

CL

0

00

a

aa

a)2

(ff

CL

0

00

a

aa

aa

Chang & Choi, PLB 316 (1993) 51Chang & Choi, PLB 316 (1993) 51

094.0)z1(3

z1Ca

094.0)z1(3

z1Ca

104 105 106 107

104 105 106 107

fa (GeV)

fa (GeV)


Lee-Weinberg Curve for Neutrinos and AxionsLee-Weinberg Curve for Neutrinos and Axions

log(log(aa))

log(mlog(maa))

MM

10 eV10 eV 10 10 eVeV

CDCDMM

HDHDMMAxionsAxions

Thermal RelicsThermal RelicsNon-ThermalNon-Thermal

RelicsRelics

log(log())

log(mlog(m))

MM

10 eV10 eV

CDCDMM

HDHDMM

10 GeV10 GeV

NeutrinosNeutrinos& WIMPs& WIMPs

Thermal RelicsThermal Relics


Axion Hot Dark Matter Limits from Precision Axion Hot Dark Matter Limits from Precision DataData

mmaa < 1.0 eV (95% CL) < 1.0 eV (95% CL)

mmaa < 0.4 eV (95% CL) < 0.4 eV (95% CL)

WMAP-5, LSS, BAO, SNIaWMAP-5, LSS, BAO, SNIa

WMAP-3, small-scale CMB,WMAP-3, small-scale CMB,HST, BBN, LSS, HST, BBN, LSS, Ly-Ly-

Hannestad, Mirizzi, RaffeltHannestad, Mirizzi, Raffelt& Wong [arXiv:0803.1585]& Wong [arXiv:0803.1585]

Melchiorri, Mena & SlosarMelchiorri, Mena & Slosar[arXiv:0705.2695] [arXiv:0705.2695]

Marginalizing over unknown neutrino hot dark matter componentMarginalizing over unknown neutrino hot dark matter component

Credible regions for neutrino plus axion hotCredible regions for neutrino plus axion hotdark matter (WMAP-5, LSS, BAO, SNIa)dark matter (WMAP-5, LSS, BAO, SNIa)Hannestad, Mirizzi, Raffelt & WongHannestad, Mirizzi, Raffelt & Wong[arXiv:0803.1585][arXiv:0803.1585]


DirectDirectsearchsearch

Too muchToo muchcold dark mattercold dark matter

TeleTelescopescopeExperimentsExperiments

Globular clustersGlobular clusters(a-(a--coupling)-coupling)

Too manyToo manyeventsevents

Too muchToo muchenergy lossenergy loss

SN 1987A (a-N-coupling)SN 1987A (a-N-coupling)

Axion BoundsAxion Bounds

101033 101066 101099 10101212 [GeV] f[GeV] faa

eVeVkeVkeV meVmeV eVeVmmaa

Too much hot dark matterToo much hot dark matter

CASTCAST ADMXADMX


Experimental Tests of the Invisible AxionExperimental Tests of the Invisible Axion

Primakoff effect:Primakoff effect:

Axions-photon transitions in externalAxions-photon transitions in externalstatic E or B fieldstatic E or B field(Originally discussed for (Originally discussed for 00 by Henri Primakoff 1951)by Henri Primakoff 1951)

Pierre Sikivie:Pierre Sikivie:

Macroscopic B-field can provide aMacroscopic B-field can provide alarge coherent transition rate overlarge coherent transition rate overa big volume (low-mass axions)a big volume (low-mass axions)

• Axion helioscope:Axion helioscope: Look at the Sun through a dipoleLook at the Sun through a dipole magnet magnet

• Axion haloscope:Axion haloscope: Look for dark-matter axions withLook for dark-matter axions with A microwave resonant cavityA microwave resonant cavity


Search for Galactic Axions (Cold Dark Matter)Search for Galactic Axions (Cold Dark Matter)

PowerPower

FrequencyFrequency mmaa

Axion Axion SignalSignal

Thermal noise of Thermal noise of cavity & detectorcavity & detector

Power of galactic axion signalPower of galactic axion signal

325aa

5

2

321

cm/g105GHz2m

10

QT5.8

B

m22.0

VW104

325aa

5

2

321

cm/g105GHz2m

10

QT5.8

B

m22.0

VW104

Microwave Microwave EnergiesEnergies (1 GHz (1 GHz 4 4 eV)eV)

DM axionsDM axions Velocities in galaxyVelocities in galaxy Energies thereforeEnergies therefore

mmaa = 1-1000 = 1-1000 eVeV

vvaa 10 1033 c c

EEaa (1 (1 101066) m) maa

Axion HaloscopeAxion Haloscope (Sikivie(Sikivie 1983)1983)

BBextext 8 Tesla 8 Tesla

Microwave Microwave ResonatorResonatorQ Q 10 1055

Primakoff ConversionPrimakoff Conversionaa

BBextext

CavityCavityovercomesovercomesmomentummomentummismatchmismatch


Axion Dark Matter SearchesAxion Dark Matter Searches

Limits/sensitivities, Limits/sensitivities, assuming axions are the galactic dark matter assuming axions are the galactic dark matter

1. Rochester-Brookhaven-1. Rochester-Brookhaven- FermilabFermilab PRD 40 (1989) 3153PRD 40 (1989) 3153

2. University of Florida2. University of Florida PRD 42 (1990) 1297PRD 42 (1990) 1297

3. US Axion Search 3. US Axion Search (Livermore)(Livermore) ApJL 571 (2002) L27ApJL 571 (2002) L27

4. CARRACK I (Kyoto)4. CARRACK I (Kyoto) preliminarypreliminary hep-ph/0101200hep-ph/0101200

44

112233

5. ADMX (Livermore)5. ADMX (Livermore) foreseenforeseen e.g. Rev. Mod. Phys.e.g. Rev. Mod. Phys. 75 (2003) 777 75 (2003) 777

55


ADMX (G.Carosi, Fermilab, May 2007)ADMX (G.Carosi, Fermilab, May 2007)



Renewed ADMXRenewed ADMXdata taking has begundata taking has begun

on 28 March 2008on 28 March 2008(Same day as CAST He-3 began)(Same day as CAST He-3 began)


Fine Structure in Axion SpectrumFine Structure in Axion Spectrum

• Axion distribution on a 3-dim sheet in 6-dim phase spaceAxion distribution on a 3-dim sheet in 6-dim phase space• Is “folded up” by galaxy formationIs “folded up” by galaxy formation• Velocity distribution shows narrow peaks that can be resolvedVelocity distribution shows narrow peaks that can be resolved• More detectable information than local dark matter densityMore detectable information than local dark matter density

P.SikivieP.Sikivie& collaborators& collaborators


Search for Solar AxionsSearch for Solar Axions

aa

SunSun

Primakoff Primakoff productionproduction

Axion Helioscope (Sikivie 1983)Axion Helioscope (Sikivie 1983)

Magnet Magnet SS

NNaa

Axion-Photon-Axion-Photon-OscillationOscillation

Tokyo Axion Helioscope (“Sumico”)Tokyo Axion Helioscope (“Sumico”) (Results since 1998, up again 2008)(Results since 1998, up again 2008)

CERN Axion Solar Telescope (CAST)CERN Axion Solar Telescope (CAST) (Data since 2003)(Data since 2003)

Axion fluxAxion flux

Alternative technique: Alternative technique: Bragg conversion in crystalBragg conversion in crystal Experimental limits on solar axion fluxExperimental limits on solar axion flux from dark-matter experimentsfrom dark-matter experiments (SOLAX, COSME, DAMA, ...)(SOLAX, COSME, DAMA, ...)


Tokyo Axion Helioscope (“Sumico”)Tokyo Axion Helioscope (“Sumico”)

S.Moriyama, M.Minowa, T.Namba, Y.Inoue, Y.TakasuS.Moriyama, M.Minowa, T.Namba, Y.Inoue, Y.Takasu& A.Yamamoto, PLB 434 (1998) 147& A.Yamamoto, PLB 434 (1998) 147

~ 3 m~ 3 m


Results and Plans of Tokyo Axion Helioscope Results and Plans of Tokyo Axion Helioscope (“Sumico”)(“Sumico”)

S. Inoue at TAUP 07S. Inoue at TAUP 07


Extending to higher mass values with gas Extending to higher mass values with gas fillingfilling

2qL

sinq

BgP 2

2a

a

2qL

sinq

BgP 2

2a

a

E2

mmq

22a

E2

mmq

22a

Axion-photon transition probabilityAxion-photon transition probability

Axion-photon momentum transferAxion-photon momentum transfer

Transition suppressed for qL Transition suppressed for qL ≳≳ 11

Gas filling: Give photons a refractiveGas filling: Give photons a refractivemass to restore full transition strengthmass to restore full transition strength(~ MSW effect)(~ MSW effect)

ee

2 nm4

m

ee

2 nm4

m

(n(nee electron density) electron density)

GasAZ

eV9.28m GasAZ

eV9.28m

HeHe44 vapour pressure at 1.8 K vapour pressure at 1.8 K33 cmg102.0 33 cmg102.0 eV26.0m eV26.0m


LHC Magnet Mounted as a Telescope to Follow LHC Magnet Mounted as a Telescope to Follow the Sunthe Sun


CAST at CERNCAST at CERN


CAST Focussing X-Ray TelescopeCAST Focussing X-Ray Telescope

One spare mirror system from the failed Abrixas x-rayOne spare mirror system from the failed Abrixas x-raysatellitesatellite

• From 43 mm From 43 mm (LHC magnet aperture) to ~3 mm (LHC magnet aperture) to ~3 mm • Signal/background improvement > 100Signal/background improvement > 100• Signal and background simultaneously measuredSignal and background simultaneously measured


Sun Spot on CCD with X-Ray TelescopeSun Spot on CCD with X-Ray Telescope


Limits from CAST-I and CAST-IILimits from CAST-I and CAST-II

CAST-I results: PRL 94:121301 (2005) and JCAP 0704 (2007) 010 CAST-I results: PRL 94:121301 (2005) and JCAP 0704 (2007) 010 CAST-II results (He-4 filling): preliminaryCAST-II results (He-4 filling): preliminary


1010-4-4

1010-6-6

1010-8-8

1010-10-10

1010-12-12

1010-14-14

1010-16-16

1010-6-61010-7-7 1010-5-5 1010-4-4 1010-3-3 1010-2-2 1010-1-1 11 1010 100100

Axion mass mAxion mass maa [eV] [eV]

Axio

n-p

hoto

n-c

ou

plin

g g

Axio

n-p

hoto

n-c

ou

plin

g g

aa [G

eV

[GeV

-1-1]]

FutureFuture

DM DM SearchSearch

+Gas+GasCAST SensitivityCAST Sensitivity HBHBStarsStars

+Gas+GasCAST SensitivityCAST Sensitivity

PVLAS expectedPVLAS expectedPVLAS expectedPVLAS expected

Tokyo HelioscopeTokyo Helioscope

Limits on Axion-Photon-CouplingLimits on Axion-Photon-Coupling

PVLAS expectedPVLAS expected

Tokyo HelioscopeTokyo Helioscope

HelioHelioseisseismologymology

Tele

scop

eTele

scop

e

LaserLaser

KSVZ model

KSVZ model

DFSZ model

DFSZ model

Axion LineAxion Line

PVLASPVLASSignaturSignaturee


AlpsAlpsAxion-like particles (ALPs)Axion-like particles (ALPs)(Pseudo)-scalar particles with a two-photon vertex(Pseudo)-scalar particles with a two-photon vertex


Particles with Two-Photon CouplingParticles with Two-Photon Coupling

Particles with two-photon vertex:Particles with two-photon vertex:• Neutral pions (Neutral pions (00), Gravitons), Gravitons• Axions (a) and similar hypothetical particlesAxions (a) and similar hypothetical particles

aBEgL aa aBEgL aa

Two-photonTwo-photondecaydecay

64

mg 3a

2a

a

64

mg 3a

2a

aPhotonPhotonCoalescenceCoalescence

PrimakoffPrimakoffEffectEffect

Conversion of photons intoConversion of photons into pions, gravitons or axions, pions, gravitons or axions, or the reverseor the reverse

Magnetically Magnetically induced vacuuminduced vacuumbirefringencebirefringence

In addition to QED In addition to QED Cotton-Mouton-effectCotton-Mouton-effect

PVLAS experiment recently PVLAS experiment recently measured anmeasured aneffect ~ 10effect ~ 1044 larger than QED larger than QED expectationexpectation(Signal now disproved)(Signal now disproved)


Dimming of Supernovae without Cosmic Dimming of Supernovae without Cosmic Acceleration?Acceleration?

Axion-photon-oscillations in intergalactic Axion-photon-oscillations in intergalactic B-field domainsB-field domains dim photon flux dim photon flux Effect grows linearly with distanceEffect grows linearly with distance Saturates at equipartition between photons and axions (unlike grey dust)Saturates at equipartition between photons and axions (unlike grey dust)

Mixing matrixMixing matrix 112

a42

a

2a

1e

2aa

a2pl Mpc

m108.7Bg15.0

Bg15.0n8.10

mBg

Bg

21

1

12a

42a

2a

1e

2aa

a2pl Mpc

m108.7Bg15.0

Bg15.0n8.10

mBg

Bg

21

Domain size ~ 1 MpcDomain size ~ 1 MpcField strength ~ 1 nGField strength ~ 1 nGa-a--coupling ~ 10-coupling ~ 101010 GeV GeV11

Axion mass Axion mass << 10 101616 eV eV

Photon energy ~ 1 eVPhoton energy ~ 1 eVElectron density Electron density ~ 10~ 1077 cm cm33

(average baryon density)(average baryon density)

Chromaticity dependsChromaticity dependssensitively on assumedsensitively on assumedvalues and distributionvalues and distribution

of nof nee and B and B

Csáki, Kaloper & Terning (hep-ph/0111311, hep-ph/0112212, astro-ph/0409596). Erlich & GrojeanCsáki, Kaloper & Terning (hep-ph/0111311, hep-ph/0112212, astro-ph/0409596). Erlich & Grojean(hep-ph/0111335). Deffayet, et al. (hep-ph/0112118). Christensson & Fairbairn (astro-ph/0207525).(hep-ph/0111335). Deffayet, et al. (hep-ph/0112118). Christensson & Fairbairn (astro-ph/0207525).Mörtsell et al. (astro-ph/0202153). Mörtsell & Goobar (astro-ph/0303081). Bassett (astro-ph/Mörtsell et al. (astro-ph/0202153). Mörtsell & Goobar (astro-ph/0303081). Bassett (astro-ph/0311495). Ostman & M0311495). Ostman & Möörtsell (astro-ph/0410501). Mirizzi, Raffelt & Serpico (astro-ph/0506078).rtsell (astro-ph/0410501). Mirizzi, Raffelt & Serpico (astro-ph/0506078).


Cantatore 12Cantatore 12


The PVLAS Dichroism SignalThe PVLAS Dichroism Signal

PVLAS, PRL 96:110406 (2006), hep-ex/0507107 PVLAS, PRL 96:110406 (2006), hep-ex/0507107


Latest PVLAS ResultsLatest PVLAS Results

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ResonantResonantcavities oncavities ongeneration &generation &regenerationregenerationsideside

hep-ph/0701198hep-ph/0701198

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BMV Experiment, using a pulsedBMV Experiment, using a pulsedlaser and pulsed magnetic fieldlaser and pulsed magnetic field(Toulouse)(Toulouse)

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Technological Applications of PVLAS ParticlesTechnological Applications of PVLAS Particles

arXiv:0704.0490v1 [hep-ph] arXiv:0704.0490v1 [hep-ph]

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