georg raffelt, mpi physics, munich physics colloquium, univ. sydney, 3 march 2014 dark matter axion...

Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014

Dark Matter

Axion Dark MatterAxion Dark Matter

Georg G. Raffelt, Max-Planck-Institut für Physik, MünchenGeorg G. Raffelt, Max-Planck-Institut für Physik, München

Physics Colloquium, University of Sydney, 3 March 2014Physics Colloquium, University of Sydney, 3 March 2014


Axions as Cold Dark Matter of the Universe

Dark Energy ~70% (Cosmological Constant)

Neutrinos 0.1-2%

Dark Matter~25%

Ordinary Matter ~5%(of this only about 10% luminous)


Neutron

ProtonGravitation (Gravitons?)

Weak Interaction (W and Z Bosons)

Periodic System of Elementary Particles

Electromagnetic Interaction (Photon)

Strong Interaction (8 Gluons)

Down

Strange

Bottom

Electron

Muon

Tau

e-Neutrino

m-Neutrino

t-Neutrino nt

nm

nee

m

t

d

s

b

1st Family

2nd Family

3rd Family

Up

Charm

Top

u

c

t

Quarks Leptons

Charge -1/3

Down

Charge -1

Electron

Charge 0

e-Neutrino need

Charge +2/3

Up u

Higgs


Supersymmetric Extension of Particle Physics In supersymmetric extensions of the particle-physics standard model,

every boson has a fermionic partner and vice versa

Sleptons (, , …)Squarks (, , …)

SpinSuperpartner

0

1/2GluinosWinoZinoPhotino ()

1/2

3/2

Higgsino

Gravitino

1/2 Leptons (e, ne, …)Quarks (u, d, …)

1 Gluons

W

Z0

Photon (g)0

2

Higgs

Graviton

Spin Standard particle

• If R-Parity is conserved, the lightest SUSY-particle (LSP) is stable• Most plausible candidate for dark matter is the neutralino, similar to a massive Majorana neutrino

Neutralino = C1 Photino + C2 Zino + C3 Higgsino


Laboratory Searches for WIMP Dark Matter

Energydeposition

Recoil energy(few keV) is measured by• Ionisation• Scintillation• Cryogenic

Galacticdark matterparticle(e.g. neutralino)


WIMP Searches (Underground Physics)

COUPPPICASSO

XENONLUX, ZEPLIN

WARP, ArDM

DEAP/CLEANDAMA/LIBRAKIMS, XMASS

DRIFTGERDA

CDMSEDELWEISS

CRESSTROSEBUD

HeatPhonons

Charge Light


WIMP Cross Section Limits 2014Klaus Eitel, 2014


High- and Low-Energy Frontiers in Particle Physics

1027eV

Planckmass

GUTscale

Electroweakscale

QCDscale

Cosmologicalconstant

10241021101810151012109106103110− 310− 6

WIMP dark matter(related to EW scale, perhaps SUSY)

Axion dark matter (related to Peccei-Quinn symmetry)

𝑓 𝑎𝑚𝜋 𝑓 𝜋 / 𝑓 𝑎 𝑚𝜋 , 𝑓 𝜋

Accelerator Frontier

CERN


Axion Physics in a Nut Shell

CP conservation in QCD byPeccei-Quinn mechanism

For fa f≫ p axions are “invisible”and very light

Axions a ~ p0

mpfp mafa

g

ga

Particle-Physics Motivation

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

• Limits from avoiding excessive energy drain• Solar axion searches (CAST, Sumico)

ag

Solar and Stellar Axions

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

Cold dark matter candidate

ma ~ 10 meV (or much smaller or larger)

Cosmology Search for Axion Dark Matter

S

Nga

Bext

Microwave resonator (1 GHz = 4 meV)

Primakoffconversion

ADMX-LF (UW Seattle) ADMX-HF (Yale)


CP Violation in Particle Physics

Physics Nobel Prize 2008

Discrete symmetries in particle physicsC – Charge conjugation, transforms particles to antiparticles violated by weak interactionsP – Parity, changes left-handedness to right-handedness violated by weak interactionsT – Time reversal, changes direction of motion (forward to backward)CPT – exactly conserved in quantum field theoryCP – conserved by all gauge interactions violated by three-flavor quark mixing matrix

M. Kobayashi T. Maskawa

All measured CP-violating effects derive from a single phase in the quark mass matrix (Kobayashi-Maskawa phase), i.e. from complex Yukawa couplings Cosmic matter-antimatter asymmetry requires new ingredients


The CP Problem of Strong Interactions

ℒQCD=∑𝑞

𝜓𝑞( i𝐷−𝑚𝑞𝑒i 𝜃𝑞 )𝜓𝑞−

14𝐺𝜇𝜈𝑎𝐺𝑎

𝜇𝜈−Θ𝛼 s

8𝜋𝐺𝜇𝜈 𝑎

~𝐺𝑎

𝜇𝜈

𝜓𝑞→𝑒❑−𝑖𝛾 5𝜃𝑞 /2𝜓𝑞

ℒQCD=∑𝑞

𝜓𝑞 (i𝐷−𝑚𝑞)𝜓𝑞−14𝐺𝐺− (Θ− arg det 𝑀𝑞)⏟

−𝜋 ≤Θ≤+𝜋

𝛼s8𝜋

𝐺~𝐺

Real quarkmass

Phase fromYukawa coupling

Anglevariable

CP-oddquantity

Remove phase of mass term by chiral transformation of quark fields

can be traded between quark phases and term No physical impact if at least one Induces a large neutron electric dipole moment (a T-violating quantity)

Experimental limits: Why so small?


Neutron Electric Dipole Moment

Violates time reversal (T) andspace reflection (P) symmetries

Natural scale𝑒

2𝑚𝑁

=1.06×10−14𝑒cm

Experimental limit|𝑑|=0.63×10− 25𝑒 cm

Limit on coefficient

Θ𝑚𝑞

𝑚𝑁

≲10−11


Strong CP Problem

+𝜋−𝜋 Θ

ΛQCD4

QCD vacuum energy

• CP conserving vacuum has (Vafa and Witten 1984)• QCD could have any , is “constant of nature”• Energy can not be minimized: not dynamical

Equivalent Equivalent

−2𝜋 +2𝜋

Peccei-Quinn solution: Make dynamical, let system relax to lowest energy


The Pool Table Analogy (Pierre Sikivie 1996)

GravitySymmetricrelativeto gravity

Pool table

New degree of freedom Axion

𝚯

(Weinberg 1978, Wilczek 1978)

Axis

Symmetrydynamicallyrestored

(Peccei & Quinn 1977)

Symmetrybroken

Floor inclined

fa


35 Years of Axions


The Cleansing Axion

Frank Wilczek

“I named them after a laundry detergent, since they clean up

a problem with an axial current.” (Nobel lecture 2004)


Axion Bounds and Searches

103 106 109 1012 [GeV] fa

eVkeV meV meVma

neV

1015

Directsearches

Too much CDM (misalignment)

TelescopeExperiments

Globular clusters(a-g-coupling)

SN 1987AToo many events

Too muchenergy loss

Too muchhot dark matter

CAST ADMX(Seattle & Yale)

Globular clusters (He ignition), WD cooling(a-e coupling)

Too much cold dark matter(re-alignment with Qi = 1)

Classicregion

Anthropicregion



Neutrinos 0.1-2%

Dark Matter~25%


Axions as Cold Dark Matter of the Universe


Creation of Cosmological Axions

(very early universe)

• UPQ(1) spontaneously broken• Higgs field settles in “Mexican hat”• Axion field sits fixed at

𝑎

𝑉 (𝑎)

𝑎

𝑉 (𝑎)

Θ=0

( eV)

• Axion mass turns on quickly by thermal instanton gas• Field starts oscillating when • Classical field oscillations (axions at rest)

Axions are born as nonrelativistic, classical field oscillationsVery small mass, yet cold dark matter


Axion Cosmology in PLB 120 (1983)


Killing Two Birds With One Stone

Peccei-Quinn mechanism• Solves strong CP problem• Provides dark matter in the form of axions


Cosmic Axion DensityModern values for QCD parameters and temperature-dependent axion massimply (Bae, Huh & Kim, arXiv:0806.0497)

If axions provide the cold dark matter:

• implies GeV and meV (“classic window”)

• GeV (GUT scale) or larger (string inspired) requires (“anthropic window”)

Ω𝑎h2=0.195Θi

2( 𝑓 𝑎1012 GeV )

1.184

=0.105Θi2( 10𝜇eV

𝑚𝑎)

1.184

Θi=0.75( 1012 GeV𝑓 𝑎 )

0.592

=1.0 ( 𝑚𝑎

10𝜇eV )0.592


Axion Production by Domain Wall and String DecayRecent numerical studies of collapseof string-domain wall system

Implies a CDM axion mass of

Hiramatsu, Kawasaki, Saikawa &Sekiguchi, arXiv:1202.5851 (2012)

Remains to be confirmed,interpretation of numerical studiesnot entirely straightforward


BEC Formation

• Axions ~ WIMP dark matter on scales axion Compton wavelength?• Larger-range correlation established by BEC dynamics? (Observable?)• Axions born as classical field oscillations → Issue of classical field dynamics (not a quantum effect)• BEC formation caused by gravitational interactions possible ???See also • Erken, Sikivie, Tam & Yang, arXiv:1111.1157 • Saikawa & Yamaguchi, arXiv:1210.7080 • Noumi, Saikawa, Sato & Yamaguchi, arXiv:1310.0167 • Davidson & Elmer, arXiv:1307.8024 • Berges & Jaeckel, arXiv:1402.4776

~100 citati

ons


High- and Low-Energy Frontiers in Particle Physics

1027eV

Planckmass

GUTscale

Electroweakscale

QCDscale

Cosmologicalconstant

10241021101810151012109106103110− 310− 6

WIMP dark matter(related to EW scale, perhaps SUSY)

Axion dark matter (related to Peccei-Quinn symmetry)

𝑓 𝑎𝑚𝜋 𝑓 𝜋 / 𝑓 𝑎 𝑚𝜋 , 𝑓 𝜋

Accelerator Frontier

CERN


Searching for Solar Axions

Searching forAxion-Like Particles


Experimental Tests of Invisible Axions

Primakoff effect:

Axion-photon transition in externalstatic E or B field(Originally discussed for by Henri Primakoff 1951)

Pierre Sikivie:

Macroscopic B-field can provide alarge coherent transition rate overa big volume (low-mass axions)• Axion helioscope: Look at the Sun through a dipole magnet• Axion haloscope: Look for dark-matter axions with A microwave resonant cavity


Search for Solar Axions

g a

Sun

Primakoff production

Axion Helioscope(Sikivie 1983)

gMagnet S

Na

Axion-Photon-Oscillation

Tokyo Axion Helioscope (“Sumico”) (Results since 1998, up again 2008) CERN Axion Solar Telescope (CAST) (Data since 2003)

Axion flux

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


Tokyo Axion Helioscope (“Sumico”)

Moriyama, Minowa, Namba, Inoue, Takasu & YamamotoPLB 434 (1998) 147Inoue, Akimoto, Ohta, Mizumoto, Yamamoto & MinowaPLB 668 (2008) 93

m


CAST at CERN


Recent “shining-light-through-a-wall” or vacuum birefringence experiments:• ALPS • BMV • BFRT• GammeV • LIPPS • OSQAR • PVLAS

Photon Regeneration ExperimentsEhret et al. (ALPS Collaboration), arXiv:1004.1313

(DESY, using HERA dipole magnet) (Laboratoire National des Champs Magnétiques Intens, Toulouse) (Brookhaven, 1993) (Fermilab) (Jefferson Lab) (CERN, using LHC dipole magnets) (INFN Trieste)


Shining TeV Gamma Rays through the Universe

Figure from a talk by Manuel Meyer (Univ. Hamburg)


Parameter Space for Axion-Like Particles

𝜋η

𝑎WW

Invisibleaxion (DM)

Axion Line 𝝉𝒂→

𝟐𝜸 =𝝉U

𝜋η

𝑎WW

Invisibleaxion (DM)


𝟐𝜸 =𝝉U

HBStars 𝜋η

𝑎WW

Invisibleaxion (DM)


𝟐𝜸 =𝝉U

HBStars

CASTSolar Axions 𝜋η

𝑎WW

Invisibleaxion (DM)


𝟐𝜸 =𝝉U

HBStars

LaserExperiments

CASTSolar Axions

TeV g rays

How

to m

ake

prog

ress

?


Next Generation Axion Helioscope (IAXO) at CERN

• Irastorza et al.: Towards a new generation axion helioscope, arXiv:1103.5334• Armengaud et al.: Conceptual Design of the International Axion Observatory (IAXO), arXiv:1401.3233

Need new magnet w/– Much bigger aperture: per bore– Lighter (no iron yoke)– Bores at Troom


Searching for Axion Dark Matter

Searching forAxion Dark Matter


Search for Galactic Axions (Cold Dark Matter)

Power

Frequency ma

Axion Signal

Thermal noise of cavity & detector

Power of galactic axion signal

Microwave Energies (1 GHz 4 meV)

Dark matter axions Velocities in galaxy Energies therefore

ma = 1-100 meV

va 10-3 c

Ea (1 10-6) maAxion Haloscope (Sikivie 1983)

Bext 8 Tesla

Microwave ResonatorQ 105

Primakoff Conversionga

Bext

Cavityovercomesmomentummismatch

4×10−21 W 𝑉

0.22 m3 ( 𝐵8.5 T )

2 𝑄105×( 𝑚a

2𝜋 GHz )( 𝜌𝑎

5×10−25 g / cm 3 )


Axion Dark Matter Experiment (ADMX), Seattle

Adapted from Gianpaolo Carosi


SQUID Microwave Amplifiers in ADMX

Adapted from Gianpaolo Carosi


Axion Dark Matter Searches

1. Rochester-Brookhaven- Fermilab, PRD 40 (1989) 3153

2. University of Florida PRD 42 (1990) 1297

3. US Axion Search ApJL 571 (2002) L27

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

123

4

Limits assuming axions are the galactic dark matter with standard halo

KSVZ

DFSZ

ADMX-LF (Seattle) search range (2015+)


ADMX-HF at Yale (Steve Lamoreaux Group)

Design of cavity & magnet

Dilution refrigerator above & below deck

ADMX-HF will also be a test-bed for innovative concepts,e.g. thin-film superconducting cavities

Adapted from Karl van Bibber


WISPDMX at DESY and MPIfR

208 MHz microwave cavities H1 detector

Microwave cavities: HERA – 50, 208, 500 MHz208 MHz cavity: resonant modes at 199, 295, 433, 524, 579, 707, 765, 832 MHzMagnets: DESY H1 1.1 T (solenoid), HERA 5 T (dipole), Receiver technology: MPIfR, Tn ~ 100 KPhase 1,2 – searches using available facilitiesPhase 3 – advanced searches with specially designed facilities


Broadband Approaches„Focusing“ the DM signal w/ spherical reflector

Feasible above 10 GHz

TOKAMAKs:- Optimize B2V factor in a radiometer mode- Good at low frequencies- Design study under way (Lobanov et al. 2013)

TOKAMAKFacility

B[T]

V[m3]

B2V[T2 m3]

ToreSupra 4 30 480

JET 4 200 3200

ITER 5 1200 30000

MPP ASDEX 3.1 14 135

TEXTOR 3.0 7 63

Microwave cavity experiment

B[T]

V[m3]

B2V[T2 m3]

ADMX 7.6 0.2 11.5

WISPDMX 1.1 0.46 0.6

Horns et al. 2013


Center for Axion and Precision Physics (CAPP)

New Institute for Basic Science (IBS), Korea

The plan is to launch a competitive Axion Dark Matter Experiment in Korea, participate in state-of-the-art axion experiments around the world, play a leading role in the proposed proton electric-dipole-moment (EDM) experiment and take a significant role in storage-ring precision physics involving EDM and muon g–2 experiments.

15 Oct 2013

YannisSemertzidis


What if the axion is found?


1D Infall and the Folding of Phase Space


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

P.Sikivie& collaborators


Axion Bounds and Searches

103 106 109 1012 [GeV] fa

eVkeV meV meVma

neV

1015

Directsearches

Too much CDM (misalignment)

TelescopeExperiments

Globular clusters(a-g-coupling)

SN 1987AToo many events

Too muchenergy loss

Too muchhot dark matter

CAST ADMX(Seattle & Yale)

Globular clusters (He ignition), WD cooling(a-e coupling)

Too much cold dark matter(re-alignment with Qi = 1)

Classicregion

Anthropicregion


Oscillating Neutron EDM by Axion Dark Matter

Assume axions are galactic dark matter: 300 MeV/cm3

Independently of expect Expect time-varying neutron EDM, MHz frequency for GeV

8 orders of magnitude below limit on static EDM, but oscillates!

+𝜋−𝜋

ΛQCD4

Θ=a / f a Oscillating axion field (DM)→ Oscillating Q term→ Oscillating neutron EDM


Searching for Axions in the Anthropic Window

Graham & Rajendran, arXiv:1101.2691Budker, Graham, Ledbetter, Rajendran & Sushkov, arXiv:1306.6089

CASPEr experimentPrecise magnetometry to measuretiny deviations from Larmor frequency


Cosmic Axion Spin Precession Experiment (CASPEr)

Budker, Graham, Ledbetter, Rajendran & Sushkov, arXiv:1306.6089

Time-varying nucleon EDM caused by axion DM in Lead Titanate magnetometer

Phase I

Phase II

Magnetometer noise limit


Helmholtz Institute Mainz (HIM)

Building under construction

New institute onStructure, symmetry and stability of matter and antimatter

Dmitry BudkerMoving from Berkeley to HIM

Plans to pursue CASPEr


Dow Jones Index of Axion Physics

19771979

19811983

19851987

19891991

19931995

19971999

20012003

20052007

20092011

20130

50

100

150

200

250inSPIRE: Citation of Peccei-Quinn papers or title axion (and similar)


Pie Chart of Dark Universe


Neutrinos 0.1-2%

Dark Matter~25%


georg raffelt, mpi physics, munich physics colloquium, univ. sydney, 3 march 2014 dark matter axion...

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