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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
Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. 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)
Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
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
Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
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
Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
Laboratory Searches for WIMP Dark Matter
Energydeposition
Recoil energy(few keV) is measured by• Ionisation• Scintillation• Cryogenic
Galacticdark matterparticle(e.g. neutralino)
Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
WIMP Searches (Underground Physics)
COUPPPICASSO
XENONLUX, ZEPLIN
WARP, ArDM
DEAP/CLEANDAMA/LIBRAKIMS, XMASS
DRIFTGERDA
CDMSEDELWEISS
CRESSTROSEBUD
HeatPhonons
Charge Light
Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
WIMP Cross Section Limits 2014Klaus Eitel, 2014
Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 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
Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
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)
Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
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
Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
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?
Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
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
Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
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
Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
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
Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
35 Years of Axions
Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
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)
Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
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
Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
Dark Energy ~70% (Cosmological Constant)
Neutrinos 0.1-2%
Dark Matter~25%
Ordinary Matter ~5%(of this only about 10% luminous)
Axions as Cold Dark Matter of the Universe
Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
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
Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
Axion Cosmology in PLB 120 (1983)
Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
Killing Two Birds With One Stone
Peccei-Quinn mechanism• Solves strong CP problem• Provides dark matter in the form of axions
Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
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
Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
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
Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
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
Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 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
Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
Searching for Solar Axions
Searching forAxion-Like Particles
Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
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
Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
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 ...)
Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
Tokyo Axion Helioscope (“Sumico”)
Moriyama, Minowa, Namba, Inoue, Takasu & YamamotoPLB 434 (1998) 147Inoue, Akimoto, Ohta, Mizumoto, Yamamoto & MinowaPLB 668 (2008) 93
m
Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
CAST at CERN
Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
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)
Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
Shining TeV Gamma Rays through the Universe
Figure from a talk by Manuel Meyer (Univ. Hamburg)
Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
Parameter Space for Axion-Like Particles
𝜋η
𝑎WW
Invisibleaxion (DM)
Axion Line 𝝉𝒂→
𝟐𝜸 =𝝉U
𝜋η
𝑎WW
Invisibleaxion (DM)
Axion Line 𝝉𝒂→
𝟐𝜸 =𝝉U
HBStars 𝜋η
𝑎WW
Invisibleaxion (DM)
Axion Line 𝝉𝒂→
𝟐𝜸 =𝝉U
HBStars
CASTSolar Axions 𝜋η
𝑎WW
Invisibleaxion (DM)
Axion Line 𝝉𝒂→
𝟐𝜸 =𝝉U
HBStars
LaserExperiments
CASTSolar Axions
TeV g rays
How
to m
ake
prog
ress
?
Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
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
Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
Searching for Axion Dark Matter
Searching forAxion Dark Matter
Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
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 )
Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
Axion Dark Matter Experiment (ADMX), Seattle
Adapted from Gianpaolo Carosi
Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
SQUID Microwave Amplifiers in ADMX
Adapted from Gianpaolo Carosi
Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
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+)
Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
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
Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
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
Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
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
Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
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
Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
What if the axion is found?
Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
1D Infall and the Folding of Phase Space
Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
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
Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
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
Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
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
Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
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
Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
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
Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
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
Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
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)
Georg Raffelt, MPI Physics, Munich Physics Colloquium, Univ. Sydney, 3 March 2014
Pie Chart of Dark Universe
Dark Energy ~70% (Cosmological Constant)
Neutrinos 0.1-2%
Dark Matter~25%
Ordinary Matter ~5%(of this only about 10% luminous)