lawrence livermore national laboratory august 2, 2004
TRANSCRIPT
Searching for the AxionLeslie J RosenbergLawrence Livermore National LaboratoryAugust 2, 2004
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Outline
What is the axion? Axion properties.The window of allowed axion masses and couplings.Selected current laboratory and astrophysical searches:
RF cavity experiments;Radiotelescope;Solar-axion search;5th force.
Overall status.Conclusions.
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QCD is expected to have large CP violation
1973: QCD…a gauge theory of color.QCD respected the observed C, P and CP conservation.
1975: QCD + instantons ⇒ QCD has CP-violating interactions.
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QCD on the lattice: CP-violating instantonsin a slice of spacetime
Peccei and Quinn:CP conserved through a hidden symmetry
This CP violation should, e.g., give a large neutron electric dipolemoment (T + CPT = CP); none is unobserved.(9 orders-of-magnitude discrepancy.)
This leads to the “Strong CP Problem”: Where did QCD CP violation go?
1977: Peccei and Quinn: Posit a hidden broken U(1) symmetry ⇒1) A new Goldstone boson (the axion);2) Remnant axion VEV nulls QCD CP violation.
Why doesn’t the neutron havean electric dipole moment?
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Properties of the axion
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What is the dark matter?
The Coma cluster of galaxies
“The difference between this result and Hubble’s value for the average mass of a nebula must remain unexplained until further information becomes available.”
Zwicky and Smith 1936
They found a huge discrepancy between the visible mass and the dynamical mass.
The nature of dark matter is one of the most pressing questions in science
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Axions and dark matter
Some properties of dark matter (from the earlier lecture):No interactions with normal matter and radiation (“dark…”);Gravitational interactions (“…matter”);Cold (slow-moving in the early universe);Mostly bosonic (to stuff large quantities into rich clusters).
Dark matter properties are those of a low-mass axion:Low mass axions are an ideal dark matter candidate.
Plus…The axion mass is constrained to 1 or 2 orders-of-magnitude;Select axion couplings are constrained to 1 order-of-magnitude;The axion is doubly-well motivated…it solves 2 problems (Occam’s razor).
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Summary of laboratory searches:A heavy axion is excludedFor example: SLAC E137 (Bjorken et al.)
detector
a→γγ
20 GeV electrons
earth shield
axions produced herevia Primakoff effectlif
etim
e of
a(s
ec)
→γγ
fPQ must be considerably greater thanthe weak scale
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Summary of astrophysical bounds:The axion mass is smallExample:neutrinos from SN1987A
Log
{axi
on lu
min
osity
(erg
/sec
)}
Supernova in the LMC.Neutrinos are trapped and diffuse outover timescales of around 10 seconds.
Kamiokande and IMB together recorded19 neutrinos from SN1987A.
An axion of mass between10-3 and 2 eV would takeso much energy out that...
the length of theexplosion wouldbe observablyforshortened.
Overall summary: Astrophysics (stellar evolution and SN1987A), cosmology, and laboratory experiments leave the invisible CDM axion window 10-6 < ma < 10-3 eV (with large uncertainties)
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Bounded window of allowed axion masses
Very light axions forbidden:else too much dark matter
Heavy axions forbidden:else new pion-like particle
⇐Dark matter range:“axion window”
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Current experiments probing the axion mass window
Two broad classes of experiments:1) Detect relic (big bang left-overs) axions;2) Produce and detect axions; this is in-general harder as there are two
factors of small couplings.
Selected current experiments:RF Cavity Experiments: ADMX, CARRACKAstrophysical: Radiotelescope, CAST*Short-range forces*
*These experiments do not depend on detecting remnant axions
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Principle of RF cavity experiments:Axion and electromagnetic fields exchange energy
The axion-photon coupling
gaγ
is a source in Maxwell’s Equations
∂ E2 /2( )∂t 2 −E ⋅ ∇ ×B( )= gaγ Ý a E ⋅B( )
Imposing a strong external magnetic field B0 allows the axion field to pump energy into the cavity.
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ADMX: Axion Dark Matter Experiment
Core team:
• LLNL: S. Asztalos, C. Hagmann, D. Kinion,L.J Rosenberg, K. van Bibber, D. Yu
• Univ. Florida: L. Duffy, P. Sikivie, N.S. Sullivan, D.B. Tanner
• U.C. Berkeley: J. Clarke
• NRAO: R. Bradley
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ADMX hardware (I)
Magnet arrivesMagnet with insert (side view)
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ADMX hardware (II)
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The axion receiver
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Sample data and candidates
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Brief outline of analysis — 100 MHz of data
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Recent exclusion limits
Particle Physics Astrophysics
These are interesting regimes ofparticle and astrophysics: realistic axioncouplings and halo densities
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The parameter space
presentexperiment
Sensitivity in the heart of the axion parameter spaceSLACSI-02aug04-ljr
Microwave amplifiers
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The world’s quietest radio receiver
Systematics-limited for signals of 10-26 W~10-3 of DFSZ axion power.
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Gigahertz SQUID amplifiers
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An old idea from antenna design(“shunt detuned frequency”)applied to quantum electronics.
The target sensitivity
Definitive sensitivity over lowest decade in mass(where dark matter axions would be)
Plus operations into second decade of mass(where unusual axions might be)
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CARRACK: Kyoto RF cavity axion search
Their apparatus is similar to that of ADMX, excepttheir receiver is an exotic “microwave-photon phototube”
∆n ⋅ ∆φ ≥1
For any detector of electromagnetic radiation, there’s anumber-of-quanta, phase-of-radiation uncertainty relation:
If you don’t measure the electromagnetic phase φ,you can measure the number of quanta n to arbitrarily high precision.
This phototube for microwave photons can evade thestandard quantum limit of phase-sensitive detectors.
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Rydberg-atom single-microwave-quantum detector
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Single-microwave-photon counting
Single-microwave-photoncounting
GHz levelspacing
sensitivity goal
Operating a 3 GHz cavity (12 µeV axion mass)with calibrations and studies of “dark” current.
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Radio telescope axion search
a
γ
γAxions in halos of astrophysical objectsspontaneously decay into photons;the lifetime is long (1050 seconds),but there are a lot of halo axions.
Synthetic axion line overlaid onpower spectrum from dwarf galaxy
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Radio telescope search:Current limits and projected sensitivities
Projected sensitivities
Limits from nearbydwarf galaxies
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CAST solar axion search
CERN Axion Solar Telescope
0 2 4 6 8 10E(keV)
0
2×1014
4×1014
6×1014
8×1014
mc2
c es
1V
e k1 Axions from the sun…
…become x-rays inside an LHC dipole magnet
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CAST technologyState-of-the-art x-ray detection borrowed from astrophysics
Micromegasx-ray camera
Grazing-incidencex-ray optics
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CAST search range
Current the bestastrophysical bounds
vary He gas pressure tomatch dispersion relation
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5th force searchesAxions mediate matter-spin couplings
ψ1
V ~ 1/r( )e−r /λ σ ⋅ ˆ r
QuickTime™ and aTIFF (LZW) decompressor
are needed to see this picture.
Ni et al. 1999
ψ2
ags iγ5gp
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Overall status
SN1987AExperiments are nowsensitive to realisticaxions in the allowedmass window
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Conclusions
A Peccei-Quinn symmetry remains a promisingsolution to the Strong CP Problem; hence axions,and axions are an attractive dark-matter candidate.
Current experiments are finally sensitive to realistic axioncouplings and masses; they could see an axion at any time.
Upgrades are underway for definitive axion searches.These would be sensitive to even the more feeble axion couplingsand would either detect or rule-out Peccei-Quinn axions.
This is an exciting time for axion searchers.
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