axion dark matter experiment - institute for nuclear theory• admx-axion dark matter experiment...
TRANSCRIPT
![Page 1: Axion Dark Matter eXperiment - Institute for Nuclear Theory• ADMX-Axion Dark Matter eXperiment Florida, LBNL/Berkeley, LLNL C Hagmann, et. al, Phys. Rev. Lett. 80, 2043 (1998) SJ](https://reader035.vdocument.in/reader035/viewer/2022070700/5e5344c4cc0b2342b60dfed1/html5/thumbnails/1.jpg)
Axion Dark
Matter eXperiment
Steve AsztalosLLNL
Collaborators: UC Berkeley, U Florida, NRAO
TAUP ‘03
![Page 2: Axion Dark Matter eXperiment - Institute for Nuclear Theory• ADMX-Axion Dark Matter eXperiment Florida, LBNL/Berkeley, LLNL C Hagmann, et. al, Phys. Rev. Lett. 80, 2043 (1998) SJ](https://reader035.vdocument.in/reader035/viewer/2022070700/5e5344c4cc0b2342b60dfed1/html5/thumbnails/2.jpg)
Sky&Telescope Nov, 2000
The Nature of Dark MatterMass and Energy Content of the Universe
Wm, the density of all matter.Wb, the density of “ordinary” matter.
WL, the “dark energy” density.
Three important components:≡Wi
ri /rc
Âi
Wi ~ 1
Axions, WIMPs, etc.
![Page 3: Axion Dark Matter eXperiment - Institute for Nuclear Theory• ADMX-Axion Dark Matter eXperiment Florida, LBNL/Berkeley, LLNL C Hagmann, et. al, Phys. Rev. Lett. 80, 2043 (1998) SJ](https://reader035.vdocument.in/reader035/viewer/2022070700/5e5344c4cc0b2342b60dfed1/html5/thumbnails/3.jpg)
If you see an EDM: T + CPT = CP
The discrete symmetry “mirrors”
T ≡ time reversal
C ≡ changing particles to antiparticles
P ≡ space inversion
spinningball
Tmirror
J
J
dE dE
The story of spinning balls, electric dipole momentsand CP violation
Axion PhysicsSearching for Strong CP Violation
![Page 4: Axion Dark Matter eXperiment - Institute for Nuclear Theory• ADMX-Axion Dark Matter eXperiment Florida, LBNL/Berkeley, LLNL C Hagmann, et. al, Phys. Rev. Lett. 80, 2043 (1998) SJ](https://reader035.vdocument.in/reader035/viewer/2022070700/5e5344c4cc0b2342b60dfed1/html5/thumbnails/4.jpg)
q
fine tuning
q
dynamics
mass
pivot
by turning screws
by itself
Here’s what happened:
Added a potential V = mg (1— cosq)
Pool table settled to
Sikivie, Physics Today, 1996
Axion Physics Sikivie’s Pool Table Analogy...
![Page 5: Axion Dark Matter eXperiment - Institute for Nuclear Theory• ADMX-Axion Dark Matter eXperiment Florida, LBNL/Berkeley, LLNL C Hagmann, et. al, Phys. Rev. Lett. 80, 2043 (1998) SJ](https://reader035.vdocument.in/reader035/viewer/2022070700/5e5344c4cc0b2342b60dfed1/html5/thumbnails/5.jpg)
The axion is a pseudoscalar whose mass is a priori unknown
Low-mass axions are good dark matter candidatesbut couple feebly, and thus are hard to detect
Cosmological Connections
Axion couplings: It can do most anything a p0 can do
For example:
Produced cold (in early universe phasetransition). They never thermalize
![Page 6: Axion Dark Matter eXperiment - Institute for Nuclear Theory• ADMX-Axion Dark Matter eXperiment Florida, LBNL/Berkeley, LLNL C Hagmann, et. al, Phys. Rev. Lett. 80, 2043 (1998) SJ](https://reader035.vdocument.in/reader035/viewer/2022070700/5e5344c4cc0b2342b60dfed1/html5/thumbnails/6.jpg)
The combination of accelerator searches,astrophysical and cosmological arguments leaves a
search window 10-6 < ma < 10-3 eV
Cosmological ConnectionsConstraints circa 1995
![Page 7: Axion Dark Matter eXperiment - Institute for Nuclear Theory• ADMX-Axion Dark Matter eXperiment Florida, LBNL/Berkeley, LLNL C Hagmann, et. al, Phys. Rev. Lett. 80, 2043 (1998) SJ](https://reader035.vdocument.in/reader035/viewer/2022070700/5e5344c4cc0b2342b60dfed1/html5/thumbnails/7.jpg)
Cosmological ImplicationsSummary of Constraints
Discovering massive axions still solves the strong-CP problem, but not the dark matter problem.
Hence the emphasis on searches for light axions.
ADMXCARRACKCAST
![Page 8: Axion Dark Matter eXperiment - Institute for Nuclear Theory• ADMX-Axion Dark Matter eXperiment Florida, LBNL/Berkeley, LLNL C Hagmann, et. al, Phys. Rev. Lett. 80, 2043 (1998) SJ](https://reader035.vdocument.in/reader035/viewer/2022070700/5e5344c4cc0b2342b60dfed1/html5/thumbnails/8.jpg)
Sikivie, 1983
a
g
nearby galactichalo axion
microwavephoton
virtualphoton
cryogenic high Qmicrowave cavity
high fieldsolenoidalmagnet
ultra-low noisedetector
cavity electric field
externalmagnetic field
Condition forresonant conversion:hn @ mac2
powerdensity
frequency
axion signal, width J(10-6 n0)
electronicscavity thermal
system output:
Local axion number density ~ 1013/cc
Microwave Cavity Approach _______________________ADMX
![Page 9: Axion Dark Matter eXperiment - Institute for Nuclear Theory• ADMX-Axion Dark Matter eXperiment Florida, LBNL/Berkeley, LLNL C Hagmann, et. al, Phys. Rev. Lett. 80, 2043 (1998) SJ](https://reader035.vdocument.in/reader035/viewer/2022070700/5e5344c4cc0b2342b60dfed1/html5/thumbnails/9.jpg)
_______________________ADMXSingle Cavity Tuning
Axion mass is unknown
Cavity must be tuneable.
50 cm
300 MHz < Tuning range < 800 MHz
n0 (TM010) = 0.115/R GHz
![Page 10: Axion Dark Matter eXperiment - Institute for Nuclear Theory• ADMX-Axion Dark Matter eXperiment Florida, LBNL/Berkeley, LLNL C Hagmann, et. al, Phys. Rev. Lett. 80, 2043 (1998) SJ](https://reader035.vdocument.in/reader035/viewer/2022070700/5e5344c4cc0b2342b60dfed1/html5/thumbnails/10.jpg)
Single Cavity Tuning
Tuning motion accomplishedby 40000:1 reduction gears (~100 nm radial displacement)
_______________________ADMX
Cavity, amplifier and drives @1.3 K in 4-7 Tfield
![Page 11: Axion Dark Matter eXperiment - Institute for Nuclear Theory• ADMX-Axion Dark Matter eXperiment Florida, LBNL/Berkeley, LLNL C Hagmann, et. al, Phys. Rev. Lett. 80, 2043 (1998) SJ](https://reader035.vdocument.in/reader035/viewer/2022070700/5e5344c4cc0b2342b60dfed1/html5/thumbnails/11.jpg)
_______________________ADMXReceiver Chain
Hi-resolutionMedium-resolution
Not so different from your FM tuner…
![Page 12: Axion Dark Matter eXperiment - Institute for Nuclear Theory• ADMX-Axion Dark Matter eXperiment Florida, LBNL/Berkeley, LLNL C Hagmann, et. al, Phys. Rev. Lett. 80, 2043 (1998) SJ](https://reader035.vdocument.in/reader035/viewer/2022070700/5e5344c4cc0b2342b60dfed1/html5/thumbnails/12.jpg)
…except that its sensitivity approaches 10-24 Watts
_______________________ADMXMedium Resolution Receiver Chain
![Page 13: Axion Dark Matter eXperiment - Institute for Nuclear Theory• ADMX-Axion Dark Matter eXperiment Florida, LBNL/Berkeley, LLNL C Hagmann, et. al, Phys. Rev. Lett. 80, 2043 (1998) SJ](https://reader035.vdocument.in/reader035/viewer/2022070700/5e5344c4cc0b2342b60dfed1/html5/thumbnails/13.jpg)
Data Processing
We see statistical peaks, environmental interference,and calibration signals
frequency (MHz)devi
atio
n fr
om m
ean
pow
er (
std
devi
atio
ns) calibration signal
log
num
ber
deviations
Calibrationpeak
Spectra are combined
_______________________ADMX
![Page 14: Axion Dark Matter eXperiment - Institute for Nuclear Theory• ADMX-Axion Dark Matter eXperiment Florida, LBNL/Berkeley, LLNL C Hagmann, et. al, Phys. Rev. Lett. 80, 2043 (1998) SJ](https://reader035.vdocument.in/reader035/viewer/2022070700/5e5344c4cc0b2342b60dfed1/html5/thumbnails/14.jpg)
Recent results
550 to 810 MHz (single cavity)ApJL, Asztalos et al., 571, L27 (2002)PRL, 80, Hagmann et al., 2043-2046 (1998)
1.1 GHz (four cavities)PhD Thesis D. Kinion DAS (2001)
461 to 550 MHz(single cavity)PRDr D.B.Yu et al. (2003?)
_______________________ADMX~ 10-22 Watts !
![Page 15: Axion Dark Matter eXperiment - Institute for Nuclear Theory• ADMX-Axion Dark Matter eXperiment Florida, LBNL/Berkeley, LLNL C Hagmann, et. al, Phys. Rev. Lett. 80, 2043 (1998) SJ](https://reader035.vdocument.in/reader035/viewer/2022070700/5e5344c4cc0b2342b60dfed1/html5/thumbnails/15.jpg)
Recent results (cont.) _______________________ADMX
Increased sensitivity translates into ~ 25% increasein scanning speed
![Page 16: Axion Dark Matter eXperiment - Institute for Nuclear Theory• ADMX-Axion Dark Matter eXperiment Florida, LBNL/Berkeley, LLNL C Hagmann, et. al, Phys. Rev. Lett. 80, 2043 (1998) SJ](https://reader035.vdocument.in/reader035/viewer/2022070700/5e5344c4cc0b2342b60dfed1/html5/thumbnails/16.jpg)
Hi-res channel increases our search sensitivity; anysignal would contain a time-ordered history of
galaxy formation.
_______________________ADMXHigh Resolution Data
![Page 17: Axion Dark Matter eXperiment - Institute for Nuclear Theory• ADMX-Axion Dark Matter eXperiment Florida, LBNL/Berkeley, LLNL C Hagmann, et. al, Phys. Rev. Lett. 80, 2043 (1998) SJ](https://reader035.vdocument.in/reader035/viewer/2022070700/5e5344c4cc0b2342b60dfed1/html5/thumbnails/17.jpg)
Below 440 MHz our search becomes ponderous…How can it be sped up?
Search rate at fixed SNR:
Already near maximum for copper
bigger B: 10-12 Tesla $5M+bigger B: 10-12 Tesla $5M+bigger V: larger center bore magnetsmaller TN: SQUID amplifiers
*All SQUID data and figures that follow: Berkeley: J.Clarke, M-.Andre Giessen: M.Muck
SQUIDS – A Path to an Upgrade
Great success in applying DC SQUIDS tomicrowave amplification*
_______________________ADMX
Increase B,V; decrease TN
![Page 18: Axion Dark Matter eXperiment - Institute for Nuclear Theory• ADMX-Axion Dark Matter eXperiment Florida, LBNL/Berkeley, LLNL C Hagmann, et. al, Phys. Rev. Lett. 80, 2043 (1998) SJ](https://reader035.vdocument.in/reader035/viewer/2022070700/5e5344c4cc0b2342b60dfed1/html5/thumbnails/18.jpg)
fi t ~ TN2
1st decade sensitivity to even pessimistic axioncouplings at fractional dark matter halo density
Near Quantum-LimitedAmplification _______________________ADMX
![Page 19: Axion Dark Matter eXperiment - Institute for Nuclear Theory• ADMX-Axion Dark Matter eXperiment Florida, LBNL/Berkeley, LLNL C Hagmann, et. al, Phys. Rev. Lett. 80, 2043 (1998) SJ](https://reader035.vdocument.in/reader035/viewer/2022070700/5e5344c4cc0b2342b60dfed1/html5/thumbnails/19.jpg)
Upgrade Mechanical Layout
Merely replacing our HEMT amplifiers withSQUIDS will increase our scan speed 4x.
The SQUIDS will occupy a field-free regioncreated by a bucking coil; design is well advanced
Entire upgrade successfully through SAGENAPand Lehman reviews.
_______________________ADMX
![Page 20: Axion Dark Matter eXperiment - Institute for Nuclear Theory• ADMX-Axion Dark Matter eXperiment Florida, LBNL/Berkeley, LLNL C Hagmann, et. al, Phys. Rev. Lett. 80, 2043 (1998) SJ](https://reader035.vdocument.in/reader035/viewer/2022070700/5e5344c4cc0b2342b60dfed1/html5/thumbnails/20.jpg)
Conclusions
• The resolution of the Strong CP Problem is verylikely due to a new chiral symmetry. Axions are anatural solution and is an excellent cold dark mattercandidate.
• ADMX is now in its 7th year of operation. Duringthis latest run we have:
- Deployed lower noise HEMT amplifiers- Taken an additional 90 MHz of data- Shown to have perhaps the lowest noise receiver in the world.- Analyzed data to achieve a better sensitivity- Implemented and analyzed a high resolution data channel
• DOE OS has essentially committed to a FY ’04axion upgrade
![Page 21: Axion Dark Matter eXperiment - Institute for Nuclear Theory• ADMX-Axion Dark Matter eXperiment Florida, LBNL/Berkeley, LLNL C Hagmann, et. al, Phys. Rev. Lett. 80, 2043 (1998) SJ](https://reader035.vdocument.in/reader035/viewer/2022070700/5e5344c4cc0b2342b60dfed1/html5/thumbnails/21.jpg)
![Page 22: Axion Dark Matter eXperiment - Institute for Nuclear Theory• ADMX-Axion Dark Matter eXperiment Florida, LBNL/Berkeley, LLNL C Hagmann, et. al, Phys. Rev. Lett. 80, 2043 (1998) SJ](https://reader035.vdocument.in/reader035/viewer/2022070700/5e5344c4cc0b2342b60dfed1/html5/thumbnails/22.jpg)
Outline
Introduction: The nature of dark matter
Axion physics: born in particle physics…
Cosmological connections: …but findsa home in cosmology
Axion searches: ADMXNew results using a new analyis techniqueNew data from a separate data channelNew future?
Conclusions
![Page 23: Axion Dark Matter eXperiment - Institute for Nuclear Theory• ADMX-Axion Dark Matter eXperiment Florida, LBNL/Berkeley, LLNL C Hagmann, et. al, Phys. Rev. Lett. 80, 2043 (1998) SJ](https://reader035.vdocument.in/reader035/viewer/2022070700/5e5344c4cc0b2342b60dfed1/html5/thumbnails/23.jpg)
Mass density of cluster based on inversion of gravitationallensing. 98% of the mass is a smooth component.
Tyson et al., 1998
M/L, virial theorem, gas x-ray temperatures, Sunyaev-Zel’dolvich effect, gravitational lensing,
Indirect - microwave background, deep redshift supernovae
~30% of the matter in the universe is in someunknown, exotic form.
The Nature of Dark MatterDetection Methods
Gravitational lensing from galaxy cluster 0024-1654
}“Direct”
![Page 24: Axion Dark Matter eXperiment - Institute for Nuclear Theory• ADMX-Axion Dark Matter eXperiment Florida, LBNL/Berkeley, LLNL C Hagmann, et. al, Phys. Rev. Lett. 80, 2043 (1998) SJ](https://reader035.vdocument.in/reader035/viewer/2022070700/5e5344c4cc0b2342b60dfed1/html5/thumbnails/24.jpg)
If the spinning ball is a neutron:
Harris et al., 1999
Quite surprising (in QCD)
Naively
Thus the “Strong CP Problem”:Why is |q| < 10-9, or, equivalently,
Why is QCD CP so small?
Axion PhysicsLimits on the Electric Dipole Moment
If the spinning ball is an electron:
Romalis, Griffith, Jacobs,Fortson, 2001 (on 199Hg)
Not too surprising (in QED)
Or, e.g., less naivelyCrewther,Di Vecchia,Veneziano,Witten, 1979
![Page 25: Axion Dark Matter eXperiment - Institute for Nuclear Theory• ADMX-Axion Dark Matter eXperiment Florida, LBNL/Berkeley, LLNL C Hagmann, et. al, Phys. Rev. Lett. 80, 2043 (1998) SJ](https://reader035.vdocument.in/reader035/viewer/2022070700/5e5344c4cc0b2342b60dfed1/html5/thumbnails/25.jpg)
• ADMX- Axion Dark Matter eXperimentFlorida, LBNL/Berkeley, LLNLC Hagmann, et. al, Phys. Rev. Lett. 80, 2043 (1998)SJ Asztalos, et.al, APJL 571 27 (2002)
Conventional HFET amplificationLarge volume, high field magnet1.2K pumped 4He coolingCosmological axions in the galactic halo
Exotic single photon Rydberg atom detectorLow volume, high field magnet10mK dilution refrigerator coolingCosmological axions in the galactic halo
• CARRACK - Cosmic Axion Research withRydberg Atoms in a ResonantCavity in KyotoKyotoK Yamamoto, et. al, hep-ph/0101200
Axion Searches Photon Conversion Experiments
• CAST – CERN Axion Solar Telescope IG Irastorza, et. al, astro-ph/0211606
Low volume, high field magnetNon-cosmological axions coming fromthe sun
![Page 26: Axion Dark Matter eXperiment - Institute for Nuclear Theory• ADMX-Axion Dark Matter eXperiment Florida, LBNL/Berkeley, LLNL C Hagmann, et. al, Phys. Rev. Lett. 80, 2043 (1998) SJ](https://reader035.vdocument.in/reader035/viewer/2022070700/5e5344c4cc0b2342b60dfed1/html5/thumbnails/26.jpg)
Search for axions - ongoingSingle cavity tuning limitation
Only the TM010 cavity modehas reasonable form factor
![Page 27: Axion Dark Matter eXperiment - Institute for Nuclear Theory• ADMX-Axion Dark Matter eXperiment Florida, LBNL/Berkeley, LLNL C Hagmann, et. al, Phys. Rev. Lett. 80, 2043 (1998) SJ](https://reader035.vdocument.in/reader035/viewer/2022070700/5e5344c4cc0b2342b60dfed1/html5/thumbnails/27.jpg)
Axion SearchesMultiple Cavities for Higher Masses
10-6 10-5 10-4
0.25 2.5 25.
100 10 1
ma (eV)n (GHz)
D (cm)
?
1 m
_______________________ADMX
![Page 28: Axion Dark Matter eXperiment - Institute for Nuclear Theory• ADMX-Axion Dark Matter eXperiment Florida, LBNL/Berkeley, LLNL C Hagmann, et. al, Phys. Rev. Lett. 80, 2043 (1998) SJ](https://reader035.vdocument.in/reader035/viewer/2022070700/5e5344c4cc0b2342b60dfed1/html5/thumbnails/28.jpg)
Axion Searches4-Cavity Tuning
20 cm
_______________________ADMX
![Page 29: Axion Dark Matter eXperiment - Institute for Nuclear Theory• ADMX-Axion Dark Matter eXperiment Florida, LBNL/Berkeley, LLNL C Hagmann, et. al, Phys. Rev. Lett. 80, 2043 (1998) SJ](https://reader035.vdocument.in/reader035/viewer/2022070700/5e5344c4cc0b2342b60dfed1/html5/thumbnails/29.jpg)
SQUID Schematic Voltage Flux Relation
Berkeley and Giessen:Configure input coil as stripline resonator:
Big technical problem: Parasitic capacitanceon SQUID input coil rolls off gain.
Stripline is resonant at“shunt detuned” frequencywhere parisitic capacityis tuned out.
Z0=50W
Z0=7W
{
open-ended stripline coil
F
Axion SearchesSQUIDs as Microwave Amplifiers
_______________________ADMX
![Page 30: Axion Dark Matter eXperiment - Institute for Nuclear Theory• ADMX-Axion Dark Matter eXperiment Florida, LBNL/Berkeley, LLNL C Hagmann, et. al, Phys. Rev. Lett. 80, 2043 (1998) SJ](https://reader035.vdocument.in/reader035/viewer/2022070700/5e5344c4cc0b2342b60dfed1/html5/thumbnails/30.jpg)
_______________________CARRACK
Axion SearchesCARRACK I and II
CARRACK I – Dilution refrigerator @ 10 mKsuppresses thermal noise, thus accidental excitation ofRydberg atom. System noise limited by thermal, notamplifier noise.
8% scan around 10 meV (acquired before 2000) - datanot yet published.
CARRACK II – Proposed to scan the region 2 meV to50 meV. Present status uncertain.
![Page 31: Axion Dark Matter eXperiment - Institute for Nuclear Theory• ADMX-Axion Dark Matter eXperiment Florida, LBNL/Berkeley, LLNL C Hagmann, et. al, Phys. Rev. Lett. 80, 2043 (1998) SJ](https://reader035.vdocument.in/reader035/viewer/2022070700/5e5344c4cc0b2342b60dfed1/html5/thumbnails/31.jpg)
Platform & magnet cryogenics
Picture taken on 13th aug 2002First provoked quench of the magnet
Igor G. Irastorza, CERN / Zaragoza U. TPC Workshop, Paris, 5-6 December 2002
_______________________________CASTAxion Searches
![Page 32: Axion Dark Matter eXperiment - Institute for Nuclear Theory• ADMX-Axion Dark Matter eXperiment Florida, LBNL/Berkeley, LLNL C Hagmann, et. al, Phys. Rev. Lett. 80, 2043 (1998) SJ](https://reader035.vdocument.in/reader035/viewer/2022070700/5e5344c4cc0b2342b60dfed1/html5/thumbnails/32.jpg)
_______________________________CAST
¸Decommissioned LHC test magnet (L=10m, B=9 T)¸Moving platform (to allow up to 50 days / year of alignment)¸4 magnet bores to look for X rays¸3 X rays detector prototypes being used.¸X ray Focusing System to increase signal/noise ratio.
Igor G. Irastorza, CERN / Zaragoza U. TPC Workshop, Paris, 5-6 December 2002
Axion Searches
![Page 33: Axion Dark Matter eXperiment - Institute for Nuclear Theory• ADMX-Axion Dark Matter eXperiment Florida, LBNL/Berkeley, LLNL C Hagmann, et. al, Phys. Rev. Lett. 80, 2043 (1998) SJ](https://reader035.vdocument.in/reader035/viewer/2022070700/5e5344c4cc0b2342b60dfed1/html5/thumbnails/33.jpg)
Technology for space X-ray telescopes recycled for CAST
Igor G. Irastorza, CERN / Zaragoza U. TPC Workshop, Paris, 5-6 December 2002
_______________________________CASTAxion Searches
X-ray Focusing Device
![Page 34: Axion Dark Matter eXperiment - Institute for Nuclear Theory• ADMX-Axion Dark Matter eXperiment Florida, LBNL/Berkeley, LLNL C Hagmann, et. al, Phys. Rev. Lett. 80, 2043 (1998) SJ](https://reader035.vdocument.in/reader035/viewer/2022070700/5e5344c4cc0b2342b60dfed1/html5/thumbnails/34.jpg)
Igor G. Irastorza, CERN / Zaragoza U. TPC Workshop, Paris, 5-6 December 2002
x-y image of 6.4 keV x-ray beam in MicroMegas chamber (logscale for density)
_______________________________CASTAxion Searches
X-ray Focusing Device
Improvement of SNR ~ 200 possible
Experiment has taken commisioning data and willsoon begin operation.
![Page 35: Axion Dark Matter eXperiment - Institute for Nuclear Theory• ADMX-Axion Dark Matter eXperiment Florida, LBNL/Berkeley, LLNL C Hagmann, et. al, Phys. Rev. Lett. 80, 2043 (1998) SJ](https://reader035.vdocument.in/reader035/viewer/2022070700/5e5344c4cc0b2342b60dfed1/html5/thumbnails/35.jpg)
_______________________CARRACK
Axion SearchesSingle Photon Counting
Conversion cavity -> Detection cavity -> Selectivefield ionization
Sensitivity of this approach nearly unlimited, intheory, but difficult, in practice, to calculate.