Particle Astrophysics in a Can: The ADMX-HF Experiment · f f f Q a τ δ Neglects coherence...
Transcript of Particle Astrophysics in a Can: The ADMX-HF Experiment · f f f Q a τ δ Neglects coherence...
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Particle Astrophysics in
a Can: The ADMX-HF
Experiment Presented by S.K. Lamoreaux
Collaborators: Yulia Gurevich, Ben Brubaker, Sidney Cahn: Yale
Karl van Bibber, Jaben Root: UC Berkeley Konrad Lehnert, Mehmet Ali Anil: Univ. Colo./JILA
Tim Shokair, Gp Carosi, LBNL FUNDING: NSF Paticle Astrophysics
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standard model
• Amazingly successful in the “gauge” sector*
• Many problems in “flavor” sector—considerable success in correlating data but at the expense of many phenomenological input parameters
(* except the overall phase of the quark mass matrix is physically meaningful)
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The Strong CP Problem
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• θ is small based on experiment: ~10-9
• Can set it to zero however standard model CP violation will
induce, diverges at 14th order • Peccei and Quinn: a new symmetry U(1)PQ implying the existence
of a new particle (Wilczek, Weinberg)
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(F. Wilczek, INT Axion Workshop)
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The Dark Matter Problem • Dark matter is in fact (nearly) invisible matter except via its
gravitational effect • Gravitationally bound to galaxies (v/c~10-3) to account for rotation
velocity/distance anomalies • Can’t be neutrinos (Fermi velocity is too high) • Assumed to be particles; the higher the mass the higher the
temperature (velocity is specified) • Main focus has been on WIMPs or supersymmetric particles:
increasing sensitivity of EDM experiments together with lack of an LHC signal is disfavoring supersymmetry as an explanation of anything
• The Axion, long known as a possible solution, is receiving renewed attention
• The Axion has other applications in astrophysics
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ADMX Phase II
ADMX-HF
R&D effort currently underway
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Axions will interact with an EM field
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10-24 W is an interesting power level
Basic Experiment
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How Much Q? • Perhaps we want the cavity bandwidth to match the galactic axion effective
bandwidth: “Maxwell-Boltzmann Distribution” and cavity interaction time both contribute to Qa 2R=D cavity diameter
• If the interaction time is for a random uncorrelated field (size of cavity)
1500/103
2)5.11(22 7 ≈×
⋅===
scmR
RcmGHzf
ffQa τ
δ
Neglects coherence length: approximately ½ de Broglie wavelength
6222
2
10)2/(22 ====== −− βτδ
cvv
vmhhcmf
ffQ aa
a
Which applies when the coherence length >> R
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QL-1=Qw
-1+Qo-1 is the “loaded Q”
High Q (low bandwidth) limits maximum scan speed Intrinsic cavity wall loss and output power coupling loss (optimum signal to
noise when coupling is approximately equal to wall loss) QL
-1=Qw-1+Qo
-1
No real reason to not reduce QW
-1 to near-zero (some technical questions, e.g. amplifier stability). We can make QL anything we want
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Dicke Radiometer equation
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Overall Scheme
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Cryomagnetics Magnet: Being Fabricated
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The Cavity
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The Amplifier • HEMT amplifier fed by Josephson Parameteric Array; can achieve
“standard quantum limit” for noise
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The “Hybrid” superconducting cavity concept
*slides from Karl van Bibber
Skin depth of Copper
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The “Hybrid” superconducting cavity concept
*slides from Karl van Bibber
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Superconducting Films • A bulk superconductor expels fields from the interior; for type II, a “normal”
layer forms near the surface, separated by a thin transition layer (Abrikosov) between the regions
• For a thin film, the entire layer is in a mixed state, if the applied field is nearly perpendicular to the thin direction
• This thin film provides a superconducting boundary condition • D. Tanner suggests that this can be used to improve cavity Q for ADMX
experiments
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• Magnetic-force microscopy of Vortex Lattice, 2002
• Magnetic Force Microscopy Nb film, 40G, 4.3K A. Volodin et al. Katholieke Universiteit Leuven Europhys. Lett. 58, 582 (2002)
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Requirements
• Strong field must be parallel to surface • Perpendicular field forms vorticies in plane
of film • Require a very homogeneous magnet and
precision alignment • Main cylinder and tuning rods coatings can
be effective; cylinder endcaps are perpendicular to field
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How Well Can We Do?
• Need to consider tuning rods • Case study: 1 cm rods, Cu, 4
symmetrically placed
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Comsol Results
10 cm diameter, 15 cm long cavity; effect of coating only the cylinder and both cylinder/tuning rods with superconductor
Cyl+rods
Cyl only
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20 cm long, 7.5 cm dia cavity, 4 1 cm rods
100 x Cu
10 x Cu
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Requirements • Need 100 times better conductivity than Cu in the
anomalous skin depth region • At any frequency other than “0”, a superconductor
presents a finite resistance • Vortices increase this resistance, and the vortex density
is proportional to the perpendicular field • <100 G perpendicular field is required– need well-
designed magnet, careful alignment (.01 T/10 T=.001 radians=.06 deg)
• Magnet has been designed and built for ADMX-HF, by Cryomagnetics, Oak Ridge
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R&D has already begun on NbTiN superconducting coatings
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Rutherford backscattering of 20 min NbTi deposition on
copper foil TiNb_3-3.AS1SimulatedO TiCuNb
Channel800600400200
Cou
nts
6,000
4,000
2,000
0
600 800 1000 1200 1400 1600 1800 2000 2200 2400 2600
Energy [keV]
Nb
Ti
O
45 nm Ti0.48Nb0.63O1.9 on 40 nm Ti0.36Cu0.15Nb0.66O1.8
*courtesy of Dr. Kin Man Yu of LBNL
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Superconducting coatings will be placed on 1” cavity barrels
Initial cryogenic tests on small cavities at LLNL followed by magnetic field at Yale. If successful scale to larger cavities.
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Test Apparatus at Yale
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Improved Higher Frequency Cavity
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Schedule