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

Transcript of Particle Astrophysics in a Can: The ADMX-HF Experiment · f f f Q a τ δ Neglects coherence...

Page 1: Particle Astrophysics in a Can: The ADMX-HF Experiment · f f f Q a τ δ Neglects coherence length: approximately ½ de Broglie wavelength . 2 2 2 6 2 10 /( 2 ) τ 2 2 − β−=

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