The Future of Dark-Matter Axion Searches

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Presentation transcript:

The Future of Dark-Matter Axion Searches Darin Kinion (LLNL/UC Berkeley) December 9, 2004

Axions and the Strong-CP Problem

Axion properties

The “axion window” The parameter space is bounded both in mass and coupling constant.

How to detect dark-matter axions (Sikivie, 1983)

Axion Dark-Matter Experiment (ADMX) Located at LLNL (Livermore, CA) ADMX Collaboration – LLNL, UF, UCB and NRAO Started data taking in February 1996.

ADMX receiver and data candidates world’s quietest radio receiver Data from 725 – 800 MHz To date, all candidates have either disappeared upon re-scanning or have been linked to external interference

Current ADMX limits Particle Physics Astrophysics ra » rhalo ¼ 0.45 GeV/cm3 Definitive experiment requires relaxing the constraint on the axion halo density as well as achieving sensitivity to DFSZ model axions.

The ADMX upgrade plan Goal : Increase the sensitivity (scan rate) by lowering the system noise temperature 1.5 K pumped LHe 2.0 K GaAs HFET amp Phase I – Improve TN with lower noise microwave amplifiers Phase II – Improve Ts with a dilution refrigerator

Phase I Upgrade – SQUID Amplifiers

Microstrip amplifiers

ADMX hardware design for Phase I 1K Pot Cavity Main Magnet 50 cm Field-free region Field cancellation coil Force compensation coil Longitudinal field on axis

Summary of ADMX Current experiment is sensitive to KSVZ axions if they dominate the local galactic halo density Phase I upgrade is underway to improve sensitivity by replacing GaAs HFET amps with SQUIDs. Phase II upgrade would provide an order-of-magnitude improvement in sensitivity by cooling the cavity and SQUID to < 100 mK. Long-term development plan involves higher-frequency cavities and amplifiers.

Other axion searches The Kyoto Rydberg Atom detector The CERN Axion Solar Telescope Sun CERN

Summary of axion exclusion regions CAST (projected) ADMX Upgrade

Summary The Peccei-Quinn mechanism remains the most compelling solution to the Strong-CP problem in QCD ADMX is currently exploring the lowest decade of the axion window at KSVZ sensitivity The goal of the two-phase ADMX upgrade is to cover the lowest two decades of the axion window with sensitivity to DFSZ axions comprising a fraction of the galactic halo