17-22 July 2016
Master Cutlers Hall
Europe/London timezone

Conceptual design of a third-generation axion detector

21 Jul 2016, 14:20
Venue: Cutlers' Banqueting Hall (First Floor); Chair: Igor Irastorza; Session Manager: Jost Migenda ()

Venue: Cutlers' Banqueting Hall (First Floor); Chair: Igor Irastorza; Session Manager: Jost Migenda


Prof. David Tanner (University of Florida)


The Axion Dark Matter eXperiment (ADMX) is conducting a search for dark-matter axions trapped in the halo of the Milky Way Galaxy. Axions, originally postulated to solve the strong CP problem in particle physics, would have been created as cold (non-relativistic) very weakly interacting particles in the early stages of the expansion of the universe. If their mass is in the range 2 to 50 $\mu$eV, axions could be a significant component of the dark matter in the universe. The discovery of the axion, or placing limits on its abundance, would therefore have very important implications for understanding the nature of dark matter, which is one of the most significant problems in contemporary physics. Axions can be detected by their conversion to microwave photons in a strong magnetic field. This process was discovered by Sikivie in 1983 and is the basis of many searches for axions and axion-like particles. The ADMX experiment employs a high-Q, 200 litre microwave cavity that can be tuned slowly through the expected axion mass range. The cavity is held at low temperatures in a field of about 7 T. If the density of axions is close to the value required to account for all of the dark matter in our Galaxy, the signal detected would be of the order of 10-22 W. SQUID preamplifiers followed by broad-band cooled HEMT amplifiers are used to obtain the required sensitivity. The frequency is swept at a rate of the order of 2 MHz/day.To date, ADMX has ruled out axions with masses in the 2.0-3.6 $\mu$eV range ($f = mc^2/h$ of 480-860 MHz) that would be predicted by the stronger of two standard axion models. The second-generation of ADMX is commissioning a dilution refrigerator to enable 100 mK temperatures for cavity and SQUID thereby increasing the signal-to-noise ratio by 20x, allowing the full band of the expected axion mass and coupling space, even in the case of pessimistically coupled models. Expected noise temperature is 150 mK. A conceptual design and associated technology development for a third-generation axion cavity detector, optimized for searches for the case where the axion mass is above the range searched by the current ADMX, say in the 10 to 50 $\mu$eV mass range (3 to 12 GHz) will be described. The detector sensitivity is proportional to B2V, so that the dilemma for searches at higher frequencies is that cavity dimensions are comparable to the wavelength, so that the cavity becomes smaller as frequency goes up. The loss of volume can be addressed by increasing the magnetic field strength, say to 25-40 T. At the same time, a method of combining two or more cavities is being developed. The signals emitted from, a modest number of nominally identical cavities are combined together in phase and brought to the front end of the low-noise amplifier. All the cavities must resonate at the same frequency for the combination to be effective. A locking scheme using phase modulated RF signals and reflection measurements, known as the Pound or Pound, Drever, Hall (PDH) reflection locking method is being investigated. This method is used by LIGO, VIRGO, and other gravitational wave experiments to bring multiple optical cavities into mutual resonance.


The next generation microwave cavity experiment to search for dark-matter axions must search for higher mass axions. The detectors must use stronger magnetic fields and multiple microwave cavities. A conceptual desgin for such a detector will be described.

Primary author

Prof. David Tanner (University of Florida)

Presentation Materials

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