A. Wagner

Search for Hidden Sector Photons with the ADMX Detector

Hidden U(1) gauge symmetries are common to many extensions of the standard model proposed to explain dark matter. The hidden gauge vector bosons of such extensions may mix kinetically with standard model photons, providing a means for electromagnetic power to pass through conducting barriers. The axion dark matter experiment detector was used to search for hidden vector bosons originating in an emitter cavity driven with microwave power. We exclude hidden vector bosons with kinetic couplings χ>3.48×10⁻⁸ for masses less than 3  μeV. This limit represents an improvement of more than 2 orders of magnitude in sensitivity relative to previous cavity experiments.

Search for nonvirialized axionic dark matter

Cold dark matter in the Milky Way halo may have structure defined by flows with low velocity dispersion. The Axion Dark Matter eXperiment high resolution channel is especially sensitive to axions in such low velocity dispersion flows. Results from a combined power spectra analysis of the high resolution channel axion search are presented along with a discussion of the assumptions underlying such an analysis. We exclude Kim-Shifman-Vainshtein-Zakharov axion dark matter densities of � * 0:2 GeV=cm 3 and Dine-Fischler-Srednicki-Zhitnitskii densities of � * 1:4 GeV=cm 3 over a mass range of ma ¼ 3:3 � eV to 3:69 � eV for models having velocity dispersions of � � & 3 � 10 � 6 .

Design and performance of the ADMX SQUID-based microwave receiver

The article of record as published may be located at http://dx.doi.org/10.1016/j.nima.2011.07.019

Modulation sensitive search for nonvirialized dark-matter axions

Non-virialized dark-matter axions may be present in the Milky Way halo in the form of low-velocity-dispersion flows. The Axion Dark Matter eXperiment performed a search for the conversion of these axions into microwave photons using a resonant cavity immersed in a strong, static magnetic field. The spread of photon energy in these measurements was measured at spectral resolutions of the order of 1 Hz and below. If the energy variation were this small, the frequency modulation of any real axion signal due to the orbital and rotational motion of the Earth would become non-negligible. Conservative estimates of the expected signal modulation were made and used as a guide for the search procedure. The photon frequencies covered by this search are 812

Search for dark matter axions with the Orpheus experiment

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Limits on axion–photon coupling or on local axion density: Dependence on models of the Milky Way’s dark halo

852 and 858

The axion dark-matter eXperiment: Results and plans

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A Technique to Search for High Mass Dark Matter Axions

892 MHz, which correspond to an axion mass of 3.36

ADMX Phase II: Progress and Expected Sensitivity

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Searching for hidden Sector Photons and Chameleons with ADMX

3.52 and 3.55