English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

It is known that haloscopes that search for dark matter axions via theaxion-photon anomaly are also sensitive to gravitational radiation through theinverse Gertsenshtein effect. Recently this way of searching for high frequencygravitational waves has gained momentum as it has been shown that the strainsensitivities of such detectors are of the same order of sensitivity to theaxion-photon theta angle. Thus, after calculating the sensitivity of ahaloscope to an axion signal, we also have calculated the order of magnitudesensitivity to a gravitational wave signal of the same spectral and temporalform. However, it is unlikely that a gravitational wave and an axion signalwill be of the same form, since physically the way the signals are generatedare completely different. For gravitational wave detection, the spectral strainsensitivity is in units strain per square root Hz, is the natural way tocompare the sensitivity of gravitational wave detectors due to its independenceon the gravitational wave signal. In this work, we introduce a systematic wayto calculate the spectral sensitivity of an axion haloscope, so instrumentcomparison may be achieved independent of signal assumptions and only dependson the axion to signal transduction sensitivity and noise in the instrument.Thus, the calculation of the spectral sensitivity not only allows thecomparison of dissimilar axion detectors independent of signal, but also allowsus to compare the order of magnitude gravitational wave sensitivity in terms ofspectral strain sensitivity, allowing comparisons to standard gravitationalwave detectors based on optical interferometers and resonant-mass technology.

Comparing Instrument Spectral Sensitivity of Dissimilar Electromagnetic Haloscopes to Axion Dark Matter and High Frequency Gravitational Waves