标题： 比较不同电磁阿基米德仪的仪器光谱灵敏度与轴子暗物质和高频引力波 显示英文标题

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

摘要： 已知通过轴子-光子异常搜索暗物质轴子的卤素探测器也通过逆Gertsenshtein效应对引力辐射敏感。最近，由于已经表明此类探测器的应变灵敏度与轴子-光子θ角的灵敏度在同一数量级，因此通过这种方式搜索高频引力波的方法重新获得了动力。因此，在计算了卤素探测器对轴子信号的灵敏度后，我们也计算了相同频谱和时间形式的引力波信号的数量级灵敏度。然而，由于引力波和轴子信号的产生方式在物理上完全不同，它们不太可能具有相同的形态。对于引力波探测，频谱应变灵敏度的单位是应变每平方根赫兹，这是比较引力波探测器灵敏度的自然方式，因为它不依赖于引力波信号。在这项工作中，我们介绍了一种系统的方法来计算轴子卤素探测器的频谱灵敏度，从而使仪器比较可以独立于信号假设，并且仅取决于轴子到信号的转换灵敏度和仪器中的噪声。因此，频谱灵敏度的计算不仅允许独立于信号比较不同的轴子探测器，还允许我们根据频谱应变灵敏度来比较引力波灵敏度的数量级，从而可以基于光学干涉仪和共振质量技术的标准引力波探测器进行比较。 显示英文摘要

摘要： It is known that haloscopes that search for dark matter axions via the axion-photon anomaly are also sensitive to gravitational radiation through the inverse Gertsenshtein effect. Recently this way of searching for high frequency gravitational waves has gained momentum as it has been shown that the strain sensitivities of such detectors are of the same order of sensitivity to the axion-photon theta angle. Thus, after calculating the sensitivity of a haloscope to an axion signal, we also have calculated the order of magnitude sensitivity to a gravitational wave signal of the same spectral and temporal form. However, it is unlikely that a gravitational wave and an axion signal will be of the same form, since physically the way the signals are generated are completely different. For gravitational wave detection, the spectral strain sensitivity is in units strain per square root Hz, is the natural way to compare the sensitivity of gravitational wave detectors due to its independence on the gravitational wave signal. In this work, we introduce a systematic way to calculate the spectral sensitivity of an axion haloscope, so instrument comparison may be achieved independent of signal assumptions and only depends on the axion to signal transduction sensitivity and noise in the instrument. Thus, the calculation of the spectral sensitivity not only allows the comparison of dissimilar axion detectors independent of signal, but also allows us to compare the order of magnitude gravitational wave sensitivity in terms of spectral strain sensitivity, allowing comparisons to standard gravitational wave detectors based on optical interferometers and resonant-mass technology.