Search for dark photon dark matter: Dark E field radio pilot experiment
Search for dark photon dark matter: Dark E field radio pilot experiment
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DOI：
10.1103/physrevd.104.012013
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发表时间：
2021-01
影响因子：
5
通讯作者：
Benjamin Godfrey;J. Tyson;S. Hillbrand;J. Balajthy;D. Polin;S. Tripathi;S. Klomp;Joseph Levine;Nate MacFadden;B. Kolner;M. Smith;P. Stucky;A. Phipps;P. Graham;K. Irwin
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文献类型：
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作者：
Benjamin Godfrey;J. Tyson;S. Hillbrand;J. Balajthy;D. Polin;S. Tripathi;S. Klomp;Joseph Levine;Nate MacFadden;B. Kolner;M. Smith;P. Stucky;A. Phipps;P. Graham;K. Irwin
我们正在建立一个实验，以寻找暗物质的形式在纳米到毫电子伏特的质量范围内的暗光子。本实验是电磁双磁探测器暗射电实验。它也是一个频率-时间双重实验，有两种方式：我们在宽带数据中搜索高Q信号，而不是调谐高Q谐振器，并且我们测量电场而不是磁场。在本文中，我们描述了一个试点实验，使用室温下的电子学，证明了可行性，并设置有用的限制动力学耦合$\xA 1\sim 10^{-12}$超过50- 300 MHz。随着实时光谱覆盖率增加2000倍，系统噪声温度降低，很快就有可能以100倍的灵敏度搜索大范围的质量。我们描述了两个阶段的计划实验：第一阶段将实现一个宽带，500万通道，实时FFT处理器在30- 300 MHz的范围与后端时域最佳滤波器搜索预测的Q\sim 10^6$线使用低噪声放大器。我们已经完成了点频率校准使用双锥偶极天线在屏蔽室，外推到5\sigma$限制为$\sigma\sim 10^{-13}$的耦合从暗场，每月的积分。第二阶段将使用低温前置放大器和新天线将搜索扩展到20 GHz。
We are building an experiment to search for dark matter in the form of dark photons in the nano- to milli-eV mass range. This experiment is the electromagnetic dual of magnetic detector dark radio experiments. It is also a frequency-time dual experiment in two ways: We search for a high-Q signal in wide-band data rather than tuning a high-$Q$ resonator, and we measure electric rather than magnetic fields. In this paper we describe a pilot experiment using room temperature electronics which demonstrates feasibility and sets useful limits to the kinetic coupling $\epsilon \sim 10^{-12}$ over 50--300 MHz. With a factor of 2000 increase in real-time spectral coverage, and lower system noise temperature, it will soon be possible to search a wide range of masses at 100 times this sensitivity. We describe the planned experiment in two phases: Phase-I will implement a wide band, 5-million channel, real-time FFT processor over the 30--300 MHz range with a back-end time-domain optimal filter to search for the predicted $Q\sim 10^6$ line using low-noise amplifiers. We have completed spot frequency calibrations using a biconical dipole antenna in a shielded room that extrapolate to a $5 \sigma$ limit of $\epsilon\sim 10^{-13}$ for the coupling from the dark field, per month of integration. Phase-II will extend the search to 20 GHz using cryogenic preamplifiers and new antennas.