Ultralight vector dark matter search with auxiliary length channels of gravitational wave detectors
Ultralight vector dark matter search with auxiliary length channels of gravitational wave detectors
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DOI：
10.1103/physrevd.102.102001
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发表时间：
2020-08
影响因子：
5
通讯作者：
Y. Michimura;Tomohiro Fujita;S. Morisaki;Hiromasa Nakatsuka;Ippei Obata
中科院分区：
文献类型：
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作者：
Y. Michimura;Tomohiro Fujita;S. Morisaki;Hiromasa Nakatsuka;Ippei Obata
最近，通过测量引力波探测器臂腔中振荡长度的变化来寻找超轻暗物质已经引起了相当大的关注。虽然引力波探测器在测量微分臂长变化方面非常灵敏，但对暗物质的灵敏度却大大减弱，因为暗物质的影响在臂腔测试质量中最常见。在这里，我们建议使用辅助长度通道，它测量功率和信号循环腔长度以及差分迈克尔逊干涉仪长度的变化。通过利用辅助干涉仪比两个臂腔更不对称的事实，可以增强对暗物质的敏感性。结果表明，将我们的方法应用于采用蓝宝石测试质量和熔融石英辅镜的低温引力波探测器KAGRA，可以大大提高对质量小于$7\ifmmode\times\else\texttimes\fi{}{10}^{\ensuremath{-}14}\text{的规范玻色子暗物质的灵敏度。我们发现，在不对现有干涉仪进行任何修改的情况下，KAGRA可以探测$1.5\ifmmode\times\else\texttimes\fi{}{10}^{\ensuremath{-}14}\text{\TEXT{}MATHROM{EV}$周围质量超过一个数量级的未知参数空间。
Recently, a considerable amount of attention has been given to the search for ultralight dark matter by measuring the oscillating length changes in the arm cavities of gravitational wave detectors. Although gravitational wave detectors are extremely sensitive for measuring the differential arm length changes, the sensitivity to dark matter is largely attenuated, as the effect of dark matter is mostly common to arm cavity test masses. Here, we propose to use auxiliary length channels, which measure the changes in the power and signal recycling cavity lengths and the differential Michelson interferometer length. The sensitivity to dark matter can be enhanced by exploiting the fact that auxiliary interferometers are more asymmetric than two arm cavities. We show that the sensitivity to $\mathrm{U}(1{)}_{B\ensuremath{-}L}$ gauge boson dark matter with masses below $7\ifmmode\times\else\texttimes\fi{}{10}^{\ensuremath{-}14}\text{ }\text{ }\mathrm{eV}$ can be greatly enhanced when our method is applied to a cryogenic gravitational wave detector KAGRA, which employs sapphire test masses and fused silica auxiliary mirrors. We show that KAGRA can probe more than an order of magnitude of unexplored parameter space at masses around $1.5\ifmmode\times\else\texttimes\fi{}{10}^{\ensuremath{-}14}\text{ }\text{ }\mathrm{eV}$, without any modifications to the existing interferometer.