作为相干暗波量子干涉的宇宙结构
Cosmic Structure as the Quantum Interference of a Coherent Dark Wave
摘要：
传统的冷粒子解释暗物质（CDM）仍然缺乏实验室的支持，并与普通矮星系的基本性质作斗争，这些矮星系具有令人惊讶的均匀中心质量和浅密度分布。相比之下，CDM预测的星系延伸到更低的质量，更陡峭，奇异的配置文件。这种张力激发了由非相对论性的玻色-爱因斯坦凝聚体组成的冷的、波动状的暗物质（$ψ$ DM），因此不确定原理在金斯尺度下对抗引力。在这里，我们实现了前所未有的高分辨率能够解决矮星系，只有一个自由参数，$\bf{m_B}$，玻色子质量的量子态的第一个宇宙学模拟。我们证明了这种$ψ$ DM模拟的大尺度结构与CDM无法区分，正如所期望的那样，但在星系内部有根本不同。连接的细丝和坍缩的晕形成了一个大的干涉网络，每个星系内部都有引力自约束的孤子核心，周围是由波动密度颗粒组成的扩展晕。这些结果使我们能够确定$\bf{m_B=(8.1^{+1.6}_{-1.7})\times 10^{-23}~eV}$使用恒星的相空间分布在矮球状星系。密度更大，更大质量的孤子预测银河系大小的星系，提供了一个实质性的种子，以帮助解释早期球状体的形成。小结构的抑制意味着$ψ$ DM星系形成的开始相对于CDM大大延迟，在我们的模拟中出现在$\bf{z\lesssim 13}$。
英文摘要：
The conventional cold, particle interpretation of dark matter (CDM) still lacks laboratory support and struggles with the basic properties of common dwarf galaxies, which have surprisingly uniform central masses and shallow density profiles. In contrast, galaxies predicted by CDM extend to much lower masses, with steeper, singular profiles. This tension motivates cold, wavelike dark matter ($ψ$DM) composed of a non-relativistic Bose-Einstein condensate, so the uncertainty principle counters gravity below a Jeans scale. Here we achieve the first cosmological simulations of this quantum state at unprecedentedly high resolution capable of resolving dwarf galaxies, with only one free parameter, $\bf{m_B}$, the boson mass. We demonstrate the large scale structure of this $ψ$DM simulation is indistinguishable from CDM, as desired, but differs radically inside galaxies. Connected filaments and collapsed haloes form a large interference network, with gravitationally self-bound solitonic cores inside every galaxy surrounded by extended haloes of fluctuating density granules. These results allow us to determine $\bf{m_B=(8.1^{+1.6}_{-1.7})\times 10^{-23}~eV}$ using stellar phase-space distributions in dwarf spheroidal galaxies. Denser, more massive solitons are predicted for Milky Way sized galaxies, providing a substantial seed to help explain early spheroid formation. Suppression of small structures means the onset of galaxy formation for $ψ$DM is substantially delayed relative to CDM, appearing at $\bf{z\lesssim 13}$ in our simulations.
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