发表机构
Donostia International Physics Center, DIPC; Department of Theoretical Physics, University of the Basque Country UPV/EHU; Ikerbasque, Basque Foundation for Science; Department of Physics, National Taiwan University; National Center for Theoretical Sciences, National Taiwan University; Department of Physics, The University of Hong Kong; The Hong Kong Institute for Astronomy and Astrophysics, The University of Hong Kong; Institute of Astronomy and Particle Physics, University of Innsbruck; ASIAA; Center for Frontier Science, Chiba University; Department of Physics, Graduate School of Science, Chiba University（多诺西亚国际物理中心; 巴斯克大学理论物理系; 伊克拉巴斯科，巴斯克科学基金会; 台湾大学物理系; 台湾大学国家理论科学中心; 香港大学物理系; 香港大学香港天体物理研究所; 因斯布鲁克大学天文与粒子物理研究所; 中央研究院天文及天文物理研究所; 千叶大学前沿科学中心; 千叶大学理学研究科物理系）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本文提出波暗物质内部恒星扩散机制解释弥散星系序列，通过孤子散射使恒星轨道膨胀，并预测轻玻色子质量，回溯演化过程。
AI 中文摘要
欧几里得卫星在低表面亮度下的广泛成像揭示，大多数邻近星系是外观弥散的球状体，其恒星半径随光度在三个数量级上单调增加。我们认为，这种弥散星系序列源于波暗物质（$\psi$DM）引起的内部恒星扩散，因为波能量随时间转移到恒星轨道上。特别是，孤子随机运动将中心恒星散射到径向轨道上，每次穿过中心时这些轨道都会增强，从而缓慢地“膨胀”恒星轮廓。大质量星系内的加热更强，因为$\psi$DM涨落更强且更频繁，重现了弥散星系序列，并且还解释了沿该序列从超暗矮星系到矮椭球星系和超弥散星系的速度弥散度上升，这有利于轻玻色子$m_\psi=2.88^{+0.14}_{-0.13}\times10^{-22}$eV。回溯这一扩散过程，我们预测弥散星系（包括球状星团）的恒星含量形成于中心附近，正如$\psi$DM模拟所预期的那样，在那里气体在致密孤子内有效冷却。这种从紧凑起源演变为今天外观弥散的球状星系的预测$\psi$DM演化，现在可以从JWST到欧几里得全面绘制。
英文摘要
Extensive Euclid satellite imaging at low surface brightness has revealed that most nearby galaxies are diffuse-looking spheroids, where the stellar radius increases for over three decades in luminosity. We argue this Diffuse Galaxy sequence results from internal stellar diffusion by Wave Dark Matter ($ψ$DM), as wave energy is transferred to star orbits over time. In particular, the soliton random motion scatters central stars onto radial orbits that become enhanced with each passage through the centre, slowly ``puffing up" the stellar profile. Heating is greater within massive galaxies as $ψ$DM fluctuations are stronger and more frequent, reproducing both the Diffuse Galaxy sequence and the rising velocity dispersion along the sequence, from Ultra-Faint to Dwarf Spheroidal and Ultra Diffuse galaxies, favouring a light boson, $m_ψ=2.88^{+0.14}_{-0.13}\times10^{-22}$eV. Winding back this diffusion, we predict the stellar content of Diffuse Galaxies, including globular clusters, formed near the centre, as anticipated by $ψ$DM simulations, where gas cools efficiently within the dense soliton. This predicted $ψ$DM evolution from compact beginnings towards diffuse spheroidal galaxies today can now be fully charted from JWST to Euclid.
Commentssimulation of radial anisotropy now included, author list and acknowledgement updated
