发表机构
Scuola Superiore Meridionale; Istituto Nazionale di Fisica Nucleare, Sez. di Napoli; Institute of Physics, University of Szczecin; Dipartimento di Fisica “E. Pancini”, Università degli Studi di Napoli “Federico II”; Dipartimento di Fisica e Astronomia “G. Galilei”, Università di Padova（南方高等学院; 意大利国家核物理研究所那不勒斯分部; 谢扎青大学物理研究所; 那不勒斯费德里科二世大学E.潘奇尼物理系; 帕多瓦大学G.伽利略物理与天文系）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究利用积分场恒星运动学首次约束旋转支持超扩散星系UDG-1和LSB-6的暗物质分布，测试多种暗物质模型，发现两者暗物质含量与典型矮星系相当，支持膨胀矮星系起源。
AI 中文摘要
我们研究了LEWIS样本中两个星系的内部结构：超扩散星系UDG-1和扩展矮星系LSB-6。两者均表现出连贯的恒星旋转，同时伴有不可忽略的随机运动分量，且没有持续扰动的迹象。这是首次尝试通过积分场恒星运动学来约束旋转支持的超扩散星系的动力学和暗物质物理。我们将这些星系建模为嵌入球形暗物质晕中的、具有典型矮星系厚度的恒星椭球体，推导出二维速度场，并在贝叶斯框架下与观测进行比较。除了冷暗物质，我们还测试了模糊暗物质、自相互作用暗物质和非最小耦合暗物质。数据倾向于UDG-1中存在尖点晕，而LSB-6中则为无尖点晕。所有替代模型仍然可行，尽管当前数据无法最终区分它们。对于模糊暗物质，我们获得了相互一致的玻色子质量，UDG-1为$m_\alpha = 4.7^{+1.8}_{-1.1} \times 10^{-22}$ eV，LSB-6为$m_\alpha = 6.3^{+0.4}_{-0.4} \times 10^{-22}$ eV。对于自相互作用暗物质，LSB-6给出了速度加权截面的稳健约束，$\langle \sigma v\rangle/m = 14.3^{+2.0}_{-1.9}$ cm$^2$ km g$^{-1}$ s$^{-1}$。对于非最小耦合暗物质，我们推导出耦合长度的上限，暗示与$\Lambda$CDM的偏差很小。无论采用何种模型，这两个星系的暗物质含量都与具有相似恒星质量的典型矮星系晕相当。结合恒星种群分析和球状星团信息，这些结果支持UDG-1和LSB-6起源于膨胀矮星系的场景。这项工作是一个系列中的第一篇，该系列利用极低表面亮度星系的运动学数据来检验基础物理，从暗物质到修正引力理论。
英文摘要
We investigate the internal structure of two galaxies from the LEWIS sample: the ultra-diffuse galaxy UDG-1 and the extended dwarf LSB-6. Both show coherent stellar rotation combined with a non-negligible fraction of random motion, with no signs of ongoing disturbance. This is the first attempt to constrain the dynamics and dark matter physics of rotation-supported UDGs through integral-field stellar kinematics. We model the galaxies as stellar spheroids with typical dwarf-like thickness embedded in spherical dark matter halos, deriving two-dimensional velocity fields that we compare with the observations in a Bayesian framework. Besides cold dark matter, we test fuzzy, self-interacting, and non-minimally coupled dark matter. The data prefer a cuspy halo in UDG-1 and a cuspless one in LSB-6. All the alternative models remain viable, although current data cannot conclusively discriminate among them. For fuzzy dark matter we obtain mutually consistent boson masses, $m_α= 4.7^{+1.8}_{-1.1} \times 10^{-22}$ eV for UDG-1 and $m_α= 6.3^{+0.4}_{-0.4} \times 10^{-22}$ eV for LSB-6. For self-interacting dark matter, LSB-6 yields a robust constraint on the velocity-weighted cross section, $\langle σv\rangle/m = 14.3^{+2.0}_{-1.9}$ cm$^2$ km g$^{-1}$ s$^{-1}$. For non-minimally coupled dark matter we derive upper bounds on the coupling length, implying marginal deviations from $Λ$CDM. Regardless of the model, both galaxies exhibit a dark matter content comparable with halos of typical dwarf galaxies with similar stellar masses. Together with stellar population analyses and globular cluster information, these results support a scenario in which UDG-1 and LSB-6 originate from puffed-up dwarfs. This work is the first in a series exploiting kinematic data of extremely low-surface-brightness galaxies to test fundamental physics, from dark matter to modified theories of gravity.
Comments26 pages, 13 figures, 3 tables. Accepted for publication on A&A
