AI 中文总结
研究针对当前观测与标准冷暗物质范式的矛盾，通过分析宇宙网丝状结构周围星系分布周期性寻找模糊暗物质特征，将丝状轮廓与特定模型比较，利用斯隆数字巡天样本分析，确定了与观测矛盾的参数空间区域，能测试丝状暗物质结构模型。
AI 中文摘要
当前观测显示与标准冷暗物质范式存在持续矛盾，引发能否仅由重子物理解释或需替代暗物质模型的问题。模糊（或波）暗物质是一种替代方案，其由质量\(m \sim 10^{-22}\) eV且德布罗意波长在kpc到Mpc尺度的超轻粒子组成，可能在宇宙网周围的非线性结构中产生大规模干涉图案。本文通过研究宇宙网丝状结构周围星系分布的周期性来寻找这些干涉条纹的可能特征。为展示方法，将丝状结构轮廓与包含\(A\cos(2\pi d/ \lambda)\)形式周期成分的简单模型比较，利用斯隆数字巡天主星系样本分析了4394条丝状结构。发现大部分参数空间在\(2\sigma\)水平与观测一致，确定了与观测矛盾的参数空间区域，能在\(3\sigma\)水平排除\(0.2\,\text{Mpc}\,\lesssim \lambda_0 \lesssim 2\,\text{Mpc}\)时\(A > 0.16 \lambda_0 + 0.18\)的值，证明该方法可测试丝状暗物质结构模型。
英文摘要
Current observations reveal persistent tensions with the standard cold dark matter paradigm, raising the question of whether these can be explained by baryonic physics alone or require alternative dark matter models. One such alternative is fuzzy (or wave) dark matter, consisting of ultralight particles with mass $m \sim 10^{-22}$ eV and de Broglie wavelengths on kpc to Mpc scales, which may give rise to large--scale interference patterns in non-linear structures around the cosmic web, such as filaments and clusters. In this work, we search for possible signatures of these interference fringes by investigating periodicities in the distribution of galaxies around cosmic web filaments. To demonstrate our methodology, we compare the filament profiles to a simple model that includes a periodic component of the form $A\cos(2πd/ λ)$, where $A$ is the maximum density contrast (amplitude) of the periodic component, with wavelength $λ=λ_0 \cosθ$ for some face-on wavelength $λ_0$ inclined at an angle $θ$ to the line of sight. Exploiting the large Sloan Digital Sky Survey (SDSS) Main Galaxy Sample, we analyse a sample of 4,394 filaments from the Tempel et al. filament catalogue, each containing at least 10 member galaxies. We find a vast portion of the parameter space is consistent with the observations at the $2σ$ level, including all models with $A = 0$ (no periodicity). We identify a region of the parameter space in tension with the observations, allowing us to exclude values of $A > 0.16 λ_0 + 0.18$ for $0.2\,\text{Mpc}\,\lesssim λ_0 \lesssim 2\,\text{Mpc}$ at the $3σ$ level, demonstrating the ability to test models of filament dark matter structure using this methodology.
Comments12 pages, 5 figures, Accepted for publication in MNRAS
