标题： 椭圆星系在深空JWST图像中“疯狂”的平滑丝状起源 显示英文标题

标题： A smooth filament origin for prolate galaxies "going bananas" in deep JWST images

摘要： 我们比较了在深度JWST调查中报告的超出z$>$3的丰富扁长星系，与详细流体模拟中三种主要暗物质候选者：冷暗物质（CDM）、波/模糊暗物质（$\psi$DM）和温暗物质（WDM）中年轻星系的预测{\it 恒星}外观。我们发现观测到的星系图像与$\psi$DM和WDM在最初$\simeq$500Myr期间预测的年轻星系的拉长恒星外观非常相似，此时物质从长而平滑的丝状结构中持续吸积。WDM和$\psi$DM的暗物质晕也具有明显的扁长延伸，类似于恒星，表明存在共享的高度三轴平衡。这与CDM不同，CDM中的早期恒星形态主要是由碎片化的丝状结构频繁合并形成的球形，导致三轴性较小。 定量上，JWST观测到的长椭星系的过剩与1.4KeV粒子质量的WDM和$2.5\times 10^{-22}$eV的$\psi$DM很好地匹配。 对于CDM，通常预测每个星系的晕半径内会有多个可见的子晕轨道运行，而WDM和$\psi$DM的合并最初是罕见的。 我们还通过模拟验证了$\psi$DM可以通过核心的形式与WDM区分开来，WDM的核心被预测为平滑且居中的，而$\psi$DM的核心则是一个密集的孤子，由恒星追踪，并在模拟中由于随机波扰动而明显偏离星系中心。 我们强调，JWST可能能够探测到缺乏星系的长平滑丝状结构，这些结构由恒星和气体追踪，共动长度为150kpc，在z$\simeq$10时预测，具体取决于$\psi$DM或WDM的粒子质量。 显示英文摘要

摘要： We compare the abundant prolate shaped galaxies reported beyond z$>$3 in deep JWST surveys, with the predicted {\it stellar} appearance of young galaxies in detailed hydro-simulations of three main dark matter contenders: Cold (CDM), Wave/Fuzzy ($\psi$DM) and Warm Dark Matter (WDM). We find the observed galaxy images closely resemble the elongated stellar appearance of young galaxies predicted for both $\psi$DM and WDM, during the first $\simeq$ 500Myr while material steadily accretes from long, smooth filaments. The dark mater halos of WDM and $\psi$DM also have pronounced, prolate elongation similar to the stars, indicating a shared, highly triaxial equilibrium. This is unlike CDM where the early stellar morphology is mainly spheroidal formed from fragmented filaments with frequent merging, resulting in modest triaxiality. Quantitatively, the excess of prolate galaxies observed by JWST matches well WDM and $\psi$DM for particle masses of 1.4KeV and $2.5\times 10^{-22}$ eV respectively. For CDM, several visible subhalos are typically predicted to orbit within the virial radius of each galaxy from subhalo accretion, whereas merging is initially rare for WDM and $\psi$DM. We also verify with our simulations that $\psi$DM may be distinguished from WDM by the form of the core, which is predicted to be smooth and centered for WDM, but is a dense soliton for $\psi$DM traced by stars and measurably offset from the galaxy center by random wave perturbations in the simulations. We emphasise that long smooth filaments absent of galaxies may prove detectable with JWST, traced by stars and gas with comoving lengths of 150kpc predicted at z$\simeq$10, depending on the particle mass of $\psi$DM or WDM.