标题： 暗物质因“龙弧”中的偏斜微透镜而区别开 显示英文标题

标题： Dark Matter distinguished by skewed microlensing in the "Dragon Arc"

摘要： 近期由 JWST 和 HST 发现的微透镜恒星沿着 A370 的“龙弧”部分紧密追踪临界曲线的所有截面。这些暂现源比$m_{AB}>26.5$暗弱，对应于渐近巨星支（AGB）恒星，并被用$\simeq 18M_\odot/pc^2$观测到的弥散星团中的恒星微透镜，或相当于投影暗物质密度的约$\simeq 1$%。大多数微透镜恒星出现在临界曲线的内边缘，沿一条宽度为$\simeq 4$千秒差距且偏移$-0.7\pm0.2$千秒差距的不对称带分布。一些偏移是可以预期的，因为最放大的图像应该在具有负奇偶性的临界曲线内边缘形成，但预测的位移较小，约为$\simeq -0.04$千秒差距，且预测检测的带宽较窄，为$\simeq 1.4$千秒差距。 添加类似CDM的暗晕$10^{6-8}M_\odot$会使带宽变宽，但检测方向偏向临界曲线的外边缘，与预期相反，在该处子晕会产生局部爱因斯坦环。 相反，“波暗物质”（作为玻色-爱因斯坦凝聚体$\psi$暗物质）固有的干涉会形成一条对负奇偶性检测有利的对称临界曲线带。 $\simeq 10$秒差距的德布罗意波长很好地匹配了观测到的$4$千帕秒微透镜带，并预测出相似于数据的\(-$\simeq -0.6$\)千帕秒的负偏度。 由此得出的对应玻色子质量为$\simeq 10^{-22}$电子伏特，当按动量比例缩放时，与矮星系核的估算值非常一致。 进一步的JWST成像可能通过简单地“连接”微透镜恒星之间来揭示临界曲线的模式，从而区分$\psi$暗物质的波状起伏和CDM亚晕。 显示英文摘要

摘要： Microlensed stars recently discovered by JWST & HST follow closely the winding critical curve of A370 along all sections of the ``Dragon Arc" traversed by the critical curve. These transients are fainter than $m_{AB}>26.5$, corresponding to the Asymptotic Giant Branch (AGB) and microlensed by diffuse cluster stars observed with $\simeq 18M_\odot/pc^2$, or about $\simeq 1$\% of the projected dark matter density. Most microlensed stars appear along the inner edge of the critical curve, following an asymmetric band of width $\simeq 4$kpc that is skewed by $-0.7\pm0.2$kpc. Some skewness is expected as the most magnified images should form along the inner edge of the critical curve with negative parity, but the predicted shift is small $\simeq -0.04$kpc and the band of predicted detections is narrow, $\simeq 1.4$kpc. Adding CDM-like dark halos of $10^{6-8}M_\odot$ broadens the band as desired but favours detections along the outer edge of the critical curve, in the wrong direction, where sub-halos generate local Einstein rings. Instead, the interference inherent to ``Wave Dark Matter" as a Bose-Einstein condensate ($\psi$DM) forms a symmetric band of critical curves that favours negative parity detections. A de Broglie wavelength of $\simeq 10$pc matches well the observed $4$kpc band of microlenses and predicts negative skewness $\simeq -0.6$kpc, similar to the data. The implied corresponding boson mass is $\simeq 10^{-22}$eV, in good agreement with estimates from dwarf galaxy cores when scaled by momentum. Further JWST imaging may reveal the pattern of critical curves by simply ``joining the dots" between microlensed stars, allowing wave corrugations of $\psi$DM to be distinguished from CDM sub-halos