The advent of new deep＋ wide photometric lensing surveys will open up the possibility of direct measurements of the dark matter halos of dwarf galaxies. The HSC wide survey will be the first with the statistical capability of measuring the lensing signal with high signal-to-noise at $log\left(M^{\ast }\right)\sim 8$. At this same mass scale, The Rubin Observatory LSST will have the most overall constraining power with a predicted signal-to-noise for the galaxy–galaxy lensing signal around dwarfs of S/N$\sim$200. Roman and Rubin will have the greatest potential to push below the $log\left(M^{\ast }\right)=7$ mass scale thanks to the depth of their imaging data. Studies of the dark matter halos of dwarf galaxies at $z\sim$0.1 with gravitational lensing are soon within reach. However, further work will be required to develop optimized strategies for extracting dwarfs samples from these surveys, determining redshifts, and accurately measuring lensing on small radial scales. Dwarf lensing will be a new and powerful tool to constrain the halo masses and inner density slopes of dwarf galaxies and to distinguish between baryonic feedback and modified dark matter scenarios.

新的深＋宽光度透镜测量法的出现将为直接测量矮星系的暗物质晕提供了可能。HSC范围的调查将是第一个具有统计功能的测量功能，该功能可以在$日志（{\mathrm{中号}}^{\ast }）〜8$。在相同的质量尺度下，鲁宾天文台LSST将具有最全面的约束力，并且对信噪比矮星周围的星系-星系透镜信号具有预测的信噪比。$〜$200.罗马和鲁宾将有最大的潜力来推低 $日志（{\mathrm{中号}}^{\ast }）=7$得益于其成像数据的深度，可实现大规模生产。矮星系暗物质晕的研究$ž〜$带有重力透镜的0.1很快就可以达到。但是，还需要进一步的工作来开发优化的策略，以从这些调查中提取矮人样本，确定红移并在小径向尺度上准确地测量透镜。矮透镜化将是一种新的强大工具，可以限制矮星系的晕质量和内部密度斜率，并区分重子反馈和改良暗物质场景。