The existence of star-to-star light-element abundance variations in massive Galactic and extragalactic star clusters has fairly recently superseded the traditional paradigm of individual clusters hosting stars with the same age, and uniform chemical composition. Several scenarios have been put forward to explain the origin of this multiple stellar population phenomenon, but so far all have failed to reproduce the whole range of key observations. Complementary to high-resolution spectroscopy, which has first revealed and characterized chemically the presence of multiple populations in Galactic globular clusters, photometry has been instrumental in investigating this phenomenon in much larger samples of stars—adding a number of crucial observational constraints and correlations with global cluster properties—and in the discovery and characterization of multiple populations also in Magellanic Clouds’ intermediate-age clusters. The purpose of this review is to present the theoretical underpinning and application of the photometric techniques devised to identify and study multiple populations in resolved star clusters. These methods have played and continue to play a crucial role in advancing our knowledge of the cluster multiple population phenomenon, and promise to extend the scope of these investigations to resolved clusters even beyond the Local Group, with the launch of the James Webb Space Telescope.

最近，巨大的银河系和河外星团中存在的恒星间轻元素丰度变化已经取代了拥有相同年龄和均匀化学成分的恒星的单个星团的传统范式。人们提出了几种设想来解释这种多恒星群体现象的起源，但到目前为止，所有设想都未能重现关键观测的全部范围。高分辨率光谱学首次揭示并以化学方式表征了银河系球状星团中多个星团的存在，光度测量学在研究更大的恒星样本中的这种现象方面发挥了重要作用，增加了许多关键的观测限制以及与全球的相关性。星团特性——以及麦哲伦星云中龄星团中多个种群的发现和表征。本综述的目的是介绍光度测量技术的理论基础和应用，该技术旨在识别和研究已解析星团中的多个星团。这些方法在推进我们对星团多重种群现象的了解方面发挥了并将继续发挥关键作用，并有望随着詹姆斯·韦伯太空望远镜的发射，将这些研究的范围扩大到已解决的星团，甚至超出本地群。