What stellar streams reveal about star clusters in the earliest galaxies
Recent observations have discovered compact star-forming regions at z > 4 that are likely proto-globular clusters (GCs), contributing over 50% of total star formation in the earliest galaxies. However, present-day GCs account for only ~0.1% of stellar mass in local galaxies. This striking contrast highlights the important role of tidal dissolution in reshaping cluster masses, yet this process remains poorly constrained. To address this challenge, we have developed pioneering numerical frameworks to measure cluster mass-loss rates driven by tidal dissolution using stellar streams as a probe. These frameworks are specifically designed for ongoing/upcoming next-generation surveys including Roman, Rubin, and DESI, whose depth and coverage will, for the first time, allow direct tests of tidal dissolution theories. Taking advantage of these surveys, we aim to establish parametric prescriptions for the tidal dissolution process, and ultimately build a unified physical theory of cluster evolution from the Cosmic Dawn to the present day.
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