Understanding galaxy growth requires studying the interplay between gas dynamics, star formation, and the environment. During the cosmic noon, a crucial shift in gas accretion mode is expected to occur, motivating us to explore the relationship between gas properties and star formation. Our target is HS1700+64, a proto-cluster with prominent filamentary structures in a vigorous assembling phase. This offers an ideal opportunity for us to know how the HI gas is distributed along the structures and how the star formation activities are influenced by the surrounding environments in the early phase of cluster assembly. Moreover, we aim to understand how the gas accretion and star formation are mutually linked. To answer these questions, we propose deeper and wider narrow-band imaging of this young proto-cluster at z=2.3 to identify its extended structures to the unexplored side of the two known linear filaments. Moreover, we go deeper to reach the uniform depth so that we can make a fair comparison with other proto-clusters at similar redshifts, spanning from high-mass to low-mass galaxies (>108.5 M⊙). This comprehensive approach will unveil the complex interplays among cluster scale assembly, gas accretion along the structures and the star formation in galaxies embedded in the structures.
This document was translated from LATEX by HEVEA.