Program: GN-2021B-Q-212

High-redshift star-forming galaxies (SFGs) are often associated with the pristine gas accretion from cosmological streams. Their gas-rich disk is suggested to be gravitationally unstable, leading to the fragmentation and formation of star-forming clumps. In this framework, clumpy SFGs should have lower metallicities compared to regular SFGs. The proposed study is a follow-up to our previous proposals to measure the fundamental metallicity relation of clumpy and regular SFGs. We propose to use GNIRS to observe 21 SFGs at z ~ 0.8, and trace their gas-phase metallicity. A combined sample size of 32 SFGs will allow us to test whether there is a metallicity offset of at least 0.15 dex between the two populations. Given the ubiquity of clumpy SFGs toward high redshifts, this study will try to clearly link the changing mode of star formation to a physical process such as the rapid accretion of pristine gas.