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Recent observations suggest that the first stages of planet formation likelytake place in the Class 0/I phase of Young Stellar Object evolution, when thestar and the disk are still embedded in an infalling envelope. In this study weperform grain coagulation calculations to investigate the very first stage ofplanet formation, the collisional growth of dust grains, in Class 0/I disks. Wefind that the slow increase in grain mass by high-velocity collision with muchsmaller grains ("sweep-up") allows $\sim 50 M_\oplus$ of grains to grow wellbeyond the fragmentation barrier into $\sim$kg pebbles by the end of Class 0/I(0.1 Myr). We analyze the linear growth and saturation of sweep-up tounderstand our results quantitatively, and test whether the sweep-up outcome issensitive to disk parameters and details of the grain coagulation model. Thesweep-up pebble population could be important for planet formation, becausethey are less well-coupled to the gas (compared to the main population belowthe fragmentation barrier) and therefore more favorable to known mechanisms ofdust clump formation (which initiate planetesimal formation). It also containsenough mass to form all planet cores, based on observational estimates of theplanet mass budget. Our findings motivate future studies of grain growth andplanetesimal formation in Class 0/I disks, including the subsequent evolutionof this sweep-up population.

Revisiting collisional dust growth in Class 0/I protostellar disks: Sweep-up can convert a few $10 M_\oplus$ of dust into kg pebbles in 0.1 Myr