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The origins of the Galilean satellites - namely Io, Europa, Ganymede, andCallisto - is not fully understood yet. Here we use N-body numericalsimulations to study the formation of Galilean satellites in a gaseouscircumplanetary disk around Jupiter. Our model includes the effects of pebbleaccretion, gas-driven migration, and gas tidal damping and drag.Satellitesimals in our simulations first grow via pebble accretion and start tomigrate inwards. When they reach the trap at the disk inner edge, scatteringevents and collisions take place promoting additional growth. Growingsatellites eventually reach a multi-resonant configuration anchored at the diskinner edge. Our best match to the masses of the Galilean satellites is producedin simulations where the integrated pebble flux is 1e-3 MJ. These simulationstypically produce between 3 and 5 satellites. In our best analogues, adjacentsatellite pairs are all locked in 2:1 mean motion resonances. However, theyhave also moderately eccentric orbits (0.1), unlike the current realsatellites. We propose that the Galilean satellites system is a primordialresonant chain, similar to exoplanet systems as TRAPPIST-1, Kepler-223, andTOI-178. Callisto was probably in resonance with Ganymede in the past but leftthis configuration - without breaking the Laplacian resonance - via divergentmigration due to tidal planet-satellite interactions. These same effectsfurther damped the orbital eccentricities of these satellites down to theircurrent values (0.001). Our results support the hypothesis that Io and Europawere born with water-ice rich compositions and lost all/most of their waterafterwards. Firmer constraints on the primordial compositions of the Galileansatellites are crucial to distinguish formation models.

Building the Galilean moons system via pebble accretion and migration: A primordial resonant chain