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Using Gaia DR3 data and the wavelet transformation technique, we study thesubstructures of the Hercules moving group (HMG): Hercules 1 (H1) and Hercules2 (H2). Spectroscopic survey data from LAMOST, APOGEE, and GALAH are used toobtain metallicities and ages of stars belonging to the HMG. Our analysis leadsto several key findings as follows: ($a$) the HMG is on average richer inmetallicity than the Galactic disk, with H2 being metal richer than H1; ($b$)the HMG likely has a radial metallicity gradient distinct from that of thedisk; ($c$) the HMG is on average older than the disk, with H2 being older thanH1; ($d$) the HMG likely has a radial age gradient distinct from that of thedisk; and ($e$) the metallicity and age distributions of the HMG depend mainlyon the Galactic radius but show no dependence on the azimuthal velocity. Takenall together, we conclude that the HMG is composed primarily of starsundergoing radial migration. We suggest that the HMG is associated with ahigher-order dynamical resonance of the bar of the Galaxy.

On the Migration Origin of the Hercules Moving Group with GAIA, LAMOST, APOGEE, and GALAH Surveys