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The Galactic disk exhibits complex chemical and dynamical substructurethought to be induced by the bar, spiral arms, and satellites. Here, we explorethe chemical signatures of bar resonances in action and velocity space andcharacterize the differences between the signatures of corotation andhigher-order resonances using test particle simulations. Thanks to recentsurveys, we now have large datasets containing metallicities and kinematics ofstars outside the solar neighborhood. We compare the simulations to theobservational data from Gaia EDR3 and LAMOST DR5 and find weak evidence for aslow bar with the "hat" moving group ($250~\text{km/s} \lesssim v_\phi \lesssim270~\text{km/s}$) associated with its outer Lindblad resonance and "Hercules"($170~\textrm{km/s} \lesssim v_\phi \lesssim 195~\text{km/s}$) with corotation.While constraints from current data are limited by their spatial footprint,stars closer in azimuth than the Sun to the bar's minor axis show much strongersignatures of the bar's outer Lindblad and corotation resonances in testparticle simulations. Future datasets with greater azimuthal coverage,including the final Gaia data release, will allow reliable chemodynamicalidentification of bar resonances.

Chemodynamical signatures of bar resonances in the Galactic disk: current data and future prospects