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The distribution of moving groups in the solar neighborhood has been used toconstrain dynamical properties of the Milky Way for decades. Unfortunately, theunique bimodality between the main mode (Hyades, Pleiades, Coma Berenices, andSirius) and Hercules can be explained by two different bar models -- via theouter Lindblad resonance of a short, fast bar, or via the corotation resonanceof a long, slow bar. In this work, we break this degeneracy by using Gaia DR3to explore the variation of Hercules across Galactic azimuth. We find thatHercules increases in $V_\phi$ and becomes stronger as we move towards theminor axis of the bar, and decreases in $V_\phi$ and becomes weaker as we movetowards the major axis of the bar. This is in direct agreement with theoreticalpredictions of a long, slow bar model in which Hercules is formed by thecorotation resonance with stars orbiting the bar's L4/L5 Lagrange points.

Constraining The Milky Way Bar Length using Hercules and Gaia DR3