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Using GALAH survey data of nearby stars, we look at how structure in theplanar (u,v) velocity distribution depends on metallicity and on viewingdirection within the Galaxy. In nearby stars, with distance d < 1 kpc, theHercules stream is most strongly seen in higher metallicity stars [Fe/H] > 0.2.The Hercules stream peak v value depends on viewed galactic longitude, which weinterpret as due to the gap between the stellar stream and more circular orbitsbeing associated with a specific angular momentum value of about 1640 km/s kpc.The association of the gap with a particular angular momentum value supports abar resonant model for the Hercules stream.  Moving groups previously identified in Hipparcos observations are easiest tosee in stars nearer than 250 pc, and their visibility and peak velocities inthe velocity distributions depends on both viewing direction (galacticlongitude and hemisphere) and metallicity. We infer that there is finestructure in local velocity distributions that varies over distances of a fewhundred pc in the Galaxy.

The GALAH Survey: Stellar streams and how stellar velocity distributions vary with Galactic longitude, hemisphere and metallicity