On the nature of the ring-like structure in the outer Galactic disk

Abstract

We examine the tidal disruption of satellite galaxies in a cosmological simulation of the formation of a disk galaxy in the $Λ$CDM scenario. We find that the disruption of satellite galaxies in orbits roughly coplanar with the disk leads naturally to the formation of ring-like stellar structures similar to that recently discovered in the outer disk of the Milky Way. Two interpretations appear plausible in this context. One is that the ring is a transitory, localized radial density enhancement reflecting the apocenter of particles stripped from a satellite during a recent pericentric passage (a ``tidal arc'' reminiscent of the tidal arms seen in disk galaxy mergers). In the second scenario, the ring is analogous to the ``shells'' found around some elliptical galaxies, and would result from a minor merger that took place several Gyr ago. The two interpretations differ in several ways. Tidal arcs are expected to span a limited longitude range; may carry a substantial fraction of the original mass of the satellite; should exhibit a significant velocity gradient with Galactic longitude; and are in all likelihood asymmetric above and below the plane of the disk. Shells, on the other hand, may comprise at most a small fraction of the original mass of the satellite and, due to their more relaxed state, ought to be symmetric above and below the plane, with no discernible velocity gradients across the structure. If confirmed as a tidal feature, the ring discovered by SDSS in the outer Galactic disk would strengthen the view--supported by numerical simulations--that minor mergers have played a significant role building up not only the stellar halo, but also the disk components of the Galaxy.