A Number of Nearby Moving Groups may be Fragments of Dissolving Open
  Clusters
  We propose that fourteen co-moving groups of stars uncovered by Kounkel &
Covey (2019) may be related to known nearby moving groups and bridge those and
nearby open clusters with similar ages and space velocities. This indicates
that known nearby moving groups may be spatially much more extended than
previously though, and some of them might be parts of tidal tails around the
cores of known open clusters, reminiscent of those recently found around the
Hyades and a handful of other nearby clusters. For example, we find that both
the nearby Carina and Columba associations may be linked to Theia 208 from
Kounkel & Covey (2019) and together form parts of a large tidal tail around the
Platais 8 open cluster. The AB Doradus moving group and Theia 301 may form a
trailing tidal tail behind the Pleiades open cluster, with hints of a possible
leading tidal tail in Theia 369. We similarly find that IC 2391 and its tidal
tails identified by Meingast et al. (2021) may be extended by the nearby Argus
association and are possibly further extended by Theia 115. The nearby Octans
and Octans-Near associations, as well as Theia 94 and 95, may form a large
tidal tail leading the poorly studied Platais 5 open cluster candidate. While a
preliminary analysis of Gaia color-magnitude sequences hint that these
structures are plausibly related, more observational evidence is still required
to corroborate their consistent ages and space velocities. These observations
may change our current understanding of nearby moving groups and the different
pathways through which they can form. While some moving groups may have formed
loosely in extended star-formation events with rich spatial structure, others
may in fact correspond to the tidal tails of nearby open clusters.
