  Using a large redshift survey covering 95 square degrees, we demonstrate that
the infall region of Abell 2199 contains Abell 2197, one or two X-ray emitting
groups, and up to five additional groups identified in redshift surveys. Our
survey shows that the X-ray emitting systems, located at projected radii of
$1.^\circ4, 1.^\circ9$, and $5.^\circ1$ (2.2, 3.1, and $8.0 h^{-1}$Mpc), are
connected kinematically to A2199. A2197 is itself an optically rich cluster;
its weak X-ray emission suggests that it is much less massive than A2199. The
absence of a sharp peak in the infall pattern at the position of A2197 supports
this hypothesis. The outermost group is well outside the virial region of A2199
and it distorts the infall pattern in redshift space. The two X-ray emitting
groups are roughly colinear, suggesting the existence of an extended ($8.0
h^{-1}$Mpc) filament. The identification of these infalling groups provides
direct support of hierarchical structure formation; studies of these systems
will provide insights into structure evolution. Groups in the infall regions of
nearby clusters may offer a unique probe of the physics of the warm/hot ionized
medium (WHIM) which is difficult to observe directly with current instruments.
