  The galaxy system around NGC4490 was recently highlighted to display a
flattened, kinematically correlated structure reminiscent of satellite galaxy
planes around other hosts. Since known satellite planes are in tension with
$\Lambda$CDM expectations from cosmological simulations, we quantitatively
assess for the first time the tension posed by the NGC4490 system. We measure
the on-sky flattening as the major-to-minor axis ratio b/a of the satellite
distribution and their line-of-sight kinematic correlation. Analogs are
selected in the IllustrisTNG-50 simulation and their flattening and correlation
are similarly measured. We confirm the strong kinematic coherence of all 12
observed objects with available line-of-sight velocities (of 14 in total): the
northern ones approach and the southern ones recede relative to the host. The
spatial distribution of all 14 objects is substantially flattened with b/a=0.38
(0.26 considering only the 12 objects with velocities). Such extreme
arrangements are rare in the simulation at 0.21-0.35%. This would drop further
if at least one of the two satellite objects without velocities is confirmed to
follow the kinematic trend, and would become zero if both are rejected as
non-members. We also identify a likely galaxy pair in the observed system, and
find a similar pair in the best-matching simulated analog. Our findings
establish NGC4490 as another strong example of a satellite plane in the Local
Volume. This emphasizes that planes of satellites are a more general issue
faced by $\Lambda$CDM also beyond the Local Group. The tension with typical
systems in simulations suggests that the observed one requires a specific
formation scenario, potentially connected to the larger-scale galaxy alignment
in its vicinity. The presence of galaxy pairs in the observed and a simulated
system hints at the importance such groupings may have to understand satellite
planes.
