  HR 6819 was recently claimed to be a hierarchical triple system of a Be star
in a wide orbit around an inner binary system of a black hole (BH) and a B III
type star. We argue that this system is unlikely to be a hierarchical triple
due to three reasons: (i) Given that this system is discovered in a magnitude
limited Bright Star Catalog, the expected number of such systems in the Milky
Way amounts to about $10^4$ while the estimate for the MW budget for such
systems is between $10^2-10^3$ systems under generous assumptions. Such a large
gap cannot be reconciled as it would otherwise likely overflow the MW budget
for BHs; (ii) The dynamical stability of this system sets lower bounds on the
orbital separation of the outer Be star, while it not being resolved by Gaia
places an upper limit on its projected sky separation. We show that these two
constraints would imply a narrow range for the outer orbit without resorting to
geometrical fine-tuning; (iii) The triple system should have survived the
stellar evolution prior to the formation of the BH in the inner binary. We
perform numerical simulations starting with conservative initial conditions of
this system and show that a small parameter space for BH progenitor star's mass
loss, BH natal kicks, and initial orbital separation can reproduce HR 6819.
Therefore, we propose this system is a chance superposition of a Be star with a
binary.
