  In this paper, we investigate the simplest wormhole solution - the
Ellis-Bronnikov one - in the context of the Asymptotically Safe Gravity (ASG)
at the Planck scale. We work with three models, which employ Ricci scalar,
Kretschmann scalar, and squared Ricci tensor to improve the field equations by
turning the Newton constant into a running coupling constant. For all the
cases, we check the radial energy conditions of the wormhole solution and
compare them with those valid in General Relativity (GR). We verify that
asymptotic safety guarantees that the Ellis-Bronnikov wormhole can satisfy the
radial energy conditions at the throat radius, $r_0$, within an interval of
values of this latter. That is quite different from the result found in GR.
Following, we evaluate the effective radial state parameter, $\omega(r)$, at
$r_0$, showing that the quantum gravitational effects modify Einstein's field
equations in such a way that it is necessary a very exotic source of matter to
generate the wormhole spacetime -- phantom or quintessence-like. That occurs
within some ranges of throat radii, even though the energy conditions are or
not violated there. Finally, we find that, although at $r_0$ we have a
quintessence-like matter, on growing of $r$ we necessarily come across
phantom-like regions. We speculate if such a phantom fluid must always be
present in wormholes in the ASG context or even in more general quantum gravity
scenarios.
