  We study equilibrium configurations of a homogenous ball of matter in a
bootstrapped description of gravity which includes a gravitational
self-interaction term beyond the Newtonian coupling. Both matter density and
pressure are accounted for as sources of the gravitational potential for test
particles. Unlike the general relativistic case, no Buchdahl limit is found and
the pressure can in principle support a star of arbitrarily large compactness.
By defining the horizon as the location where the escape velocity of test
particles equals the speed of light, like in Newtonian gravity, we find a
minimum value of the compactness for which this occurs. The solutions for the
gravitational potential here found could effectively describe the interior of
macroscopic black holes in the quantum theory, as well as predict consequent
deviations from general relativity in the strong field regime of very compact
objects.
