  One of the aims of Aether Scalar Tensor Theory (AeST) is to reproduce the
successes of Modified Newtonian Dynamics (MOND) on galactic scales. Indeed, the
quasi-static limit of AeST achieves precisely this, assuming that the vector
field $\vec{A}$ vanishes and that the so-called ghost condensate can be
neglected. The effects of the ghost condensate were investigated in detail in
previous studies. Here, we focus on the assumption of a vanishing vector field.
We argue that this assumption is not always justified and show how to correctly
take into account the vector field, finding that the quasi-static limit depends
on a model parameter $m_\times$. In the limit $m_\times \to 0$, one recovers
the quasi-static limit with a vanishing vector field. In particular, one finds
a two-field version of MOND. In the opposite limit, $m_\times \to \infty$, one
finds a single-field version of MOND. We show that, in practice, much of the
phenomenology of the quasi-static limit depends only very little on the value
of $m_\times$. Still, for some observational tests, such as those involving
wide binaries, $m_\times$ has percent-level effects that may be important.
