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One of the aims of Aether Scalar Tensor Theory (AeST) is to reproduce thesuccesses of Modified Newtonian Dynamics (MOND) on galactic scales. Indeed, thequasi-static limit of AeST can achieve precisely this, assuming that the vectorfield $\vec{A}$ vanishes. However, this assumption of a vanishing vector fieldis not always justified. Here, we show how to correctly take into account thevector field and find that the quasi-static limit depends on a model parameter$m_\times$. In the limit $m_\times \to 0$, one recovers the quasi-static limitwith a vanishing vector field. In particular, one finds a two-field version ofMOND. In the opposite limit, $m_\times \to \infty$, one finds a single-fieldversion of MOND. We show that, in practice, much of the phenomenology of thequasi-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.

The Two Quasi-Static Limits of Aether Scalar Tensor Theory