  If modified gravity holds, but the weak lensing analysis is done in the
standard way, one finds that dark matter halos have peculiar shapes, not
following the standard Navarro-Frenk-White profiles, and are fully predictable
from the distribution of baryons. Here we study in detail the distribution of
the apparent dark matter around point masses, which approximate galaxies and
galaxy clusters, and their pairs for the QUMOND MOND gravity, taking an
external gravitational acceleration $g_e$ into account. At large radii, the
apparent halo of a point mass $M$ is shifted against the direction of the
external field. When averaged over all lines-of-sight, the halo has a hollow
center, and denoting the by $a_0$ the MOND acceleration constant, its density
behaves like $\rho(r)=\sqrt{Ma_0/G}/(4\pi r^2)$ between the galacticentric
radii $\sqrt{GM/a_0}$ and $\sqrt{GMa_0}/g_e$, and like $\rho\propto
r^{-7}G^2M^3a_0^3/g_e^5$ further away. Between a pair of point masses, there is
a region of a negative apparent dark matter density, whose mass can exceed the
baryonic mass of the system. The density of the combined dark matter halo is
not a sum of the densities of the halos of the individual points. The density
has a singularity near the zero-acceleration point, but remains finite in
projection. We compute maps of the surface density and the lensing shear for
several configurations of the problem, and derive formulas to scale them to
further configurations. In general, for a large subset of MOND theories in
their weak field regime, for any configuration of the baryonic mass $M$ with
the characteristic size of $d$, the total lensing density scales as
$\rho({\vec{x}})=\sqrt{Ma_0/G}d^{-2}f\left(\vec{\alpha},\vec{x}/d,g_ed/\sqrt{GMa_0}\right)$,
where the vector $\vec{\alpha}$ describes the geometry of the system.
Distinguishing between QUMOND and cold dark matter seems possible with the
existing instruments.
