  We study the shadows cast by near-extremal Kerr-MOG black holes for different
values of the parameter in modified gravity (MOG). In particular, we consider
an isotropic emitter orbiting near such black holes and analytically compute
the positions, fluxes and redshift factors of their images. The size of the
shadow decreases when the modified parameter is increased. For each shadow, the
images of the emitter appear on a special part of the shadow which has a rich
structure. The primary image and secondary images are similar to those produced
for the near-extremal (high spin) Kerr black hole, but the near-extremal
Kerr-MOG black hole can have a spin ($\hat{J}/M^2_{\alpha}$) which is finitely
lower than 1. When the modified parameter is varied, the typical positions of
the corresponding images do not change, nor does the typical redshift factor
associated with the primary image. However, another typical redshift factor
associated with the secondary image increases when the modified parameter is
increased. We also find that the fluxes increase in that case. These images
appear periodically with period greater than that of Kerr. This provides an
alternative signature away from the Kerr case which may be tested by the Event
Horizon Telescope.
