  With recent advancements in observing supermassive black holes with the Event
Horizon Telescope, there has been persistent exploration into what the images
can reveal about fundamental physics, including space-time geometries and
astrophysical emission sources. Inspired by Penrose's aberration formula for a
rigid sphere, which clarified that increased speed does not flatten the
appearance of the sphere, we extend the studies to the behavior of the images
of accretion emissions. This paper examines the impact of aberration effects on
the images of a thin accretion disk around Kerr-de Sitter black holes for
finite distant observers, specifically focusing on the primary, secondary, and
$n=2$ images. We employ the analytical ray-tracing scenario and extend the
astrometric approach to investigate the images in the presence of aberration.
This study is non-trivial because we do not assume a specific form of the
aberration formula, instead, all aberration effects emerge from a
coordinate-independent and tetrad-independent framework referred to as the
astrometric approach. Our study finds that the shapes of the lower-order images
get highly distorted for finite observers in motion, and the shapes and sizes
of primary images are more sensitive to aberration than those of the $n=2$
images. This finding suggests that the primary images could theoretically be
distinguished from the shadow based on their distinctive variations.
