  The short-period AP Dor eclipsing binary's first in-depth and multiband
photometric solutions are presented. We made use of our eight nights of
ground-based at a southern hemisphere observatory, and twelve sectors of TESS
observations. We extracted eight and 1322 minima from our observations and
TESS, respectively. We suggested a new linear ephemeris based on the trend of
orbital period variations using the Markov chain Monte Carlo (MCMC) approach.
The PHysics Of Eclipsing BinariEs (PHOEBE) Python code and the MCMC approach
were used for the light curve analysis. This system did not require a starspot
for the light curve solutions. We calculated the absolute parameters of the
system using Gaia DR3 parallax method. The orbital angular momentum (J_0) of
the AP Dor indicates that this system is located in a region of contact
binaries. According to our results, this system is an overcontact binary system
with a mass ratio of 0.584, a fillout factor of 48\%, and an inclination of
53deg. The positions of AP Dor stars on the Hertzsprung-Russell (HR) diagram
are represented.
