  We performed the first photometric study of the CSS J003106.8+313347 W Ursae
Majoris (W UMa)-type system based on ground-based observations. We extracted
times of minima from our observations and proposed a linear ephemeris based on
the increasing incline of the orbital period using a Markov chain Monte Carlo
(MCMC) approach. The PHOEBE Python code and the MCMC approach were used for the
light curve analysis. This system did not need starspots for the light curve
analysis. Mass ratio, fillout factor, and inclination were obtained as 0.699,
0.322, and 60.6deg respectively. We also estimated the absolute parameters of
the system using the Gaia DR3 parallax method. Therefore, the masses, radii,
and luminosities have been determined to be M1=1.675, M2=1.171, R1=1.292,
R2=1.097, L1=1.348, and L2=1.221. The orbital angular momentum (J0) of the CSS
J003106.8+313347 illustrates that this system is located in a region of contact
binaries. The positions of the primary and secondary components on the
Hertzsprung-Russell (HR) diagram are depicted.
