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We present the photometric properties of V608 Cas from detailed studies oflight curves and eclipse timings. The light curve synthesis indicates that theeclipsing pair is an overcontact binary with parameters of $\Delta T$ = 155 K,$q$ = 0.328, and $f$ = 26 %. We detected the third light $\ell_{3}$, whichcorresponds to about 8 % and 5 % of the total systemic light in $V$ and $R$bands, respectively. Including our 6 timing measurements, a total of 38 timesof minimum light were used for a period study. It was found that the orbitalperiod of V608 Cas has varied in some combination of an upward parabola and twoperiodic variations. The continuous period increase with a rate of$+$3.99$\times$10$^{-7}$ d yr$^{-1}$ can be interpreted as a mass transfer fromthe secondary component to the primary star at a rate of 1.51$\times$10$^{-7}$M$_\odot$ yr$^{-1}$. The periods and semi-amplitudes of the two periodicvariations are about $P_3$ = 16.0 yr and $P_4$ = 26.3 yr, and $K_3$ = 0.0341 dand $K_4$ = 0.0305 d, respectively. The most likely explanation of both cyclesis a pair of light-traveling time effects operated by the possible presence ofthird and fourth components with estimated masses of $M_3$ = 2.20 M$_\odot$ and$M_4$ = 1.27 M$_\odot$ in eccentric orbits of $e_3$ = 0.66 and $e_4$ = 0.52.Because the contribution of $\ell_{3}$ is very low compared to the estimatedmasses of two circumbinary objects, they can be inferred as very faint compactobjects.

V608 Cassiopeiae: A W UMa-type eclipsing binary with two possible circumbinary companions