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A new ephemeris, period change analysis and light curve modeling of the WUMa-type eclipsing binary BF Pav are presented in this study. Light curves ofthe system taken in BVRI filters from two observatories in Australia andArgentina were modeled using the Wilson-Devinney code. The results of thisanalysis demonstrate that BF Pav is a contact binary system with a photometricmass ratio q=1.460+_0.014, a fillout factor f=12.5%, an inclination of87.97+_0.45 deg and a cold spot on the secondary component. By using thedistance modulus formula, the distance of BF Pav was calculated to be d=268+_18pc which is in good agreement with the Gaia EDR3 distance. We obtain an orbitalperiod increase at a rate of 0.142 s/century due to a quadratic trend in theO-C diagram. Also, an alternative sudden period jump probably has occurredwhich could be interpreted as a rapid mass transfer from the lower mass star toits companion about DeltaM=2.45*10^(-6) Msun. Furthermore, there is anoscillatory behavior with a period of 18.3+_0.3 yr. Since BF Pav does not seemto have significant magnetic activity, this behavior could be interpreted asthe light-time effect caused by an undetected third body in this system. Inthis case, the probability for the third body to be a low mass star withM>=0.075 Msun or a brown dwarf is 5.4% and 94.6% respectively. If we assumei'=90deg, a_3=8.04+_0.33 AU. The mass of the secondary component was alsodetermined using two different methods which result close to each other.

BVRI Photometric Observations, Light Curve Solutions and Orbital Period Analysis of BF Pav