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V606 Centauri (V606 Cen) is an early B-type close binary with an orbitalperiod of 1.4950935\,d and the complete light curves are very difficult to beobserved on the ground. By analyzing the unbroken and continuous light curveobtained by TESS, we found that it is a marginal contact binary with a very lowfill-out factor of about 2\%. The O-C diagram of V606 Cen is constructed forthe first time based on the 118.8-years eclipse times. It is found that the O-Cdiagram shows a downward parabolic change together with a cyclic oscillationwith an amplitude of 0.0544\, d and a period of 88.8\, yr. The downwardparabolic variation reveals a linear period decrease at a rate of $dP/dt =-2.06 \times{10^{-7}} d \cdot yr^{-1}$ that can be explained by the masstransfer from the more massive component to the less massive one. Both themarginal contact configuration and the continuous period decrease suggest thatV606 Cen is a newly formed contact binary via Case A mass transfer. Meanwhile,the cyclic change in the O-C diagram can be explained by the Light-Travel TimeEffect via the presence of a third body. The lowest mass of the tertiarycompanion is determined as M$_{3}$ = 4.51($\pm0.38$)M$_{\odot}$ that isorbiting around the central eclipsing binary in a nearly circular orbit(e=0.32). All the results indicate that V606 Cen is a newly formed massivecontact binary and just reaches the contact configuration during the masstransfer in a hierarchical triple system.

V606 Cen: A Newly Formed Massive Contact Binary in a Hierarchical Triple System