age determined for the Collinder359 has changed dramatically since the early determination by [@wi] of 20 to 50Myr. Later studies derived 30Myr [@abt]. Both results are in agreement and consistent with the more recent values range from 50Myr [@ba; @kha]. [@jef] put an upper limit of 100Myr on the age of Collinder 359 using the lithium test described by [@reb]. Comparison with the various evolutionary tracks indicates that the components of V2653Oph have an age of about 300($\pm$100)Myr, older than the cluster. If the binary is really a member of the cluster its age should be at least three times older than the values estimated up to date.

$\gamma$ Dor type variables in close binary systems
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Fig.4 shows that there is a considerable light variations at outside of eclipses. The $\gamma$ Dor type pulsating single stars and components in the eclipsing binaries were plotted in the logT$_{eff}$-logL/L$_{\odot}$ plane and shown in Fig.5. The empty symbols show the single stars taken from the catalog of @henry while the filled circles indicate the $\gamma$ Doradus type pulsators in the eclipsing binaries. The primary component of V2653Oph locates in the instability strip of $\gamma$ Doradus type variable stars. The known $\gamma$ Dor 