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We present the period analysis of unfiltered photometric observations ofV5116 Sgr (Nova Sgr 2005 #2) and we search for superhump candidates in novaeremnants. The PDM method for period analysis is used. The masses of the novaecomponets are estimated from the secondary mass -- orbital period and primarymass -- decline time relations. We found that 13 nights of V5116 Sgrobservations in the year 2006 are modulated with a period of $0.1238 \pm0.0001$ d ($2.9712 \pm 0.0024$ h). Following the shape of the phased lightcurves and no apparent change in the value of the periodicity in differentsubsamples of the data, we interpret the period as orbital in nature. Thebinary system then falls within the period gap of the orbital perioddistribution of cataclysmic variables. From the maximum magnitude -- rate ofdecline relation, we estimate the maximum absolute visual magnitude of $M_{\rmVmax} = -8.85 \pm 0.04$ mag using the measured value of decline $t_{\rm 2} =6.5 \pm 1.0$ d. The mass-period relation for cataclysmic variables yields asecondary mass estimate of about $0.26 \pm 0.05 {\rm M}_{\rm \odot}$. Wepropose that V5116 Sgr is a high inclination system showing an irradiationeffect of the secondary star. No fully developed accretion disc up to the tidalradius with the value lower than $3.5 10^{10}$ cm is probable. The mass ratiowas estimated in a few novae and the presence or absence of superhumps in thesesystems was compared with the mass ratio limit for superhumps of about 0.35. Wefound that in the majority of novae with expected superhumps, this variabilityhas not been found yet. Therefore, more observations of these systems isencouraged.

Nova V5116 Sgr and searching for superhumps in nova remnants