  Optical quasi-periodic oscillations (QPOs) are the most preferred signs of
sub-pc binary black hole (BBH) systems in AGN. In this manuscript, robust
optical QPOs are reported in quasar SDSS J1609+1756 at $z=0.347$. In order to
detect reliable optical QPOs, four different methods are applied to analyze the
4.45 years-long ZTF g/r/i-band light curves of SDSS J1609+1756, direct fitting
results by sine function, Generalized Lomb-Scargle periodogram, Auto-Cross
Correlation Function and Weighted Wavelet Z-transform method. The Four
different methods can lead to well determined reliable optical QPOs with
periodicities $\sim340$ days with confidence levels higher than 5$\sigma$, to
guarantee the robustness of the optical QPOs in SDSS J1609+1756. Meanwhile,
based on simulated light curves through CAR process to trace intrinsic AGN
activities, confidence level higher than $3\sigma$ can be confirmed that the
optical QPOs are not mis-detected in intrinsic AGN activities, re-confirming
the robust optical QPOs and strongly indicating a central sub-pc BBH system in
SDSS J1609+1756. Furthermore, based on apparent red-shifted shoulders in broad
Balmer emission lines in SDSS J1609+1756, space separation of the expected
central BBH system can be estimated to be smaller than $107\pm60$ light-days,
accepted upper limit of total BH mass $\sim(1.03\pm0.22)\times10^8{\rm
M_\odot}$. Therefore, to detect and report BBH system expected optical QPOs
with periodicities around 1 year is efficiently practicable through ZTF light
curves, and combining with peculiar broad line emission features, further clues
should be given on space separations of BBH systems in broad line AGN in the
near future.
