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We present new results concerning the sub-stellar binary population in theOrion Nebula Cluster (ONC). Using the Karhunen-Lo\`{e}ve Image Projection(KLIP) algorithm, we have reprocessed images taken with the IR channel of theWide Field Camera 3 mounted on the Hubble Space Telescope to unveil faint closecompanions in the wings of the stellar PSFs. Starting with a sample of $1392$bona-fide not saturated cluster members, we detect $39$ close-pairs clustercandidates with separation $0.16''-0.77''$. The primary masses span a rangeM$_p$ $\sim 0.015-1.27$ M$_{\odot}$ whereas for the companions we derive M$_c$$\sim 0.004-0.54$ M$_{\odot}$. Of these $39$ binary systems, $18$ were alreadyknown while the remaining $21$ are new detections. Correcting for completenessand combining our catalog with previously detected ONC binaries, we obtain anoverall binary fraction of $11.5\% \pm 0.9\%$. Compared to other star formingregions, our multiplicity function is $\sim 2$ smaller than e.g. Taurus, whilecompared to the binaries in the field we obtain comparable values. We analyzethe mass function of the binaries, finding differences between the massdistribution of binaries and single stars and between primary and companionmass distributions. The mass ratio shows a bottom-heavy distribution withmedian value of $M_c/M_p \sim 0.25$. Overall our results suggest that ONCbinaries may represent a template for the typical population of field binaries,supporting the hypothesis that the ONC may be regarded as a most typical starforming region in the Milky Way.

HST survey of the Orion Nebula Cluster in the H$_2$O 1.4 $\mu$m absorption band: III. The population of sub-stellar binary companions