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We present the analysis of the binary-lens microlensing eventOGLE-2013-BLG-0911. The best-fit solutions indicate the binary mass ratio ofq~0.03 which differs from that reported in Shvartzvald+2016. The event suffersfrom the well-known close/wide degeneracy, resulting in two groups of solutionsfor the projected separation normalized by the Einstein radius of s~0.15 ors~7. The finite source and the parallax observations allow us to measure thelens physical parameters. The lens system is an M-dwarf orbited by a massiveJupiter companion at very close (M_{host}=0.30^{+0.08}_{-0.06} M_{Sun},M_{comp}=10.1^{+2.9}_{-2.2} M_{Jup}, a_{exp}=0.40^{+0.05}_{-0.04} au) or wide(M_{host}=0.28^{+0.10}_{-0.08} M_{Sun}, M_{comp}=9.9^{+3.8}_{-3.5}M_{Jup},a_{exp}=18.0^{+3.2}_{-3.2} au) separation. Although the mass ratio is slightlyabove the planet-brown dwarf (BD) mass-ratio boundary of q=0.03 which isgenerally used, the median physical mass of the companion is slightly below theplanet-BD mass boundary of 13M_{Jup}. It is likely that the formationmechanisms for BDs and planets are different and the objects near theboundaries could have been formed by either mechanism. It is important to probethe distribution of such companions with masses of ~13M_{Jup} in order tostatistically constrain the formation theories for both BDs and massiveplanets. In particular, the microlensing method is able to probe thedistribution around low-mass M-dwarfs and even BDs which is challenging forother exoplanet detection methods.

OGLE-2013-BLG-0911Lb: A Secondary on the Brown-Dwarf Planet Boundary around an M-dwarf