([denoted]{} “bkgd star” for background star), we derived a mass range of $\sim$2–4 $M_{\rm{J}}$ according to the [atmospheric and evolutionary models of @Baraffe2015 and @Baraffe2003]{} considering the uncertainties on its measured magnitudes and the system distance and age [@Mueller2011]. Using consortium tools developed for the classification and the ranking of the companion candidates discovered in SPHERE/SHINE, we also computed a background probability for this point source of $\sim$13.5% assuming the Besançon model predictions [@Robin2003]. With the same suite of tools, we derived the color-magnitude diagram of the [point source]{} shown in Fig. \[fig:cmdiagram\] to compare its $K1-K2$ color to the colors of field and young dwarfs covering the M, L, T, and Y types. Further details about the derivation of the color-magnitude diagram are provided in [@Mesa2016. Its $K1-K2$ color]{} is similar to a late-L or early-T [dwarf,]{} but its $K1$ magnitude is slightly fainter with respect to what is expected for objects of these spectral types. The point source is also seen in an HST/STIS image published in @Grady2009 (program GO-8674, P.I. Lagrange). We retrieved [the reduced image (corrected for cosmetics and distortion) from the HST archive,]{} and measured the astrometry of the [point source]{} ($r$=4932$\pm$28 mas, $\theta$=314.5$\pm$0.33$^{\circ}$) to 