Mass-metallicity plane populated with companions from different samples, adapted from Thorngren et al. (2016), Nasedkin et al. (2024) and Balmer et al. (2024). The orange points show transiting giant exoplanets from Thorngren et al. (2016). The grey points illustrate a set of directly detected planets, and the blue points show a subset that was observed using VLTI/GRAVITY. Both samples were compiled by Nasedkin et al. (2024) and references therein. For context, Jupiter and Saturn are included with the metallicity measurements taken from Guillot (1999). The orange line and confidence interval trace the empirical relation between mass and metallicity for giant exoplanets presented by Thorngren et al. (2016). The black diamond indicates the ratio derived for HIP 99770 b when assuming a solar metallicity for the host. We took the higher metallicity ratios obtained from the host metallic-ity estimates by Paunzen et al. (1999, 2002), and Villaume et al. (2017) into account by presenting the data point with an inflated error bar that reflects a skewed systematic error encompassing the 68% confidence interval of the highest encountered ratio.