  More than two decades after the widespread detection of Jovian-class planets
on short-period orbits around other stars, their dynamical origins remain
imperfectly understood. In the traditional narrative, these highly irradiated
giant planets, like Jupiter and Saturn, are envisioned to have formed at large
stello-centric distances and to have subsequently undergone large-scale orbital
decay. Conversely, more recent models propose that a large fraction of hot
Jupiters could have formed via rapid gas accretion in their current orbital
neighborhood. In this study, we examine the period-mass distribution of
close-in giant planets, and demonstrate that the inner boundary of this
population conforms to the expectations of the in-situ formation scenario.
Specifically, we show that if conglomeration unfolds close to the disk's inner
edge, the semi-major axis - mass relation of the emergent planets should follow
a power law $a \propto M^{-2/7}$ - a trend clearly reflected in the data. We
further discuss corrections to this relationship due to tidal decay of
planetary orbits. Although our findings do not discount orbital migration as an
active physical process, they suggest that the characteristic range of orbital
migration experienced by giant planets is limited.
