A Homogeneous Catalog of Rossiter-McLaughlin Systems: Distinct $e$-$\lambda$ Trends in Three Gas-Giant Mass Regimes

Stellar obliquity ($\lambda$) and orbital eccentricity ($e$) trace the dynamical histories of close-in giant planets, but the current observational picture is assembled from heterogeneous analyses that have obscured population-level trends. In this work, we homogeneously refit systems with Rossiter-McLaughlin (RM) measurements by performing a joint global fit to spectral energy distributions, transit light curves, mid-transit times, out-of-transit and in-transit radial velocities, yielding self-consistent posterior distributions for the physical and orbital parameters of both stars and planets across 255 systems. Restricting to 145 single-star systems with reliable planet-mass measurements, we uncover pronounced structure in the $e-\lambda$ plane that depends on planet mass: (i) sub-Saturns ($M_{\mathrm{p}}\le \sim 0.3M_{\mathrm{J}}$) can be both eccentric and misaligned; (ii) Jupiters ($\sim 0.3M_{\mathrm{J}}<M_{\mathrm{p}}\le \sim 3M_{\mathrm{J}}$) are misaligned only on circular orbits; and (iii) super Jupiters and brown dwarfs ($M_{\mathrm{p}}>\sim 3M_{\mathrm{J}}$) are aligned across the full eccentricity range. A two-dimensional Kolmogorov-Smirnov test shows that the joint $(e,\lambda )$ distributions differ significantly among these three mass regimes. These trends demonstrate that $\lambda$ depends jointly on eccentricity and planet mass, implying that obliquity alone is not a unique tracer of evolutionary history and underscoring the need for a unified framework for the origins of spin-orbit misalignment. The full catalog from this work is publicly available at https://www.stellarobliquity.com .