2025MNRAS.536.3745D

We report the first instance of an M dwarf/brown dwarf obliquity measurement for the TOI-2119 system using the Rossiter-McLaughlin effect. TOI-2119 b is a transiting brown dwarf orbiting a young, active early M dwarf ($T_{\rm {eff}}$ = 3553 K). It has a mass of 64.4 M$_{\rm {J}}$ and radius of 1.08 R$_{\rm {J}}$, with an eccentric orbit (e = 0.3) at a period of 7.2 d. For this analysis, we utilize NEID spectroscopic transit observations and ground-based simultaneous transit photometry from the Astrophysical Research Consortium and the Las Campanas Remote Observatory. We fit all available data of TOI-2119 b to refine the brown dwarf parameters and update the ephemeris. The classical Rossiter-McLaughlin technique yields a projected star-planet obliquity of $\lambda =-0.8\pm 1.1^\circ$ and a three-dimensional obliquity of $\psi =15.7\pm 5.5^\circ$. Additionally, we spatially resolve the stellar surface of TOI-2119 utilizing the Reloaded Rossiter-McLaughlin technique to determine the projected star-planet obliquity as $\lambda =1.26 \pm 1.3^{\circ }$. Both of these results agree within $2\sigma$ and confirm the system is aligned, where TOI-2119 b joins an emerging group of aligned brown dwarf obliquities. We also probe stellar surface activity on the surface of TOI-2119 in the form of centre-to-limb variations as well as the potential for differential rotation. Overall, we find tentative evidence for centre-to-limb variations on the star but do not detect evidence of differential rotation.