The PFS view of TOI-677 b: A spin-orbit aligned warm Jupiter in a dynamically hot system

Abstract

TOI-677 b is part of an emerging class of ``tidally-detached'' gas giants ($a/R_{\star }\gtrsim 11$) that exhibit large orbital eccentricities and yet low stellar obliquities. Such sources pose a challenge for models of giant planet formation, which must account for the excitation of high eccentricities without large changes in the orbital inclination. In this work, we present a new Rossiter-McLaughlin (RM) measurement for the tidally-detached warm Jupiter TOI-677 b, obtained using high-precision radial velocity observations from the PFS/Magellan spectrograph. Combined with previously published observations from the ESPRESSO/VLT spectrograph, we derive one of the most precisely constrained sky-projected spin-orbit angle measurements to date for an exoplanet. The combined fit offers a refined set of self-consistent parameters, including a low sky-projected stellar obliquity of $\lambda =3.2_{-1.5}^{+1.6}$ deg and a moderately high eccentricity of $e=0.460_{-0.018}^{+0.019}$, that further constrains the puzzling architecture of this system. We examine several potential scenarios that may have produced the current TOI-677 orbital configuration, ultimately concluding that TOI-677 b most likely had its eccentricity excited through disk-planet interactions. This system adds to a growing population of aligned warm Jupiters on eccentric orbits around hot ($T_{\mathrm{eff}}>6100$ K) stars.

arXiv comment16 pages, 4 figures, accepted for publication in the Astronomical Journal

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