New data break the eccentricity multimodality of TOI-2134 c to e=0.31±0.01, refine both planets' masses and radii, and yield a 4.7σ RM obliquity of 59±31° for planet c.
On the Inference of a Star's Inclination Angle from its Rotation Velocity and Projected Rotation Velocity
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abstract
It is possible to learn about the orientation of a star's rotation axis by combining measurements of the star's rotation velocity ($v$) and its projection onto our line of sight ($v\sin i$). This idea has found many applications, including the investigation of the obliquities of stars with transiting planets. Here, we present a method for the probabilistic inference of the inclination of the star's rotation axis based on independent data sets that constrain $v$ and $v\sin i$. We also correct several errors and misconceptions that appear in the literature.
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Understanding eccentric temperate giants: an in-depth study of the architecture and stellar obliquity of the TOI-2134 system
New data break the eccentricity multimodality of TOI-2134 c to e=0.31±0.01, refine both planets' masses and radii, and yield a 4.7σ RM obliquity of 59±31° for planet c.