An Aligned Sub-Neptune Revealed with MAROON-X and a Tendency Towards Alignment for Small Planets

TL;DR

This study measures the obliquity of a long-period sub-Neptune, revealing a tendency towards alignment in small planets, and discusses implications for their formation history and system architecture.

Contribution

It provides the first obliquity measurement for a long-period sub-Neptune and analyzes the distribution of obliquities among small planets, highlighting a trend towards alignment.

Findings

TOI-1759A b is consistent with full alignment within uncertainties.

Small planets with R<8 R$_{ ext{Earth}}$ tend to be aligned, especially sub-Neptunes and super-Earths.

Misaligned small planets are more likely to be isolated than in compact systems.

Abstract

We present the Rossiter-McLaughlin measurement of the sub-Neptune TOI-1759A b with MAROON-X. A joint analysis with MuSCAT3 photometry and nine additional TESS transits produces a sky-projected obliquity of $|\lambda|$= $4^\circ\pm18^{\circ}$. We also derive a true obliquity of $\psi$=24$\pm12^{\circ}$ making this planet consistent with full alignment albeit to $<1\sigma$. With a period of 18.85 days and an $a/R_{*}$ of 40, TOI-1759A b is the longest period single sub-Neptune to have a measured obliquity. It joins a growing number of smaller planets which have had this measurement made and, along with K2-25 b, is the only single, aligned sub-Neptune known to date. We also provide an overview of the emerging distribution of obliquity measurements for planets with R$<8$ R$_{\oplus}$. We find that these types of planets tend toward alignment, especially the sub-Neptunes and super-Earths implying a dynamically cool formation history. The majority of misaligned planets in this category have 4$<$R$\leq$8 R$_{\oplus}$ and are more likely to be isolated than planets rather than in compact systems. We find this result to be significant at the $3\sigma$ level, consistent with previous studies. In addition, we conduct injection and recovery testing on available archival radial velocity data to put limits on the presence of massive companions in these systems. Current archival data is insufficient for most systems to have detected a giant planet.