  Although close-orbiting, massive exoplanets -- known as hot and warm Jupiters
-- are among the most observationally accessible known planets, their formation
pathways are still not universally agreed upon. One method to constrain the
possible dynamical histories of such planets is to measure the systems'
sky-projected spin-orbit angles using the Rossiter-McLaughlin effect. By
demonstrating whether planets orbit around the stellar equator or on offset
orbits, Rossiter-McLaughlin observations offer clues as to whether the planet
had a quiescent or violent formation history. Such measurements are, however,
only a reliable window into the history of the system if the planet in question
orbits sufficiently far from its host star; otherwise, tidal interactions with
the host star can erase evidence of past dynamical upheavals. We present a
WIYN/NEID Rossiter-McLaughlin measurement of the tidally detached ($a/R_* =
13.18^{+0.35}_{-0.37}$) warm Jupiter WASP-106 b, which orbits a star along the
Kraft break ($T_{\mathrm{eff}}=6002\pm164$ K). We find that WASP-106 b is
consistent with a low spin-orbit angle ($\lambda=6^{+17}_{-16}\,^{\circ}$ and
$\psi = 26^{+12}_{-17}\,^{\circ}$), suggesting a relatively quiescent formation
history for the system. We conclude by comparing the stellar obliquities of hot
and warm Jupiter systems, with the WASP-106 system included, to gain insight
into the possible formation routes of these populations of exoplanets.
