  Warm Jupiters lay out an excellent laboratory for testing models of planet
formation and migration. Their separation from the host star makes tidal
reprocessing of their orbits ineffective, which preserves the orbital
architectures that result from the planet-forming process. Among the measurable
properties, the orbital inclination with respect to the stellar rotational
axis, stands out as a crucial diagnostic for understanding the migration
mechanisms behind the origin of close-in planets. Observational limitations
have made the procurement of spin-orbit measurements heavily biased toward hot
Jupiter systems. In recent years, however, high-precision spectroscopy has
begun to provide obliquity measurements for planets well into the warm Jupiter
regime. In this study, we present Rossiter-McLaughlin (RM) measurements of the
projected obliquity angle for the warm Jupiter TOI-677 b using ESPRESSO at the
VLT. TOI-677 b exhibits an extreme degree of alignment ($\lambda = 0.3 \pm 1.3$
deg), which is particularly puzzling given its significant eccentricity ($e
\approx 0.45$). TOI-677 b thus joins a growing class of close-in giants that
exhibit large eccentricities and low spin-orbit angles, which is a
configuration not predicted by existing models. We also present the detection
of a candidate outer brown dwarf companion on an eccentric, wide orbit ($e
\approx 0.4$ and $P \approx 13$ yr). Using simple estimates, we show that this
companion is unlikely to be the cause of the unusual orbit of TOI-677 b.
Therefore, it is essential that future efforts prioritize the acquisition of RM
measurements for warm Jupiters.
