  The distribution of stellar obliquities provides critical insight into the
formation and evolution pathways of exoplanets. In the past decade, it was
found that hot stars hosting hot Jupiters are more likely to have high
obliquities than cool stars, but it is not clear whether this trend exists only
for hot Jupiters or holds for other types of planets. In this work, we extend
the study of the obliquities of hot (6250-7000\,K) stars with transiting
super-Earth and sub-Neptune-sized planets. We constrain the obliquity
distribution based on measurements of the stars' projected rotation velocities.
Our sample consists of 170 TESS and \textit{Kepler} planet-hosting stars and
180 control stars chosen to have indistinguishable spectroscopic
characteristics. In our analysis, we find evidence suggesting that the planet
hosts have a systematically higher $\langle \sin i \rangle$ compared to the
control sample. This result implies that the planet hosts tend to have lower
obliquities. However, the observed difference in $\langle \sin i \rangle$ is
not significant enough to confirm spin-orbit alignment, as it is 3.8$\sigma$
away from perfect alignment. We also find evidence that within the
planet-hosting stars there is a trend of higher obliquity (lower $\langle \sin
i\rangle$) for the hotter stars ($\teff > 6250$ K) than for the cooler stars in
the sample. This suggests that hot stars hosting smaller planets exhibit a
broader obliquity distribution($\langle \sin i\rangle = 0.79 \pm 0.053$) than
cooler planet-hosting stars, indicating that high obliquities are not exclusive
to hot Jupiters and instead are more broadly tied to hot stars.
