  OB associations are important probes of recent star formation and Galactic
structure. In this study, we focus on the Auriga constellation, an important
region of star formation due to its numerous young stars, star-forming regions
and open clusters. We show using \textit{Gaia} data that its two previously
documented OB associations, Aur OB1 and OB2, are too extended in proper motion
and distance to be genuine associations, encouraging us to revisit the census
of OB associations in Auriga with modern techniques. We identify 5617 candidate
OB stars across the region using photometry, astrometry and our SED fitting
code, grouping these into 5 high-confidence OB associations using HDBSCAN.
Three of these are replacements to the historical pair of associations - Aur
OB2 is divided between a foreground and a background association - while the
other two associations are completely new. We connect these OB associations to
the surrounding open clusters and star-forming regions, analyse them physically
and kinematically, constraining their ages through a combination of 3D
kinematic traceback, the position of their members in the HR diagram and their
connection to clusters of known age. Four of these OB associations are
expanding, with kinematic ages up to a few tens of Myr. Finally, we identify an
age gradient in the region spanning several associations that coincides with
the motion of the Perseus spiral arm over the last $\sim$20 Myr across the
field of view.
