  The high-precision astrometry from the second data release of the Gaia
mission has made it possible to greatly improve the census of members of nearby
clusters and associations. I have applied the Gaia data to the Taurus
star-forming region, refining the sample of known members and identifying
candidates for undiscovered members. The resulting samples of members and
candidates provide the best constraints to date on the distribution of ages and
the initial mass function (IMF) in Taurus. Several studies over the last 30
years have proposed the existence of a population of older stars (>=10 Myr)
that is associated with the Taurus clouds. The data from Gaia demonstrate that
such a population does not exist. Meanwhile, previous IMF estimates for small
fields surrounding the Taurus aggregates have exhibited a surplus of K7-M0
stars (0.7-0.8 Msun) relative to star-forming clusters like IC 348 and the
Orion Nebula Cluster. However, that difference disappears when the new census
of the entire region is considered, which should be complete for spectral types
earlier than M6-M7 at A_J<1. Thus, there is little variation in the stellar IMF
across the 3-4 orders of magnitude in stellar density that are present in
nearby star-forming regions. Finally, I note that the proper motions of two
previously known members, KPNO 15 and 2MASS J04355209+2255039, indicate that
they may have been ejected from the same location within the L1536 cloud ~7200
years ago.
