  We present observational constraints for the initial-to-final mass relation
(IFMR) derived from 9 white dwarfs (WDs) in wide binaries (WBs) that contain a
turnoff/subgiant primary. Because the components of WBs are coeval to a good
approximation, the age of the WD progenitor can be determined from the study of
its wide companion. However, previous works that used WBs to constrain the IFMR
suffered from large uncertainties in the initial masses because their MS
primaries are difficult to age-date with good precision. Our selection of WBs
with slightly evolved primaries avoids this problem by restricting to a region
of parameter space where isochrone ages are significantly easier to determine
with precision. We selected a sample of WBs with adequate characteristics for
our program by matching existing catalogs of WDs with the Gaia astrometric
surveys. We obtained more precise constraints than existing ones in the mass
range 1-2.2 M$_{\odot}$, corresponding to a previously poorly constrained
region of the IFMR. Having introduced the use of turnoff/subgiant-WD binaries,
the study of the IFMR is not limited anymore by the precision in initial mass,
but now the pressure is on final mass, i.e., the mass of the WD today. Looking
at the full dataset, our results would suggest an unexpectedly large dispersion
in the IFMR at low initial masses. However, such behavior is driven by three
overmassive WDs in systems with SG primaries that, upon closer inspection,
appear to be (close) binaries themselves. Improved characterization for these
systems would be important for settling this question.
