The chemical connection between 67P/C-G and IRAS 16293-2422
  The chemical evolution of a star- and planet-forming system begins in the
prestellar phase and proceeds across the subsequent evolutionary phases. The
chemical trail from cores to protoplanetary disks to planetary embryos can be
studied by comparing distant young protostars and comets in our Solar System.
One particularly chemically rich system that is thought to be analogous to our
own is the low-mass IRAS 16293-2422. ALMA-PILS observations have made the study
of chemistry on the disk scales (< 100 AU) of this system possible. Under the
assumption that comets are pristine tracers of the outer parts of the innate
protosolar disk, it is possible to compare the composition of our infant Solar
System to that of IRAS 16293-2422. The Rosetta mission has yielded a wealth of
unique in situ measurements on comet 67P/C-G, making it the best probe to date.
Herein, the initial comparisons in terms of the chemical composition and
isotopic ratios are summarized. Much work is still to be carried out in the
future as the analysis of both of these data sets is still ongoing.
