The bright stars 16 Cyg A and B have long been studied as solar analogs, with an age near 7 Gyr. Although they are members of a hierarchical triple system with a red dwarf companion, there are no dynamical constraints on the masses because the orbital period is longer than 18,000 years. After the 1997 discovery of a Jovian-mass exoplanet around 16 Cyg B, the system has generated even more interest. The Kepler space telescope obtained 30 months of nearly continuous observations of 16 Cyg A and B, allowing a more detailed asteroseismic characterization than is possible for any star other than the Sun. After reviewing recent determinations of the interior rotation and bulk helium abundance for 16 Cyg A and B, I will present new modeling results for the asteroseismic properties of these stars using the full-length Kepler data set. In particular, I will show how the composition and age derived independently for each component depend on the adopted set of constraints (asteroseismology, spectroscopy, luminosity, interferometric radius), the input physics, and the fitting methodology. The results provide important lessons for the future of automated asteroseismic analysis.