The multiple star 14 Aurigae (= ADS 3824) contains five visual members, of which A and C (both of them single-lined spectroscopic binaries) form a physical system. Extreme ultraviolet observations reveal a hot white dwarf superposed on 14 Au r C. Ultraviolet spectroscopy reveals that it is a distant companion to the optical spectroscopic binary, but that is a physical member of the system. Capitalizing on the fact that the visible component of 14 Aur A, KW Aur, in somewhat evolved, and is both an ellipsoidal variable and δ Scuti pulsator, we are able to model this quintuple system, obtaining both an evolutionary age for the system and a cooling age for the white dwarf, also masses for all five components, orbital inclinations for the two spectroscopic binaries, and an improved distance estimate to the system. Our results provide empirical values of the pulsation constants of KW Aur, and an estimate of the initial as well as final mass of the white dwar.