In this review I will discuss early problems which confused our understanding of NGC 5128 and provide an overview of what we have learned about the properties of its old stars, with an emphasis on the globular cluster and field star populations. Because NGC 5128 is < 4 Mpc away ((m = M)0 = 27.9) we can study its stellar component in greater depth and detail than is possible for any other large elliptical galaxy. Consequently we have data for hundreds of globular clusters and planetary nebulae which are telling a rich history of how and when its stars formed. In addition (and unknown to many readers) we can now resolve individual halo stars, long period variables and Cepheids in NGC 5128, telling us its distance and providing additional clues to its history. For recent results on these and other stellar components see: distance (Harris et al. 2010), ages of field stars and long period variables (Rejkuba et al. 2003, Rejkuba et al. 2005), globular clusters (Peng et al. 2004b, Woodley & Gomez 2010b, Woodley et al. 2010a), and planetary nebulae (Walsh 1999, Peng et al. 2004a, Walsh et al. 2010).