2009/11/30 by Gretchen L. H. Harris, Marina Rejkuba, William E. Harris · 225 citations
Physics and Astronomy · #Astronomy and Astrophysical Research #Brightness #Distance modulus #Galaxy #History and Developments in Astronomy #Hubble sequence #Luminosity #Milky Way #Photometry (optics) #Stellar, planetary, and galactic studies #Surface brightness fluctuation #astro-ph.GA
paper · pdf · doi:10.1071/as09061
published in Publications of the Astronomical Society of Australia 27(4), 457-462 (Cambridge University Press) · in press PASA; minor text changes
arxiv created 2009/12/03 · openalex publication_date 2010/01/01 · arxiv updated 2015/05/14 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/08
Abstract In this paper we review the various high precision methods that are now available to determine the distance to NGC 5128. These methods include: Cepheids, TRGB (tip of the red giant branch), PNLF (planetary nebula luminosity function), SBF (surface brightness fluctuations), and Long Period Variable (LPV) Mira stars. From an evaluation of these methods and their uncertainties, we derive a best-estimate distance of 3.8±0.1 Mpc to NGC 5128 and find that this mean is now well supported by the current data. We also discuss the role of NGC 5128 more generally for the extragalactic distance scale as a testbed for the most direct possible comparison among these key methods.