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The Distance to NGC 5128 (Centaurus A)

Published online by Cambridge University Press:  02 January 2013

Gretchen L. H. Harris ,
Marina Rejkuba  and
William E. Harris
Gretchen L. H. Harris*
Affiliation:
Department of Physics and Astronomy, University of Waterloo, Waterloo ON, N2L 3G1, Canada
Marina Rejkuba
Affiliation:
European Southern Observatory, Karl-Schwarzschild-Strasse 2, D-85748 Garching, Germany
William E. Harris
Affiliation:
Department of Physics and Astronomy, McMaster University, Hamilton ON, L8P 2X7, Canada
*
DCorresponding author. Email: glharris@astro.uwaterloo.ca
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Abstract

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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.

Keywords

Galaxies: distances and redshiftsgalaxies: individual (NGC 5128)galaxies: stellar content

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