The Halo Stars in NGC 5128. II. An Outer Halo Field and a New Metallicity Distribution

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The Distance to NGC 5128 (Centaurus A) (2009, methodology): “(V, I) photometry of resolved stars in three halo fields (at projected galactocentric distances of ,20, 30, and 40 kpc) has been done in NGC 5128 with the HST cameras WFPC2 and ACS/WFC (Harris et al. 1999; Harris & Harris 2000, 2002; Rejkuba et al. 2005).”
Photometry and the Metallicity Distribution of the Outer Halo of M31. II. The 30 Kiloparsec Field (2001, methodology): “In practice, we use stars in the brightest two magnitudes of the RGB and a grid of fiducial RGB model tracks to estimate the abundance [m/H] of each star (defined as [m/H] = log(Z/Z⊙), where we adopt Z⊙ = 0.0172 as in Harris & Harris 2000 and paper I).”
Observational evidence for AGN feedback in early-type galaxies (2007, methodology): “We construct an analytic form of the typical metallicity distribution from observations of the bulge of M31 and the closest earlytype galaxy NGC 5128 where individual stars can be resolved (Sarajedini & Jablonka 2005; Harris et al. 1999; Harris & Harris 2000, 2002).”
A CATALOG OF GLOBULAR CLUSTER SYSTEMS: WHAT DETERMINES THE SIZE OF A GALAXY'S GLOBULAR CLUSTER POPULATION? (2013, background): “By 1991 the number had grown to 60 (Harris 1991) and a decade later to 73 (Harris & Harris 2000), with the sample starting to include galaxies in a wider range of environments.”