The Nature of the Halo Population of NGC 5128 Resolved with NICMOS on the [ITAL]HUBBLE SPACE TELESCOPE[/ITAL][ITAL]Hubble Space Telescope[/ITAL]

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Abstract
We present the first infrared (IR) color-magnitude diagram (CMD) for the halo of a giant elliptical galaxy. The CMD for the stars in the halo of NGC 5128 (Centaurus A) was constructed from Hubble Space Telescope NICMOS observations of the WFPC2 CHIP-3 field of Soria et al. to a 50% completeness magnitude limit of [F160W] = 23.8. This field is located at a distance of 08'50''(~9 kpc) south of the center of the galaxy. The luminosity function (LF) shows a marked discontinuity at [F160W] ≈ 20.0. This is 1–2 mag above the tip of the red giant branch (TRGB) expected for an old population (~12 Gyr) at the distance modulus of NGC 5128. We propose that the majority of stars above the TRGB have intermediate ages (~2 Gyr), in agreement with the WFPC2 observations of Soria et al. Five stars with magnitudes brighter than the LF discontinuity are most probably due to Galactic contamination. The weighted average of the mean giant branch color above our 50% completeness limit is [F110W]-[F160W] = 1.22 ± 0.08 with a dispersion of 0.19 mag. From our artificial-star experiments we determine that the observed spread in color is real, suggesting a real spread in metallicity. We estimate the lower and upper bounds of the stellar metallicity range by comparisons with observations of Galactic star clusters and theoretical isochrones. Assuming an old population, we find that, in the halo field of NGC 5128 we surveyed, stars have metallicities ranging from roughly 1% of solar at the blue end of the color spread to roughly solar at the red end, with a mean of [Fe/H] = -0.76 and a dispersion of 0.44 dex.
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