Deep ACS Imaging of the Halo of NGC 5128: Reaching the Horizontal Branch

Details Deep ACS Imaging of the Halo of NGC 5128: Reaching the Horizontal Branch Deep ACS Imaging of the Halo of NGC 5128: Reaching the Horizontal Branch

2005-05-31

arxiv.org/abs/astro-ph/0505622v1

Astrophys.J. 631 (2005) 262-279

Astronomy and Astrophysics

Astrophysics

Accepted by ApJ; 31 pages, uses emulateapj; 24 figures, most figures highly compressed; the full resolution version available

Scientific paper

10.1086/432462

Using the HST Wide Field Camera of the Advanced Camera for Surveys (ACS), we have obtained deep (V,I) photometry of an outer-halo field in NGC 5128, to a limiting magnitude of I~29. Our photometry directly reveals the core helium-burning stellar population (the ``red clump'' or horizontal branch) in a giant E/S0 galaxy for the first time. The color-magnitude diagram displays a very wide red giant branch (RGB), an asymptotic giant branch (AGB) bump, and the red clump; no noticeable population of blue HB stars is present, confirming previous suggestions that old, very metal-poor population is not ubiquitous in the halo of this galaxy. From the upper RGB we derive the metallicity distribution, which we find to be very broad and moderately metal-rich, with average [M/H]=-0.64 and dispersion 0.49 dex. The MDF is virtually identical to that found in other halo fields observed previously with the HST, but with an enhanced metal-rich population which was partially missed in the previous surveys due to V-band incompleteness for these very red stars. Combining the metallicity sensitive colors of the RGB stars with the metallicity and age sensitive features of the AGB bump and the red clump, we infer the average age of the halo stars to be 8^{+3}_{-3.5} Gy. As part of our study, we present an empirical calibration of the ACS F606W and F814W filters to the standard V and I bands, achieved with ground-based observations of the same field made from the EMMI camera of the New Technology Telescope of the ESO La Silla Observatory.

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