A 2dF spectroscopic study of globular clusters in NGC 5128: probing the formation history of the nearest giant elliptical

We have performed a spectroscopic study of globular clusters (GCs) in the nearest giant elliptical NGC 5128 using the 2dF facility at the Anglo-Australian Telescope. We obtained integrated optical spectra for a total of 254 GCs, 79 of which are newly confirmed on the basis of their radial velocities and spectra. In addition, we obtained an integrated spectrum of the galaxy starlight along the southern major axis. We derive an empirical metallicity distribution function (MDF) for 207 GCs (similar to 14 per cent of the estimated total GC system) based upon MilkyWay GCs. This MDF is multimodal at high statistical significance with peaks at [Z/H]similar to -1.3 and -0.5. A comparison between the GC MDF and that of the stellar halo at 20 kpc (similar to 4R(e)) reveals close coincidence at the metal-rich ends of the distributions. However, an inner 8-kpc stellar MDF shows a clear excess of metal-rich stars when compared to the GCs. We compare a higher signal-to-noise ratio (S/N) subsample ( 147 GCs) with two stellar population models which include non-solar abundance ratio corrections. The vast majority of our sample (similar to 90 per cent) appears old, with ages similar to the MilkyWay GC system. There is evidence for a population of intermediate-age (similar to 4-8 Gyr) GCs (<= 15 per cent of the sample) which are on average more metal-rich than the old GCs. We also identify at least one younger cluster (similar to 1 - 2 Gyr) in the central regions of the galaxy. Our observations are consistent with a picture where NGC 5128 has undergone at least two mergers and/or interactions involving star formation and limited GC formation since z = 1, however the effect of non-canonical hot stellar populations on the integrated spectra of GCs remains an outstanding uncertainty in our GC age estimates.