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Simulated color-magnitude diagrams (CMDs) are used to investigate the recentstar formation history in NGC 5128. The comparison of the simulations with theobserved UV CMD for a field in the NE shell, where recent star formation ispresent, constrains the initial mass function (IMF) and the duration of thestar formation episode. The star formation burst is still on-going or at mosthas stopped some 2 Myr ago. The look-back time on the main sequence is set bythe incompleteness of the U-band observations at V~26, and is of the order of50 Myr. The post main sequence phases have a look-back time up to 100 Myr,setting the maximum observable time for the star formation in this field. Thecomparison of the observed and simulated luminosity functions and the number ofpost main sequence vs. total number of stars favours models with active starformation in the last 100 Myr. The data are best fitted by an IMF with Salpeterslope (\alpha=2.35), and are also consistent with slopes in the range of2<~\alpha<~2.6. They exclude steeper IMF slopes. The mean star formation ratefor a Salpeter IMF in the range of masses 0.6<~M<~100 M_sun within the last 100Myr is 1.6x10^-4 M_sun yr^-1 kpc^-2.Comment: 16 pages, 10 figures; A&A in pres

Simulating the recent star formation history in the halo of NGC 5128