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In order to investigate whether the brightest globular clusters (GCs) in thegiant elliptical galaxies are similar to the less luminous GCs like those foundin Local Group galaxies, we study the velocity dispersion and structuralparameter correlations of a sample of bright GCs in the nearest gE galaxy NGC5128. UVES echelle spectrograph on the ESO VLT, and EMMI on the ESO NTT wereused to obtain high resolution spectra of bright GCs in NGC 5128. The velocitydispersions were obtained for all the targets. The structural parameters wereeither taken from the existing literature, or derived from our VLT FORS1 imagesusing the ISHAPE software. The velocity dispersion and structural parametermeasurements were used to obtain masses and M/L_V ratios of 22 clusters. Themasses of the clusters in our sample range from M_vir=10^5-10^7 M_sun and theaverage M/L_V is 3+/-1. The three GCs harbouring X-ray point sources are thesecond, third and sixth most massive in our sample. The most massive cluster,HCH99-18, is also the brightest and the largest in size. It has the mass(M_vir=1.4x10^7 M_sun) an order of magnitude larger than the most massiveclusters in the Local Group, and a high M/L_V ratio (4.7+/-1.2). We discussbriefly possible formation scenarios for this object. The correlations ofstructural parameters, velocity dispersion, masses and M/L_V for the bright GCsin NGC 5128 extend the properties established for the most massive Local Groupclusters towards those characteristic of dE galaxy nuclei and Ultra CompactDwarfs (UCDs). The detection of the mass-radius and the mass-M/L_V relationsfor the GCs with masses greater than ~2x10^6 M_sun provides the missing linkbetween ``normal'' old globular clusters, young massive clusters, and evolvedobjects like UCDs. (Abridged)Comment: Accepted for publication in A&A; 18 pages, 11 figure

Bright globular clusters in NGC 5128: the missing link between young massive clusters and evolved massive objects