Early TANAMI Results 3 (Chile) and O’Higgins (Antarctica) telescopes only at 8.4 GHz, the lower frequency image has the higher res- olution, resolving the core and providing the finest view of the putative γ -ray production region seen so far. These simultaneous dual-frequency data are part of a set of simultaneous broadband data being used to model the behavior of Centaurus A [3]. First epoch images at 8.4 GHz of all 43 sources in the initial TANAMI sample have been analyzed and the results are presented in [15]. The images have high dynamic range and are often the best and sometimes the first images of an AGN at milliarcsecond scale resolution. Here we conclude this presentation with a few highlights from this analysis. Unless explicitly stated all discussions below are made with reference to the LAT 3-month list [2]. IV. FIRST EPOCH RESULTS FIG. 2: The core region of Centaurus A at 8.4 GHz. The best view yet of a possible γ -ray birthplace. FIG. 3: The core region of Centaurus A at 22 GHz. Note the close agreement with the core region at 8.4 GHz shown in the previous figure. • Morphology and the Fermi connection Figure 4 shows four sources which represent the four morphological classes we have classi- fied the TANAMI sample into. All the images are made with naturally weighted, 8.4 GHz data. The axes are labeled in units of milliarcseconds. The restoring beam of each image is shown as a hatched ellipse on the bottom left and, for the three sources that have known redshifts, a bar indicating a linear scale of 10 pc or 1 pc is shown on the bottom right. The root-mean- square (rms) noise in the images is typically about ∼ 0 . 5 mJy beam $^{$_{−}$1}$. The lowest contour level is at 3 times the root-mean-square noise level. of 0 . 68 × 0 . 41 mas happens to be comparable to the resolution (0 . 8 × 0 . 7mas) of the previous highest reso- lution image of this object [7]. Though these observa- tions are separated by about a decade the structures are remarkably similar which would appear to be con- trary to the previously reported apparent velocity of ∼ 1 . 4 mas [20]. Velocity information obtained from continuing multi-epoch TANAMI observations is be- ing used to investigate this. The classification scheme we have adopted is that of [9] which makes no assumptions about the physical nature of the objects thus sepa- rating their description from their interpreta- tion. Clockwise from the top left, are examples of single-sided (SS), compact (C), double-sided (DS) and Irregular (Irr) morphology. The initial TANAMI sample has 33 SS sources and 5 DS sources with just one example each of the other two morphological types. Three sources do not have an optical identification. All of the quasars and BL Lacertae objects in the sample have an SS morphology while all 5 DS sources are galax- ies. The lone C source is optically unidenti- fied while the only Irr source is a GPS galaxy 1718 − 649 which is tentatively detected by LAT [4]. Figure 2 and Figure 3 show the core region from naturally weighted images of Centaurus A at 8.4 GHz and 22 GHz respectively. In both cases the data have been self-calibrated using the CLEAN algorithm and the clean components in the final model have been replaced by Gaussian model components in order to parametrize the core region. There is close agree- ment between these two figures suggesting that the “core” has the same size at both frequencies. Due to the presence of trans-oceanic baselines to the TIGO In its first three months of operation Fermi de- tected 12 of 43 TANAMI sources with > 10 σ significance. All but one of these sources are quasars and BLLacertae objects with an SS eConf C091122