Early TANAMI Results 5 V. CONCLUSION ples. The core brightness temperature ( T B ) limit of all initial TANAMI sources was calculated. The high end of the distribution of calculated bright- ness temperatures is dominated by quasars and the low end by BLLacertae objects and galaxies. Of the 43 sources in the sample, 13 have a max- imum T B below the equipartition value of 10 11 K [17], 29 below the inverse Compton limit of 10 12 K [10], putting about a third of the values above this limit. Doppler boosting is the most likely reason behind these high values though a variety of exotic mechanisms are also possible. There is no significant difference in the bright- ness temperature distribution of LBAS and non- LBAS sources. Many of the highest brightness temperature sources are not detected by LAT yet which is counterintuitive since they are ex- pected to have higher Doppler factors. The TANAMI program is providing high quality, high resolution radio monitoring for the southern third of the sky. Such data is a crucial member of the suite of multiwavelength observations that is set to revolu- tionize our understanding of the physics of AGN in the era of Fermi . Data from the TANAMI program is already a part of several individual AGN studies and statistical anal- ysis of the growing sample of TANAMI sources is pro- viding insight into the nature and origin of high energy radiation from AGN. The availability of core and jet component spectra as well as proper motions is going to greatly expand the questions that TANAMI can help answer. The core and the total luminosity was calcu- lated for all 38 initial TANAMI sources that had published redshifts, assuming isotropic emission. There is no significant difference in the distri- bution of luminosities of LBAS and non-LBAS sources. On the other hand, there is a clear re- lationship between luminosity and optical type with quasars dominating the high luminosity end of the distribution, galaxies dominating the low luminosity end while the BL Lacertae ob- jects fall in between, None of the five most distant and most lumi- nous sources have been detected by Fermi in its first 3 months of operation. Intriguingly, none of the nine most luminous jets (difference of total and core luminosities) are detected. If this per- sists it would suggest a completely unexpected anti-correlation between jet luminosity and γ - brightness. We are grateful to Dirk Behrend, Neil Gehrels, Julie McEnery, David Murphy, and John Reynolds, who contributed in various ways to the success of the TANAMI program so far. Furthermore, we thank the Fermi /LAT AGN group for the good collaboration. This research has been partially funded by the Bun- desministerium f¨ ur Wirtschaft und Technologie under Deutsches Zentrum f¨ ur Luft- und Raumfahrt grant number 50OR0808. This research has made use of the United States Naval Observatory (USNO) Radio Ref- erence Frame Image Database (RRFID). This research has made use of data from the NASA/IPAC Extra- galactic Database (NED, operated by the Jet Propul- sion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration); and the SIMBAD database (operated at CDS, Strasbourg, France). This research has made use of NASA’s Astrophysics Data System. VI. ACKNOWLEDGMENTS • Brightness Temperature • Luminosities [1] Abdo, A., A. et al. 2009 ApJ, 697, 934 [2] Abdo A. A., et al., 2009, ApJ 700, 597 [3] Abdo A. A., et al., 2010, In Preparation. [4] B¨ ock et al. 2009, These Proceedings [5] Ferrarese L. et al. 2007, ApJ, 654, 186 [6] Hartman, R. C. et al. 1999, ApJS, 123, 79 [7] Horiuchi, S., Meier, D., Preston, R., Tingay, S. 2005 PASJ, 58, 211 [8] Kadler, M. et al. 2010, In Preparation. [9] Kellermann K.I., Vermeulen R.C., Zensus J.A., Cohen M.H. 1998, AJ 115, 1295 [10] Kellermann K.I., Pauliny-Toth, I. I. K. 1969, ApJ 155, L71 [11] Kovalev Y.Y., Aller H.D., Aller M.F., et al., 2009, ApJ 696, L17 [12] Lister M.L., Aller H.D., Aller M.F., et al., 2009a, AJ 137, 3718 [13] M¨ uller et al. 2009, These Proceedings [14] Ojha R. et al., 2008, AIPC, 1053, 395 [15] Ojha R. et al., 2010, A&A, Submitted [16] Pushkarev, A. B., Kovalev, Y. Y., Lister, M. L., Savolainen, T. 2009, A&A, 507, L33 [17] Readhead, A. C. S. 1994, ApJ, 426, 51 [18] Taylor, G. B. et al. 2007, ApJ, 671, 1355 [19] Tingay, S. J. et al. 1998, AJ, 115, 960 [20] Tingay, S. J., Preston, R. A., Jauncey, D. L. 2001, eConf C091122