3 2009 Fermi Symposium, Washington, D.C., Nov. 2-5 Table I: Physical parameters estimation IAU Name (B1950.0) Alternative Name Epoch p a$_{,}$b B b$_{,}$c ⊥ [G] Comments 0235+164 AO 0235+16 2008-09-02 0 . 8 ≤ 0 . 89 0528+134 2008-10-02 1 . 4 ≤ 0 . 12 0716+714 2009-02-05 inverted spectrum α = 0 . 4, model N/A d 0827+243 OJ 248 2009-04-09 1 . 6 ≤ 3 . 4 0851+202 OJ 287 2009-02-02 inverted spectrum α = 0 . 7, model N/A d 1219+285 W Com 2009-05-14 0 . 8 ≤ 108 preliminary analysis 1226+023 3C 273 2009-02-05 2 . 0 ≤ 0 . 016 1253 − 055 3C 279 2009-02-02 1 . 4 ≤ 0 . 89 1510 − 089 2009-04-09 inverted spectrum α = 0 . 2, model N/A d 1633+383 4C 38.41 2009-06-20 1 . 0 ≤ 0 . 24 preliminary analysis 1652+398 Mrk 501 2009-05-14 1 . 6 ≤ 3 . 5 preliminary analysis 1730 − 130 NRAO 530 2009-06-20 1 . 6 ≤ 3 . 6 preliminary analysis 1959+650 2008-10-23 1 . 4 ≤ 17 2155 − 304 2008-09-05 1 . 0 ≤ 26 2200+420 BL Lac 2008-09-02 1 . 0 ≤ 0 . 44 2251+158 3C 454.3 2008-10-02 inverted spectrum α = 0 . 8, model N/A d 2344+514 2008-10-23 1 . 2 ≤ 57 43 GHz data not included in the fit a p is the power law index in the electron energy distribution N ( E ) = N 0 E − p . Note, that for the optically thin part of the synchrotron spectrum p = 1 − 2 α , where α is defined as S$_{ν}$ ∼ ν α . b The estimates correspond to the region of parsec-scale radio core. c The values are in the observer’s frame. d The homogeneous synchrotron source model is not applicable for this spectrum. K. Sokolovsky is supported by the International Max-Planck Research School (IMPRS) for Astron- omy and Astrophysics at the universities of Bonn and Cologne. T. Savolainen is a research fellow of the Alexander von Humboldt foundation. T. Savolainen also acknowledges support by the Academy of Fin- land grant 120516. Y. Kovalev was supported by the return fellowship of Alexander von Humboldt foun- dation and the Russian Foundation for Basic Re- search (RFBR) grant 08-02-00545. This research has been partially funded by the Bundesministerium f¨ ur Wirtschaft und Technologie under Deutsches Zentrum f¨ ur Luft- und Raumfahrt grant number 50OR0808. This work is based on data obtained from the National Radio Astronomy Observatory’s Very Long Baseline Array (VLBA), project BK150. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agree- ment by Associated Universities, Inc. This research has made use of NASA’s Astrophysics Data Sys- tem; the NASA/IPAC Extragalactic Database (NED) which is operated by the JPL, Caltech, under contract with the NASA, the SIMBAD database, operated at CDS, Strasbourg, France. The authors are grateful to E. Ros for reviewing this manuscript. References Acknowledgments eConf C091122 1 Atwood W. B., et al., 2009, ApJ, 697, 1071 2 Zensus J. A., 1997, ARA&A, 35, 607 3 Savolainen T., Wiik K., Valtaoja E., Tornikoski M. 2008, ASPC, 386, 451 4 Lobanov, A. P. 1998, A&AS,132, 261 5 Napier P. J., 1994, IAUS, 158, 117 6 Fomalont E., 1981, NRAON, 3, 3 7 Shepherd M.C., Pearson T.J. and Taylor G.B. 1994, BAAS, 26, 987 8 Kovalev, Y. Y., Lobanov, A. P., Pushkarev, A. B., & Zensus, J. A. 2008, A&A, 483, 759 9 Lobanov, A. P. 1998, A&A, 330, 79 10 Pacholczyk A.G. 1970, Radio astrophysics, San Francisco: Freeman 11 Virtanen, J. J. P., & Vainio, R. 2005, ApJ, 621, 313 12 Kovalev, Y. Y., et al. 2009, ApJL, 696, L17 13 Marscher A.P. 1983, ApJ, 264, 296