2 2009 Fermi Symposium, Washington, D.C., Nov. 2-5 IAU B 1950 name Alt. name Source type z β$_{app}$ a LAT 1st-year b pc-scale structure c 0333+321 NRAO 140 LPRQ d 1.258 12.9 ± 0.3 Y core-jet over 20 mas (168 pc) 0403 − 132 PKS 0403 − 13 HPRQ e 0.571 21.0 ± 1.0 Y core-jet over 15 mas (97.7 pc) 0422+004 PKS B0422+004 BL Lac - No redshift f Y core-jet over 10 mas 0823+033 PKS 0823+033 BL Lac 0.506 15.0 ± 1.0 Y core-jet over 15 mas (91.8 pc) 1458+718 3C 309.1 LPRQ d 0.905 8.0 ± 3.0 N core-jet over 30 mas (235 pc) 1828+487 3C 380 LPRQ d 0.692 13.1 ± 0.4 Y core-jet over 25 mas (178 pc) a Apparent projected speed in units of the speed of light (values from MOJAVE, see [8]). b Preliminary LAT first-year catalog. c pc-scale structure from [2]. d Low polarization radio quasar. e High polarization radio quasar. f The redshift of this source is not available. The sky proper motion is 0.38 ± 0.08 mas yr $^{$_{−}$1}$. Table I: Source properties not included in the preliminary Fermi LAT year-one source list (Abdo et al., in preparation). synchrotron peak (see [11]). In contrast to this, we see a trend that the SSC peak is comparable or lower than the synchrotron peak in the SED of these gamma-faint blazars, which are among the radio-brightest blazars in the sky. However, we need additional data to study the correlation between both peaks, as well as a de- tailed model of the physical process to reproduce the observed SED. There are two categories of SED models, with an interpretation of the high-energy part as being caused by Compton upscattering by leptons [9] or by hadronic processes [10]. The lower energy part (corresponding to the synchrotron radiation) is originated by leptons. For gamma-faint sources, we are interested in investi- gating the relation between the synchrotron peak and the synchrotron self-Compton (SSC) peak, and the ex- trapolation from the rising part before the SSC peak (X-ray) to the gamma-ray range. In this aspect, SED fitting is needed, and will be included in a near future. Here we discuss our preliminary SED results. Most of the sources appear to have a compa- rable value of the synchrotron peak and the SSC peak. The spectra of NRAO 140, PKS 0403 − 13, PKS B0422+004, and PKS 0823+033 (Figure 1 to 4) are flat to inverted in flux density, and the latter two are steeper. The slopes of the radio spectra are milder for 3C 309.1 and 3C 380 (Figure 5 and 6). If we ex- trapolate the SED from X-ray to gamma-rays, we see that the SSC peak seems lower than the synchrotron peak in PKS B0422+004 and 3C 309.1 (Figure 3 and 5). For PKS 0823+033, although the SSC peak ap- pears slightly lower than the synchrotron peak by ex- trapolating from the X-ray spectrum, the gamma-ray flux increases at higher energies. This source is not in the TeV catalog $^{1}$, and we need further analysis on the hardness of the gamma-ray spectrum in order to confirm this spectral rise in higher energies. For NRAO 140 (Figure 1), PKS 0403 − 13 (Figure 2), and 3C 380 (Figure 6), the SSC peak is comparable with the synchrotron peak. For gamma-bright blazars, the SSC peak in their SED tend to be a bit higher than the We are compiling a broadband SED catalog for the 135 sources in the MOJAVE sample. Once collected, detailed analysis of the emission processes involved in the SED will be performed, and the deduced prop- erties will be compared with the radio properties de- termined by the MOJAVE and by single-dish observ- ing programs. Among the radio-bright sample, the gamma-faint sources are especially interesting for that they provide us a chance to probe the link between radio and gamma-rays, and to find out the key which affects the emission process. For further investiga- tion, the broadband SED modelling will be performed in the future, in order to understand the nature of blazars. We thank especially C. Ricci, M. B¨ ock, L. Barrag´ an, J. Wilms, and C. M. Fromm for valuable discussions. This research was supported by the EU Framework 6 Marie Curie Early Stage Training program under contract number MEST/CT/2005/19669 ESTRELA. C. S. Chang is a member of the International Max Acknowledgments 3. Outlook $^{1}$http://tevcat.uchicago.edu/ eConf C091122