4 Figure 4: The γ -ray index versus submillimeter index plane. The blazars fall more steeply in the γ -rays than in the submillimeter band, where most are, in fact, rising. This LAT-detected sample contrasts with the full SMA sample, where the blazars are more distributed around α$_{S}$ ∼ 0. as the presence of SSC versus ERC. Here, we use sub- millimeter luminosity as a proxy for jet power, which is correlated with the integrated luminosity of the syn- chrotron component. Elevated γ -ray luminosity with respect to the synchrotron component (which is often seen in FSRQs) suggests the upscattering of external photons off the synchrotron-emitting electrons. These objects should occupy the upper right of the ratio/jet power plot, and BL Lacs, which generally exhibit com- ponents with roughly comparable luminosities, should occupy the lower left. It is clear from the figure, how- ever, that many FSRQs exhibit ratios similar to those of the BL Lacs and vis versa. low luminosity ratios and high luminosity, which sug- gest they may be undergoing the same changes as 3C 454.3. A possible interpretation of the elevated lumi- nosity ratios observed in some BL Lacs objects is that there has been a dramatic increase in γ -ray luminos- ity due to ERC, which would not be reflected in the synchrotron component. Sikora et al. [10] report that, during its flaring epochs, 3C 454.3 transitions from its typical FSRQ state to a more BL Lac-like state, where the syn- chrotron component emits much more strongly com- pared to the γ -ray component than during its “low state”. 3C 454.3, which is the highest submillime- ter luminosity FSRQ in our sample, would then shift down and to the right in Figure 5 when it enters a flaring period. For the first three months of the Fermi mission, 3C 454.3 was not flaring, which may explain its present location in Figure 5. The three objects for which there is a type discrepancy between CGRaBS and LBAS are all FSRQs (in CGRaBS) and exhibit The motivation for observing blazars in the sub- millimeter is to study behavior close to the central engine, where the jet material is presumably still be- ing accelerated. The separate emission processes that contribute to overall SED may present differently in BL Lacs and FSRQs, allowing us to understand the similarities and differences between blazar types. We have investigated these differences between objects in terms of submillimeter behavior and, in conclusion, find that • The SMA blazars exhibit submillimeter energy spectral indexes that follow the spectral se- quence interpretation of blazars. 5. CONCLUSIONS eConf C091122 2009 Fermi Symposium, Washington, D.C., Nov. 2-5