2009 Fermi Symposium, Washington, D.C., Nov. 2-5 5 Figure 5: Ratio of γ -ray luminosity to submillimeter luminosity in the 1mm band. The location of an object in this plot should be directly correlated with its blazar “state”, with FSRQs occupying the upper right and BL Lacs the lower left. Flat-spectrum radio quasar 3C 454.3 is the object with the highest submillimeter luminosity in this plot. • BL Lacs and FSRQs do not exhibit significant differences in amplitude of submillimeter vari- ability or characteristic timescale, but our sam- ple of BL Lacs may be dominated by high- peaked BL Lacs (HBLs), which exhibit obser- vational similarities with FSRQs. • Blazar submillimeter light curves are consistent with being produced by a single process that ac- counts for both high and low states, with char- acteristic timescales 10 < τ$_{rest}$ < 500 days. • The blazars detected by Fermi have synchrotron peaks at higher frequencies, regardless of sub- millimeter luminosity. • FSRQs exhibit higher ratios of γ -ray to sub- millimeter luminosity than BL Lacs (Figure 5), but all objects inhabit a region of parameter space suggesting transitions between states dur- ing flaring epochs. As Fermi continues to observe fainter sources, the sample of objects for which we can perform this type of analysis will increase and provide better limits on our results. To understand the physical relevance of these results, however, it is important to be able to distin- guish between the difference in variability between BL Lacs and FSRQs. One avenue for exploring this dif- ference is to monitor changing submillimeter energy spectral index and the ratio of γ -ray to submillime- ter luminosity as functions of time. The full mean- ing of the results of our autoregressive method is not yet clear, and will require better-sampled blazar light curves and the comparison between τ$_{rest}$ with physical timescales such as the synchrotron cooling timescale. These analyses would allow us to place constraints on the processes occurring near the base of the jet in blazars and further understand the intimate connec- tion between them. This work was supported in part by the NSF REU and DoD ASSURE programs under Grant no. 0754568 and by the Smithsonian Institution. Par- tial support was also provided by NASA contract NAS8-39073 and NASA grant NNX07AQ55G. We have made use of the SIMBAD database, operated at CDS, Strasbourg, France, and the NASA/IPAC Ex- tragalactic Database (NED) which is operated by the JPL, Caltech, under contract with NASA. Acknowledgments eConf C091122