text: In general, we ﬁnd that in the submillimeter, we 
  are observing these blazars at or near the peak of the 
  synchrotron component (αS ∼ 0), but that Fermi - 
  detected sources have more negative energy spectral 
  indices overall than Fermi -nondetected sources. 
  In 
  Figure 4, we see that while the majority of Fermi 
  blazars are observed on the rising part of the syn- 
  chrotron component (at lower energies than the peak), 
  all of the objects have very steeply falling γ-ray energy 
  spectral indexes, putting the γ-ray peak at lower en- 
  ergies than the observed Fermi band. Knowing that 
  we are not observing the synchrotron and γ-ray com- 
  ponents at analagous points in the spectrum may al- 
  low us to better understand the magnetic ﬁeld in the 
  parsec-scale jet region and the population of external 
  photons that is being upscattered to γ-rays. 
  
  This method yielded some surprising results. 
  In 
  Figure 3, we see that the BL Lacs and FSRQs exhibit 
  virtually no diﬀerence in characteristic timescale, with 