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  **1. INTRODUCTION**
  
  The timescales on which high-amplitude ﬂaring 
  events occur in blazars indicate that much of the en- 
  ergy is being produced deep within the jet on small, 
  sub-parsec scales [1, 2]. Understanding if/how emis- 
  sion diﬀers between blazar subclasses (i.e., BL Lacs 
  objects and ﬂat-spectrum radio quasars (FSRQs)) 
  may oﬀer important insight into the similarity be- 
  furthermore, can provide con- 
  tween blazars and, 
  straints on the formation and acceleration of the jets 
  themselves. 
  
  **2. SMA BLAZARS**
  
  The Submillimeter Array [4] consists of eight 6 m 
  antennas located near the summit of Mauna Kea. The 
  SMA is used in a variety of baseline conﬁgurations 
  and typically operates in the 1mm and 850µm win- 
  dows, achieving spatial resolution as ﬁne as 0.25” at 
  850µm. The sources used as phase calibrators for the 
  array are compiled in a database known as the SMA 
  Calibrator List2 [5]. Essentially a collection of bright 
  objects (stronger than 750 mJy at 230 GHz and 1 Jy 
  at 345 GHz), these sources are monitored regularly, 
  both during science observations and dedicated ob- 
  serving tracks. 