The Ultraviolet-to-Mid-Infrared Spectral Energy Distribution of Weak
  Emission Line Quasars
  We present Spitzer Space Telescope photometry of 18 Sloan Digital Sky Survey
(SDSS) quasars at 2.7 <= z <= 5.9 which have weak or undetectable
high-ionization emission lines in their rest-frame ultraviolet (UV) spectra
(hereafter weak-lined quasars, or WLQs). The Spitzer data are combined with
SDSS spectra and ground-based, near-infrared (IR) photometry of these sources
to produce a large inventory of spectral energy distributions (SEDs) of WLQs
across the rest-frame ~0.1-5 mum spectral band. The SEDs of our sources are
inconsistent with those of BL Lacertae objects which are dominated by
synchrotron emission due to a jet aligned close to our line-of-sight, but are
consistent with the SED of ordinary quasars with similar luminosities and
redshifts that exhibit a near-to-mid-IR 'bump', characteristic of hot dust
emission. This indicates that broad emission lines in WLQs are intrinsically
weak, rather than suffering continuum dilution from a jet, and that such
sources cannot be selected efficiently from traditional photometric surveys.
