  With their rapid, violent variability and broad featureless continuum
emission, blazars have puzzled astronomers for over two decades. Today blazars
represent the only extragalactic objects detected in high-energy gamma-rays.
Their spectral energy distributions (SEDs) are characteristically
double-humped, with lower-energy emission originating as synchrotron radiation
in a relativistically beamed jet, and higher-energy emission due to
inverse-Compton processes. This has accentuated the biases inherent in any
survey to favor objects which are bright in the survey band, and should serve
as a cautionary note both to those designing new surveys as well as theorists
attempting to model blazar properties. The location of the synchrotron peak
determines which blazar population is dominant at GeV and TeV energies. At GeV
energies, low-energy peaked, high luminosity objects, which have high $L_C/L_S$
ratios, dominate, while at TeV energies, high-energy peaked objects are all
that is seen. I review the differences between low-energy peaked and
high-energy peaked blazars, and models to explain those differences. I also
look at efforts to bridge the gap between these classes with new surveys. Two
new surveys have detected a large population of high-energy peaked emission
line blazars (FSRQ), with properties somewhat different from previously known
objects. This discovery has the potential to revolutionize blazar physics in a
way comparable to the discovery of X-ray selected BL Lacs ten years ago by {\it
Einstein}. I cull from the new and existing surveys a list of $z<0.1$
high-energy peaked blazars which should be targets for new TeV telescopes.
Among these are several high-energy peaked FSRQ.
