Reaching the Peak of the Quasar Spectral Energy Distribution I:
  Observations and Models
  We perform a spectral analysis of a sample of 11 medium redshift (1.5 < z <
2.2) quasars. Our sample all have optical spectra from the SDSS, infrared
spectra from GNIRS and TSPEC, and X-ray spectra from XMM-Newton. We first
analyse the Balmer broad emission line profiles which are shifted into the IR
spectra to constrain black hole masses. Then we fit an energy-conserving, three
component accretion model of the broadband spectral energy distribution (SED)
to our multi-wavelength data. Five out of the 11 quasars show evidence of an
SED peak, allowing us to constrain their bolometric luminosity from these
models and estimate their mass accretion rates. Based on our limited sample, we
suggest that estimating bolometric luminosities from L_5100A and L_2-10keV may
be unreliable, as has been also noted for a low-redshift, X-ray selected AGN
sample.
