Evaluating and Improving the Redshifts of z>2.2 Quasars
  Quasar redshifts require the best possible precision and accuracy for a
number of applications, such as setting the velocity scale for outflows as well
as measuring small-scale quasar-quasar clustering. The most reliable redshift
standard in luminous quasars is arguably the narrow [OIII]
$\lambda\lambda$4959,5007 emission line doublet in the rest-frame optical. We
use previously published [OIII] redshifts obtained using near-infrared spectra
in a sample of 45 high-redshift (z > 2.2) quasars to evaluate redshift
measurement techniques based on rest-frame ultraviolet spectra. At redshifts
above z = 2.2 the MgII $\lambda$2798 emission line is not available in
observed-frame optical spectra, and the most prominent unblended and unabsorbed
spectral feature available is usually CIV $\lambda$1549. Peak and centroid
measurements of the CIV profile are often blueshifted relative to the
rest-frame of the quasar, which can significantly bias redshift determinations.
We show that redshift determinations for these high-redshift quasars are
significantly correlated with the emission-line properties of CIV (i.e., the
equivalent width, or EW, and the full width at half maximum, or FWHM) as well
as the luminosity, which we take from the Sloan Digital Sky Survey Data Release
7. We demonstrate that empirical corrections based on multiple regression
analyses yield significant improvements in both the precision and accuracy of
the redshifts of the most distant quasars and are required to establish
consistency with redshifts determined in more local quasars.
