Abstract
The discovery of a systematic difference between the redshifts of the emission lines arising from the different ionization zones of broad-line quasar clouds is reported. The C UFscmcapsiv, N UFscmcapsv, C UFscmcapsiii), (Fe,UFscmcapsx), (Fe UFscmcapsxi), and possibly Lyman-..cap alpha.. lines are at a lower redshift than the O UFscmcapsi, Mg UFscmcapsii, and Balmer lines. Comparison with the redshifts of the narrow emission lines shows that it is the high-ionization broad emission lines that are systematically blueshifted by 600 km s/sup -1/. This blueshift together with the high degree of symmetry of the high-ionization lines strongly constrains models of the broad emission line region. The blueshifting of the strongest emission lines readily observable in high-redshift quasars will affect the number of absorption-line systems which appear to have z/sub a/bs> or =z/sub e/m.
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