Shedding New Light on Weak Emission-line Quasars in the C iv-H Parameter Space

Weak emission-line quasars (WLQs) are a subset of type 1 quasars that exhibit extremely weak Ly alpha + N v lambda 1240 and/or C iv lambda 1549 emission lines. We investigate the relationship between emission-line properties and accretion rate for a sample of 230 "ordinary" type 1 quasars and 18 WLQs at z < 0.5 and 1.5 < z < 3.5 that have rest-frame ultraviolet and optical spectral measurements. We apply a correction to the H beta-based black hole mass (M (BH)) estimates of these quasars using the strength of the optical Fe ii emission. We confirm previous findings that WLQs' M (BH) values are overestimated by up to an order of magnitude using the traditional broad-emission-line region size-luminosity relation. With this M (BH) correction, we find a significant correlation between H beta-based Eddington luminosity ratios and a combination of the rest-frame C iv equivalent width and C iv blueshift with respect to the systemic redshift. This correlation holds for both ordinary quasars and WLQs, which suggests that the two-dimensional C iv parameter space can serve as an indicator of accretion rate in all type 1 quasars across a wide range of spectral properties.