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We present quasar bolometric corrections using the [O III] $\lambda5007$narrow emission line luminosity based on the detailed spectral energydistributions of 53 bright quasars at low to moderate redshift($0.0345<z<1.0002$). We adopted two functional forms to calculate$L_{\textrm{iso}}$, the bolometric luminosity determined under the assumptionof isotropy: $L_{\textrm{iso}}=A\,L_{[O\,III]}$ for comparison with theliterature and log$(L_{iso})=B+C\,$log$(L_{[O\,III]})$, which bettercharacterizes the data. We also explored whether "Eigenvector 1", whichdescribes the range of quasar spectral properties and quantifies theirdiversity, introduces scatter into the $L_{[O\,III]}-L_{iso}$ relationship. Wefound that the [O III] bolometric correction can be significantly improved byadding a term including the equivalent width ratio $R_{Fe\,II}\equivEW_{Fe\,II}/EW_{H\beta}$, which is an Eigenvector 1 indicator. Inclusion of$R_{Fe\,II}$ in predicting $L_{iso}$ is significant at nearly the $3\sigma$level and reduces the scatter and systematic offset of the luminosityresiduals. Typically, [O III] bolometric corrections are adopted for Type 2sources where the quasar continuum is not observed and in these cases,$R_{Fe\,II}$ cannot be measured. We searched for an alternative measure ofEigenvector 1 that could be measured in the optical spectra of Type 2 sourcesbut were unable to identify one. Thus, the main contribution of this work is topresent an improved [O III] bolometric correction based on measured bolometricluminosities and highlight the Eigenvector 1 dependence of the correction inType 1 sources.

Updating quasar bolometric luminosity corrections. III. [O III] bolometric corrections