The intermediate-ionization lines as virial broadening estimators for Population A quasars

TL;DR

This study evaluates intermediate-ionization lines Aliii 1860 and Ciii] 1909 as virial broadening estimators for estimating black hole masses in Population A quasars across a wide redshift range, finding strong correlations with H-beta.

Contribution

It demonstrates that Aliii 1860 and Ciii] 1909 lines can reliably estimate black hole masses, extending virial estimators to high-redshift quasars using UV lines.

Findings

Aliii 1860 line width correlates strongly with H-beta.

Ciii] 1909 requires a correction factor to match H-beta.

Scaling laws with ~0.3 dex scatter for black hole mass estimates.

Abstract

The identification of a virial broadening estimator in the quasar UV rest frame suitable for black hole mass computation at high redshift has become an important issue. We compare the HI Balmer H-beta line width to the ones of two intermediate ionization lines: the Aliii 1860 doublet and the Ciii] 1909 line, over a wide interval of redshift and luminosity (0 < z < 3.5; 43 < logL < 48.5 [erg a/]), for 48 sources belonging to the quasar population characterized by mid-to-high values of the Eddington ratio (Population A). The present analysis indicates that the line width of Aliii 1860 and H-beta are highly correlated, and can be considered equivalent for most Population A quasars over five orders of magnitude in luminosity; forCiii] 1909, multiplication by a constant correction factor xi ~ 1.25 is sufficient to bring the FWHM of Ciii] in agreement with the one of H-betaa. The statistical concordance between low-ionization and intermediate-ionization lines suggests that they predominantly arise from the same virialized part of the broad line region. However, blueshifts of modest amplitude (few hundred km /s) with respect to the quasar rest frame and an excess (~ 1.1) Aliii broadening with respect to H-beta are found in a fraction of our sample. Scaling laws to estimate M_BH of high redshift quasar using the Aliii and the Ciii] line widths have rms scatter ~ 0.3 dex. The Aliii scaling law takes the form log M_BH ~ 0.58 log L1700,44 + 2 log FWHM + 0.49 [solar masses].