# The Intermediate-ionization Lines as Virial Broadening Estimators for Population A Quasars

DOI:
10.3847/1538-4365/ac6fd6
Publication date:
08/08/2022
Main author:
Marziani, Paola
IAA authors:
Authors:
Marziani, Paola;Olmo, Ascensión del;Negrete, C. Alenka;Dultzin, Deborah;Piconcelli, Enrico;Vietri, Giustina;Martínez-Aldama, Mary Loli;D'Onofrio, Mauro;Bon, Edi;Bon, Natasa;Deconto Machado, Alice;Stirpe, Giovanna M.;Buendia Rios, Tania Mayte
Journal:
The Astrophysical Journal Supplement Series
Refereed:
Yes
Publication type:
Article
Volume:
261
Pages:
30
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 H I Balmer H β line width to the ones of two intermediate-ionization lines: the Al III λ1860 doublet and the C III] λ1909 line, over a wide interval of redshift and luminosity (0 ≲ z ≲ 3.5; $43\lesssim \mathrm{log}L\lesssim 48.5$ [erg s<SUP>-1</SUP>]), for 48 sources belonging to the quasar population characterized by intermediate to high values of the Eddington ratio (Population A). The present analysis indicates that the line widths of Al III λ1860 and H β are highly correlated and can be considered equivalent for most Population A quasars over five orders of magnitude in luminosity; for C III] λ1909, multiplication by a constant correction factor ξ ≍ 1.25 is sufficient to bring the FWHM of C III] in agreement with that of H β. 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 kilometers per second) with respect to the quasar rest frame and an excess (≲1.1) Al III broadening with respect to H β are found in a fraction of our sample. Scaling laws to estimate M <SUB>BH</SUB> of high-redshift quasars using the Al III and C III] line widths have rms scatter ≍0.3 dex. The Al III scaling law takes the form $\mathrm{log}{M}_{\mathrm{BH}}\approx 0.58\mathrm{log}{L}_{\mathrm{1700,44}}+2\mathrm{logFWHM}+0.49$ [M <SUB>⊙</SUB>]. *Based in part on observations made with ESO Telescopes at the Paranal Observatory under programs 082.B-0572(A) and 083.B-0273(A).
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