Measuring the black hole masses of high redshift quasars

Details Measuring the black hole masses of high redshift quasars Measuring the black hole masses of high redshift quasars

2002-04-27

arxiv.org/abs/astro-ph/0204473v2

Mon.Not.Roy.Astron.Soc.337:109,2002

Astronomy and Astrophysics

Astrophysics

Replaced to address comments of referee and Dan Maoz (astro-ph/0207295). Minor revision of R_{BLR}-Luminosity calibration. Res

Scientific paper

10.1046/j.1365-8711.2002.05871.x

A new technique is presented for determining the black-hole masses of high-redshift quasars from optical spectroscopy. The new method utilizes the full-width half maximum (FWHM) of the low-ionization MgII emission line and the correlation between broad-line region (BLR) radius and continuum luminosity at 3000 Angstroms. Using archival UV spectra it is found that the correlation between BLR radius and 3000 Angstrom luminosity is tighter than the established correlation with 5100 Angstrom luminosity. Furthermore, it is found that the correlation between BLR radius and 3000 Ang luminosity is consistent with a relation of the form $R_{BLR} \propto lambda L_{lambda}^{0.5}$, as expected for a constant ionization parameter. Using a sample of objects with broad-line radii determined from reverberation mapping it is shown that the FWHM of MgII and H beta are consistent with following an exact one-to-one relation, as expected if both H beta and MgII are emitted at the same radius from the central ionizing source. The resulting virial black-hole mass estimator based on rest-frame UV observables is shown to reproduce black-hole mass measurements based on reverberation mapping to within a factor of 2.5 (1 sigma). Finally, the new UV black-hole mass estimator is shown to produce identical results to the established optical (H beta) estimator when applied to 128 intermediate-redshift (0.3

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