The evolution of host mass and black hole mass in quasi-stellar objects from the 2dF QSO Redshift Survey

• Published in: Monthly notices of the Royal Astronomical Society 2006-12, Vol.373 (2), p.613-622
• Main Authors: Fine, S., Croom, S. M., Miller, L., Babic, A., Moore, D., Brewer, B., Sharp, R. G., Boyle, B. J., Shanks, T., Smith, R. J., Outram, P. J., Loaring, N. S.
• Format: Article
• Language: English
• Subjects: Astronomy; Astrophysics; Black holes; cosmology: observations; Dark matter; Earth, ocean, space; Evolution; Exact sciences and technology; galaxies: evolution; galaxies: haloes; quasars: emission lines; quasars: general; Red shift
• ISSN: 0035-8711; 1365-2966
• DOI: 10.1111/j.1365-2966.2006.11004.x

We investigate the relation between the mass of supermassive black holes (M BH) in quasi-stellar objects (QSOs) and the mass of the dark matter haloes hosting them (M DH). We measure the widths of broad emission lines (Mg iiλ2798, C ivλ1549) from QSO composite spectra as a function of redshift. These widths are then used to determine virial black hole mass estimates. We compare our virial black hole mass estimates to dark matter halo masses for QSO hosts derived by Croom et al. based on measurements of QSO clustering. This enables us to trace the M BH-M DH relation over the redshift range z= 0.5-2.5. We calculate the mean zero-point of the M BH-M DH relation to be M BH= 108.4±0.2 M⊙ for an M DH= 1012.5 M⊙. These data are then compared with several models connecting M BH and M DH as well as recent hydrodynamical simulations of galaxy evolution. We note that the flux-limited nature of QSO samples can cause a Malmquist-type bias in the measured zero-point of the M BH-M DH relation. The magnitude of this bias depends on the scatter in the M BH-M DH relation, and we re-evaluate the zero-point assuming three published values for this scatter. We create a subsample of our data defined by a constant magnitude interval around L* and find (1 +z)3.3±1.3 evolution in M BH between z∼ 0.5 and 2.5 for typical, L* QSOs. We also determine the Eddington ratios (L/L Edd) for the same subsample and find no significant evolution: (1 +z)−0.4±1.1. Taken at face value, our data suggest that a decrease in active black hole mass since z∼ 2.5 is the driving force behind luminosity evolution of typical, L*, optically selected QSOs. However, we note that our data are also consistent with a picture in which reductions in both black hole mass and accretion rate contribute equally to luminosity evolution. In addition, we find that these evolution results are strongly affected by the virial black hole mass estimators used. Changes to the calibration of these have a significant effect on the evolution results.