Evolution of the Black Hole - Bulge Relationship in QSOs
Abstract
QSOs allow study of the evolution of the relationship between black holes in galactic nuclei and their host galaxies. The black hole mass can be derived from the widths of the broad emission lines, and the stellar velocity dispersion (sigma*) of the host galaxy can be inferred from the narrow emission lines. Results based on [OIII] and [OII] line widths indicate that the black hole mass - sigma* relationship, at redshifts up to z ~ 2, is consistent with no evolution or an increase of up to ~ 0.5 dex in black hole mass at fixed sigma*. CO line widths offer an estimate of sigma* for luminous QSOs at high redshifts. The available objects from z ~ 4 to 6 have very massive black holes, \~ 109.5 Msun, but their CO line widths suggest much smaller host galaxies than would be expected by the local black hole mass - sigma* relationship. The most massive black holes must continue to reside in comparatively modest galaxies today, because their number density inferred from QSO statistics exceeds the present-day abundance of proportionally massive galaxies.
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