Abstract / Description of output
Galaxy bulge luminosity L, black hole mass MBH, and stellar
velocity dispersion σ* increase together in a way
suggesting a close evolutionary relationship. Measurements of the
MBH-σ* relationship as a function of cosmic
time may shed light on the origin of this relationship. Direct
measurements of σ* at high redshift are difficult, and
the width of the narrow emission lines of active galactic nuclei (AGN)
has been proposed as a surrogate for σ*. We investigate
the utility of using σ[OIII] for σ* by
examining host galaxy magnitudes and [O III] line widths for
low-redshift QSOs. For radio-quiet QSOs, σ[OIII] is
consistent in the mean with the value of σ* predicted
by the Faber-Jackson relation. For our limited range of
Lhost, scatter obscures the expected increase of
σ[OIII] with Lhost. However, for a sample of
AGN covering a wide range of measured or inferred σ*,
there is a clear increase of σ[OIII] with
σ*. Radio-loud QSOs on average have
σ[OIII] smaller by 0.1 dex than radio-quiet QSOs of
similar Lhost, at least for luminosities typical of PG QSOs.
Star formation rates in our low-redshift QSOs are smaller than required
in order to maintain the typical observed ratio of bulge mass to black
hole mass.
| Original language | English |
|---|---|
| Pages (from-to) | 89-94 |
| Journal | Astrophysical Journal |
| Volume | 626 |
| DOIs | |
| Publication status | Published - 1 Jun 2005 |