Abstract
We summarize what large surveys of the contemporary Universe have taught
us about the physics and phenomenology of the processes that link the
formation and evolution of galaxies with their central supermassive
black holes. We present a picture in which the population of active
galactic nuclei (AGNs) can be divided into two distinct populations. The
radiative-mode AGNs are associated with black holes (BHs) that produce
radiant energy powered by accretion at rates in excess of ˜1% of
the Eddington limit. They are primarily associated with less massive BHs
growing in high-density pseudobulges at a rate sufficient to produce the
total mass budget in these BHs in ˜10 Gyr. The circumnuclear
environment contains high-density cold gas and associated star
formation. Major mergers are not the primary mechanism for transporting
this gas inward; secular processes appear dominant. Stellar feedback is
generic in these objects, and strong AGN feedback is seen only in the
most powerful AGNs. In jet-mode AGNs the bulk of energetic output takes
the form of collimated outflows (jets). These AGNs are associated with
the more massive BHs in more massive (classical) bulges and elliptical
galaxies. Neither the accretion onto these BHs nor star formation in
their host bulge is significant today. These AGNs are probably fueled by
the accretion of slowly cooling hot gas that is limited by the
feedback/heating provided by AGN radio sources. Surveys of the
high-redshift Universe paint a similar picture. Noting that the
volume-averaged ratio of star formation to BH growth has remained
broadly constant over the past 10 Gyrs, we argue that the processes that
linked the cosmic evolution of galaxies and BHs are still at play today.
| Original language | English |
|---|---|
| Pages (from-to) | 589-660 |
| Journal | Annual Review of Astronomy and Astrophysics |
| Volume | 52 |
| Publication status | Published - 1 Aug 2014 |