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Abstract
We compare observed clustering of quasars and galaxies as a function of redshift, mass, luminosity, & color/morphology, to constrain models of quasar fueling and spheroid-BH co-evolution. High redshift quasars are shown to be drawn from progenitors of local early-type galaxies, with the characteristic quasar luminosity L* reflecting a characteristic mass of 'active' BH/host populations at each redshift. Evolving observed high-z quasar clustering to z=0 predicts a trend of clustering in 'quasar remnants' as a function of stellar mass identical to that observed for early-types. However, quasar clustering does not simply reflect observed early (or late)-type populations; at each redshift, quasars cluster as an 'intermediate' population. Comparing with the age of elliptical stellar populations reveals that this 'intermediate' population represents those ellipticals undergoing or terminating their final significant star formation at each epoch. Assuming that quasar triggering is associated with the formation/termination epoch of ellipticals predicts quasar clustering at all observed redshifts without any model dependence or assumptions about quasar light curves, lifetimes, or accretion rates. This is not true for disks or quasar halos: i.e. quasars do not generically trace star formation, disks, or halo assembly. Quasar clustering at all z is consistent with a constant halo mass ~4x10^{12} M_sun, similar to local 'group scales.' The observations support a scenario in which major mergers trigger quasar activity and dominate bright, high-z quasar populations. We show that measurements of quasar clustering versus luminosity at z~1 can be used to constrain different lower-luminosity AGN fueling mechanisms, and that high-z clustering is sensitive to whether or not systems 'shut down' growth at z>3.
Highlights
In recent years, it has become clear that essentially all galaxies harbor supermassive black holes (BHs) (e.g., Kormendy & Richstone 1995), the masses of which are correlated with many properties of their host spheroids, including luminosity, mass (Magorrian et al 1998), velocity dispersion (Ferrarese & Merritt 2000; Gebhardt et al 2000), concentration and Sersic index (Graham et al 2001)
High redshift quasars are shown to be drawn from the progenitors of local early-type galaxies, with the characteristic quasar luminosity L∗ at a given redshift reflecting a characteristic mass of the “active” BH/host population at that epoch
It has become clear that essentially all galaxies harbor supermassive black holes (BHs) (e.g., Kormendy & Richstone 1995), the masses of which are correlated with many properties of their host spheroids, including luminosity, mass (Magorrian et al 1998), velocity dispersion (Ferrarese & Merritt 2000; Gebhardt et al 2000), concentration and Sersic index (Graham et al 2001)
Summary
It has become clear that essentially all galaxies harbor supermassive black holes (BHs) (e.g., Kormendy & Richstone 1995), the masses of which are correlated with many properties of their host spheroids, including luminosity, mass (Magorrian et al 1998), velocity dispersion (Ferrarese & Merritt 2000; Gebhardt et al 2000), concentration and Sersic index (Graham et al 2001). Wide-field surveys such as the Two Degree Field (2dF) QSO Redshift Survey (2QZ; Boyle et al 2000) and the Sloan Digital Sky Survey (SDSS; York et al 2000) have enabled tight measurements of quasar clustering to redshifts z ∼ 3, and a detailed breakdown of galaxy clustering as a function of galaxy mass, luminosity, color, and morphology (e.g., Norberg et al 2002; Zehavi et al 2002; Li et al 2006) These observations allow us to consider the possible triggering mechanisms of quasars in a robust, empirical manner, and answer several key questions. Small fields in galaxy surveys limit one’s ability to measure clustering as a bivariate function of luminosity and color/morphology at the highest luminosities, where the relics of z ∼ 2 − 3 quasars are expected
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