Abstract
High resolution, deep imaging surveys are instrumental in setting constraints on semi-analytical structure formation models in Cold Dark Matter (CDM) cosmologies. We show here that the lack of unresolved B-band ``dropouts'' with V > 25 mag in the Hubble Deep Field (HDF) appears to be inconsistent with the expected number of quasars if massive black holes form with a constant universal efficiency in all CDM halos. To reconcile the models with the data, a mechanism is needed that suppresses the formation of quasars in halos with circular velocities v(circ) 5 objects per field or provide even stronger constraints on the models than existing B, V, and I data.
Highlights
One of the primary goals of models for structure formation in the universe is to explore the formation process of luminous objects such as quasars or galaxies and to explain the shape and evolution of their observed luminosity functions (LFs)
Recent theoretical work has focused on the formation of galaxies within the framework of hierarchical structure formation in cold dark matter (CDM) cosmologies, employing either three-dimensional numerical simulations (Gnedin & Ostriker 1997 ; Zheng et al 1997) or semianalytic modeling (Kau†man, Guiderdoni, & White 1994 ; Cole et al 1994 ; Baugh et al 1998 ; Somerville & Primack 1998 ; Haiman & Loeb 1997, hereafter HL97)
The existing data on the LF only constrains the individual quasar model pz a[ra3m.5etneurms sbuecrhcoaus nvtQs aanredptr0edtoicwteidthtion a factor of D2, the a much better accuracy, since the model is calibrated by simultaneously adjustirnegsuvltQ, aanndotv0ertporerdepicrtoiodnucoef the quasar LF at z D 3. the miniquasar counts
Summary
One of the primary goals of models for structure formation in the universe is to explore the formation process of luminous objects such as quasars or galaxies and to explain the shape and evolution of their observed luminosity functions (LFs). Recent theoretical work has focused on the formation of galaxies within the framework of hierarchical structure formation in cold dark matter (CDM) cosmologies, employing either three-dimensional numerical simulations (Gnedin & Ostriker 1997 ; Zheng et al 1997) or semianalytic modeling (Kau†man, Guiderdoni, & White 1994 ; Cole et al 1994 ; Baugh et al 1998 ; Somerville & Primack 1998 ; Haiman & Loeb 1997, hereafter HL97) These calculations have been quite successful in reproducing the observed Tully-Fisher relation in the local universe, the faint galaxy LFs out to moderately high redshifts z [ 3, and the recently discovered clustering of Lymanbreak galaxies at z D 3 (Baugh et al 1998 ; Governato et al 1998 ; Steidel et al 1998). The trapezoidal region selects objects with z Z 4.5
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