Dissipation and Extra Light in Galactic Nuclei. Iv. Evolution in the Scaling Relations of Spheroids

We develop a model for the origins and redshift evolution of spheroid scaling. We consider spheroid sizes, velocity dispersions, masses, profile (Sersic indices), and black hole (BH) masses, and their related. Our approach combines advantages of observational constraints in halo models and hydrodynamic merger simulations. This allows us to the relative roles of dissipation, dry mergers, formation time, and evolution, and identify their effects on scalings at each redshift. is the most important factor determining spheroid sizes and plane (FP) scalings, and can account for the FP tilt and between disk and spheroid scalings. Because disks at high-z have gas fractions, mergers are more gas-rich, yielding more compact. This predicts mass-dependent evolution in spheroid sizes, in with observations. This relates to subtle evolution in the FP, to studies that assume a fixed intrinsic FP. This also predicts mild in BH-host correlations, towards larger BHs at higher z. Dry mergers significant, but only for massive systems which form early: they form, but undergo dry mergers (consistent with observations) such that their at later times are similar to spheroids of similar mass formed more. We model descendants of observed compact high-z spheroids: most will cores of BCGs, with sizes, velocity dispersions, and BH masses with observations, but we identify a fraction that might survive to=0 intact.