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| Paper: |
Quenching Models: Their Interplay and Degeneracies |
| Volume: |
399, Panoramic Views of Galaxy Formation and Evolution |
| Page: |
405 |
| Authors: |
Hopkins, P.F. |
| Abstract: |
Semi-analytic models invoke a variety of prescriptions to explain “quenching” of red galaxies. We compare a variety of these models, in which quenching is primarily driven by different processes: halo mass (accretion shocks and the transition to “hot accretion”), secular processes and disk instabilities, and major mergers between galaxies. These models can be equally successful at reproducing some observables, in particular the z = 0 galaxy mass functions and their evolution with redshift, and the local fraction of “quenched” galaxies as a function of mass. There are, however, unique and robust qualitative predictions for a number of observables, including the bivariate red fraction as a function of galaxy and halo mass, the density of passive galaxies at high redshifts, the emergence/evolution of the color-morphology-density relations at high redshift, and the fraction of disky/boxy (or cusp/core) spheroids as a function of mass. In each case, the observations favor models more complex than pure halo processes, although this may still be the primary driver of evolution (with contributions from other mechanisms playing a secondary role). |
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