quenching and structural & morphological evolution: physics rachel somerville Rutgers University with thanks to: Ryan Brennan, Viraj Pandya, Ena Choi Guillermo Barro, Stijn Wuyts, Dale Kocevski, Arjen van der Wel & the CANDELS team Census, Evolution, Physics November 16-19 2015 New Haven
specific star formation rate star-forming quiescent disks slow track? spheroids fast track based on Barro et al. extended compactness compact
SAMs with mergers+di qualitatively reproduce build-up of quiescent galaxies and spheroids seen in CANDELS z~3-0 spheroid growth combination of major+minor mergers and disk instabilities quiescent fraction spheroid-dominated fraction redshift Brennan et al. 2015 redshift
current simulations qualitatively capture the observed correlation between quenching and internal structure in these models, arises from correlation between BH mass and quiescence (Lang et al. 2014; Brennan et al. in prep.) Snyder et al. 2015 Illustris simulation (**not on same color scale) Brennan et al. 2015 semi-analytic model
solid lines: size of disk or spheroid component; dashed: size of composite galaxy semi-analytic model rss, Porter+CANDELS in prep; observations from van der Wel et al. 2014
Barro et al. 2014
Semi-analytic models reproduce evolution in the Barro diagram w/ Viraj Pandya & Ryan Brennan SAM log ssfr color=sersic CANDELS observations compactness
theoretical picture: see discussion in Barro et al. 2013, 2014; also Naab et al. 2009; Hilz et al. 2013; Porter, rss et al. 2014 and references therein specific star formation rate star-forming quiescent disks smooth gas accretion wet merger/ disk instabilities BH fueling spheroids gas removal (and/or strangulation) quenching dry mergers extended internal density compact
Cosmological hydrodynamical zoom-in simulations including AGN feedback (thermal, radiative, and mechanical) 20 halos (1.1E12<M h (z=0)<1.0e13) M sun (8.9E10<M * (z=0)<1.0e12) M sun star and gas particles 6E06 M sun DM particles 3.6E07 M sun size-mass scaling relations size evolution fraction of accreted/in situ all very sensitive to details of stellar and AGN feedback! (and also to numerics) E. Choi et al. 2015+work in prep w/ rss, Naab, J. Ostriker, Oser, Hu, Moster
no AGN feedback incomplete quenching indefinite compaction with AGN-driven winds compactionà quenchingà expansion Choi, rss et al. in prep; rss et al. in prep
example tracks for individual halos from hydro zoom simulations with AGN hosts shown (open stars = bright AGN hosts; boxes=faint AGN hosts) compaction quenching Choi et al. in prep
work in progress mock HST/JWST image library (merger, isolated, & cosmological zooms with 10-100pc resolution) with RT (Sunrise, Powderday) (E. Choi) wind energetics/kinematics in simulations & comparison with direct observations (R. Brennan PhD) updated AGN fueling & feedback physics in SAMs (w/ M. Hirschmann) merger rates & close pair fractions in SAM mock catalogs (R. Brennan) large scale outflows driven by AGN broad-line region winds Ryan Brennan & Ena Choi
summary we have a cartoon picture of the physics that drives quenching, structural & morphological transformation that seems to qualitatively match current observations dissipationà bulge & BH growth à AGN feedback à dry merging next step: understand physical processes (especially AGN feedback) in more detail