quenching and structural & morphological evolution: physics

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1 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 New Haven

2 specific star formation rate star-forming quiescent disks slow track? spheroids fast track based on Barro et al. extended compactness compact

3 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 redshift

4 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 Illustris simulation (**not on same color scale) Brennan et al semi-analytic model

5 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

6 Barro et al. 2014

7 Semi-analytic models reproduce evolution in the Barro diagram w/ Viraj Pandya & Ryan Brennan SAM log ssfr color=sersic CANDELS observations compactness

8 theoretical picture: see discussion in Barro et al. 2013, 2014; also Naab et al. 2009; Hilz et al. 2013; Porter, rss et al 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

9 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 work in prep w/ rss, Naab, J. Ostriker, Oser, Hu, Moster

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11 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

12 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

13 work in progress mock HST/JWST image library (merger, isolated, & cosmological zooms with pc 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

14 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

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