Galaxy Evolution & Black-Hole Growth (review)
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1 Galaxy Evolution & Black-Hole Growth (review) Avishai Dekel The Hebrew University of Jerusalem & UCSC Delivered by Fangzhou Jiang Dali, China, November 2018 See also Claude-Andre s talk and Joel s talk
2 A Characteristic Mass for Galaxy Formation Efficiency of galaxy formation low-mass quenching high-mass quenching Behroozi+ 2013
3 A Characteristic Time Mass for Galaxy Formation Star-formation density high-mass quenching low-mass quenching typical halos at z~2 are ~ M
4 AGN Preferentially in Massive Galaxies z=0.85 AGN AGN log M star > 10.2 log M vir > 12 AGN = rapid growth of BH? stars SF z=0.2 BPT Vitale+13 zcosmos Kauffmann+04 SDSS
5 Why do galaxies like to form at the magic mass (and time)? Why do black holes grow rapidly once their host galaxies are above the magic mass (and time)?
6 A Characteristic Mass for Galaxies and BHs M star ~ M M vir ~10 12 M V vir ~100 km/s - Supernova feedback efficient at M<M crit (V crit ) Larson 74, Dekel & Silk 86 - Hot CGM (virial shock heating) at M>M crit Rees & Ostriker 77, Silk 77, Binney 77, Dekel & Birnboim 06 -> Compaction to Blue Nuggets + quenching at ~M crit (any z) Zolotov+15, Tacchella+16, Dekel+18 -> Black Holes suppressed by supernovae at M<M crit, Black hole growth at M>M crit Driven by compaction -> Quenching of star formation at M>M crit triggered by compaction, maintained by hot halo & black hole
7 1. Supernova Fdbk Scale V vir ~100 km/s Dekel & Silk 86 Energy fed to ISM by SN bubble before fading: E SN M V V 2 SN, SN 120 km/s Energy for ejecting gas from the galaxy potential well: 2 2 E M V V = gas gas vir, vir GM R E SN ~ E gas and M * ~M gas at peak efficiency of SFR --> An upper limit for effective SN feedback: 11 Vvir, SN 120 km/s M vir, SN 7 10 M (at z = 0)
8 2. Hot CGM Mass: shutdown of cold gas supply Dekel & Birnboim 06, Rees & Ostriker 77, Silk 77, Binney 77 Critical halo mass ~ M ʘ 1 1 t cool < t compress slow cooling -> shock log T Kravtsov+
9 M crit by SN Fdbk & Hot CGM : M vir ~ M M vir [M ʘ ] hot CGM hot CGM cold streams shock heating Dekel & Birnboim cold CGM Dekel & Silk 86 typical halos Press & Schechter redshift z
10 3. Wet Compaction to Blue Nuggets Dekel & Burkert 14, Zolotov+15, Tacchella+16a,b, Dekel, Lapiner+18 See Joel s talk VELA simulations Red Nugget Blue Nugget
11
12 vela v2 07 gas + young stars wet compaction max density core: blue nugget vdi disk core depletion: a hole and a ring
13 vela v2 07 stars wet compaction max density core: blue nugget green nugget red nugget + envelope
14 Compaction -> quenching in the inner 1 kpc M 10 1 kpc dark matter stars gas 8 diffuse compaction quenching star-formation rate 2 M 0 time
15 Compaction and Quenching in Simulations star forming diffuse blue nugget quenched L-shape track red nugget Zolotov+15 Tacchella+16 Dekel+17 diffuse compact
16 Observed L-Shape Track Barro+17 compaction BN quenching
17 Blue Nugget --> Red Nugget gas stars gas stars blue nugget red nugget dense gas core -> dense stellar core gas depletion from core, gas ring may form, -> inside-out quenching stellar core remains dense from BN to RN
18 What is the Trigger of wet Compaction? Drastic loss of angular momentum - Mergers (major, minor) (Barnes, Hernquist 91; Hopkins+ 06) - VDI-driven inflow (Dekel, Burkert 15) - Counter-rotating streams (Danovich+ 15) - Tidal compression (Dekel+ 03; Renaud+ 14; Mandelker+ 16) - Triaxial halo core (Ceverino+ 15; Tomassetti+ 16) - Return of recycled low-am gas (Elmegreen+ 14; DeGraf+ 16)
19 A Critical Mass for Blue Nuggets (at all z) M star ~10 10 M M vir ~ M Hot CGM SN fdbk Origin of BN scale? SN fdbk + hot CGM
20 Deep Learning: BNs intheory vs Observations Huertas-Company+ 18 See Joel s talk Pre BN Blue Nugget Post BN Identify BNs in 3D simulations (gas, stars) Train CNN on mock images of simulations Classify BNs in HST images
21 Blue Nuggets at a Magic Mass in CANDELS Deep Learning: Huertas-Company+ 18 Luminosity (mass) eliminated
22 Transition in Galaxy Properties at the BN - Diffuse -> compact core + extended disk - Star forming -> quenched - Oscillations across the Main Sequence -> quenching - Dark-matter -> baryon dominated core - Prolate -> oblate stellar system - V/s~1 -> V/s~4, dispersion -> rotation dominated -
23 Transition of Shape: Prolate to Oblate Ceverino+ 15 Tomassetti+ 16 Shape M B /M DM Pre-BN, M * < M, DM-dominated -> prolate assembly along filament anisotropic dispersion Post-BN baryon-dominated -> box orbits deflected -> oblate, rotation-dominated
24 4. Compaction and Black-Hole Growth Dekel, Lapiner, Dubois
25 Interplay between SNe and BHs RAMSES Simulation SN+BH by Dubois+ 15 z=3.60 z=3.44 no SN merger with SN merger compaction time - M<M crit : strong SN fdbk suppresses BH growth - Compaction overcomes SNe -> rapid BH growth
26 Compaction driving BH Growth New Horizon simulations SN+BH Dubois+ Lapiner+ stars stars 1kpc compaction gas 1kpc BHx10 4 DM 1kpc BH growth gravity r BH
27 Compaction driving BH Growth New Horizon simulations SN+BH Dubois+ Lapiner+
28 BH Below the Linear Relation for M BH ~10 5 M New Horizon Sims Lapiner+ See also Claude-Andre s talk BN
29 Magic Mass for BH is Robust in Simulations EAGLE Bower+ 16 Illustris TNG Habouzit+18 no SN w SN FIRE Angles-Alcazar+17
30 Compaction-Driven BH Growth
31 BH Growth by Compaction at M vir ~ M - M vir < M crit, pre-compaction SN phase: V esc < 100 km/s -> SN winds of 100 km/s escape and evacuate the core -> BH growth is suppressed, BN formation is suppressed - M vir ~ M crit, major compaction overcoming SN fdbk: The compressed gas activates rapid BH growth - M vir > M crit, post-compaction hot CGM phase: V esc > 100 km/s -> SN winds are bound (by halo potential and hot gas) -> gas falls back in -> BH growth continues -> AGN self-regulates with the accretion, AGN fdbk keeps the CGM hot and suppresses SFR long term
32 Observed High Fraction of AGN in BN Pase Kocevski+17 CANDELS SFR RN diffuse BN comactnesss -> Compaction triggers BH growth and AGN -> quenching
33 AGN Activation at the Critical Mass Forster-Schreiber+18 KMOS 3D z= galaxies
34 Fraction of AGN dm/dt L L = 0.1 dm bh /dt c 2 simulations BH accretion rate L= KMOS 3D New Horizon sims
35 AGN Correlate with Compactness Forster-Schreiber+18 KMOS 3D z= galaxies incidence M * = M * =
36 AGN Correlate with Mass and ssfr: Blue Nugget Phase Forster-Schreuer+18 KMOS 3D z= galaxies Blue Nuggets
37 A Characteristic Mass for Galaxies and BHs M star ~ M M vir ~10 12 M V vir ~100 km/s - Supernova feedback efficient at M<M crit (V crit ) Larson 74, Dekel & Silk 86 - Hot CGM (virial shock heating) at M>M crit Rees & Ostriker 77, Silk 77, Binney 77, Dekel & Birnboim 06 -> Compaction to Blue Nuggets + quenching at ~M crit (any z) Zolotov+15, Tacchella+16, Dekel+18 -> Black Holes suppressed by supernovae at M<M crit, Black hole growth at M>M crit Driven by compaction -> Quenching of star formation at M>M crit See Tao s talk triggered by compaction, maintained by hot halo & black hole
38 Interplay between Galaxies and Central Region Mpc kpc cosmic web gal halo gal core cold streams + mergers, streams + compaction Blue Nugget - hot CGM + pc SF, SN SF - SN - + SF SF trigger SF - maintain <<pc BH BH BH growth AGN M crit mass
39 M crit by SN Feedback: M vir ~ M hot CGM SF quenching hot CGM M vir [M ʘ ] BH growth cold streams shock heating Dekel & Birnboim SN-suppressed SF SN-suppressed BH typical halos redshift z Dekel & Silk 86 Press & Schechter 74
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