The Monster Roars: AGN Feedback & Co-Evolution with Galaxies
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1 The Monster Roars: AGN Feedback & Co-Evolution with Galaxies Philip Hopkins
2 Ø (Nearly?) Every massive galaxy hosts a supermassive black hole Ø Mass accreted in ~couple bright quasar phase(s) (Soltan, Salucci+, Tremaine+, Yu & Lu, PFH, Shankar, et al.)
3 BHs and Bulges Co-evolve McConnell et al.
4 Problems? Oppenheimer & Dave Number Density Observed No AGN FB Spheroid & BH Formation Times: Ø Ø Ø Sharp color bimodality Lowering mass of >M* galaxies Removing/heating gas in groups Marconi et al.
5 Quasar Feedback as a Means to Regulate BHs SANDERS 88, SILK & REES 98, MURRAY ET AL. 05, MANY MORE
6 Quasar Feedback as a Means to Regulate BHs SANDERS 88, SILK & REES 98, MURRAY ET AL. 05, MANY MORE F rad L c M BH c t Salpeter
7 Quasar Feedback as a Means to Regulate BHs SANDERS 88, SILK & REES 98, MURRAY ET AL. 05, MANY MORE F rad L c M BH c t Salpeter F grav GM gal M gas R 2 gal f gas 4 G
8 Quasar Feedback as a Means to Regulate BHs SANDERS 88, SILK & REES 98, MURRAY ET AL. 05, MANY MORE F rad L c M BH c t Salpeter F grav GM gal M gas R 2 gal f gas 4 G Shut down accretion when: F rad & F grav
9 Quasar Feedback as a Means to Regulate BHs SANDERS 88, SILK & REES 98, MURRAY ET AL. 05, MANY MORE F rad L c M BH c t Salpeter F grav GM gal M gas R 2 gal f gas 4 G Shut down accretion when: F rad & F grav M BH f gas t S Gc M 200 km s 1 4
10 Star Formation BH Growth
11
12 BAL Winds on ~1pc - 1kpc scales: Wada et al. No BAL Winds With BAL Winds Ṁ launch (0.1 pc) = 0.5 ṀBH v launch (0.1 pc) = 10, 000 km/s
13 M-sigma Suggests Self-Regulated BH Growth FEEDBACK PREVENTS RUNAWAY BLACK HOLE GROWTH Black hole growth without feedback with feedback Di Matteo et al., PFH et al. 2005
14 Predictions? MBH- evolution: Hosts more gas rich/compact at high-z more work for the BH before self-regulation PFH, Murray et al Size evolution of spheroid hosts Corresponding increase in M BH /M host Doesn t mean that BHs grew before their hosts PFH et al. 2006, 2007
15 Co-Evolution falls out naturally: Downsizing in BHs and Galaxies is the same: BH accretion rate (x1000) BH mass of an L* QSO SFR (points) PFH, Richards, & Hernquist 2007 Merloni et al Ø Provided self-regulation exists, average correlations are independent of fueling
16 Helps Ensure Ellipticals are Red and Dead Gas Density Springel et al Gas Temperature No AGN Feedback With AGN Feedback
17 Feedback-Driven Winds METAL ENRICHMENT & BUILDING THE X-RAY HALO X-Ray Emission Cox et al. 2005
18 Quasar Outflows May Be Significant for the ICM & IGM SHUT DOWN COOLING FOR ~ COUPLE GYR. PRE-HEATING? McCarthy et al., Schaye et al with AGN feedback without AGN feedback simulated vs. observed profiles
19 AGN or Starburst-Driven Winds? WHICH ARE MORE IMPORTANT? BHs Dominate Feedback Stars Dominate Feedback Halo Mass [Msun]
20 AGN or Starburst-Driven Winds? WHICH ARE MORE IMPORTANT? Efficient star formation Inefficient star formation BHs Dominate Feedback Stars Dominate Feedback Halo Mass [Msun]
21 AGN or Starburst-Driven Winds? WHICH ARE MORE IMPORTANT? Efficient star formation Inefficient star formation BHs Dominate Feedback Stars Dominate Feedback Halo Mass [Msun] How is this inefficient star formation *maintained*?
22 Transition Ø Quasar mode (high mdot) Ø Move mass from Blue to Red? Ø Rapid (~10 7 yr) Ø Small(er) scales (~pc-kpc) Ø Gas-rich/Dissipational Mergers? Ø Regulates Black Hole Mass vs. Maintenance Ø Radio mode (low mdot) Ø Keep it Red Ø Long-lived (~Hubble time) Ø Large (~halo) scales Ø Hot Halos & Dry Mergers Ø Regulates Galaxy Mass
23 Maintenance Mode IS IT ALSO RADIO -MODE? Ho: P(radio) versus Eddington ratio: Allen: P(jet) versus P(accretion): Observational constraints on the power involved are leading the way
24 Maintenance Mode IS IT ALSO RADIO -MODE? Know that (non-cooling flow) clusters do look pre-heated... but we also see radio jets doing work: What is typical? Allen (X-ray Ellipticals) Fabian (Perseus Cluster)
25
26
27 Dead Bulges (stellar wind/hot gas halo accretion) Seyferts (disk-dominated, secular/minor mergers) Fading Mergers (post-starburst spheroids) Log(Number Density) Seyferts Quasars Blowout (Bright Mergers) Log(L/L sun ) Ø Observed luminosity function: populations at different evolutionary stages
28 Where to From Here?
29 Step 1: Stellar Feedback & the ISM sub-grid ISM = cutting-edge analytic models multi-phase ISM with outflows ESA
30 Step 1: Stellar Feedback & the ISM sub-grid ISM = cutting-edge analytic models multi-phase ISM with outflows Ø Non-linear QSO-Stellar feedback interactions matter ESA
31 Step 2: Inflow R < 0.1 pc: ~ few M yr -1 Ø Beginning to directly follow inflow to sub-pc scales Mayer, Callegari, 09,10 Levine, Gnedin, Kravtsov 09,10 PFH & Quataert 2009,10,11
32 Step 2: Inflow R < 0.1 pc: ~ few M yr -1 Ø Beginning to directly follow inflow to sub-pc scales Mayer, Callegari, 09,10 Levine, Gnedin, Kravtsov 09,10 PFH & Quataert 2009,10,11 Ø NOT: Ø Bondi-Hoyle Ø Viscous ( -Disk)
33 (PFH & Quataert 2010) Bars w/in Bars (Shlosman et al. 1989) It s Bars all the Way Down...
34 (PFH & Quataert 2010) Bars w/in Bars (Shlosman et al. 1989) It s Bars all the Way Down... More accurately... It s Non-axisymmetric Features all the Way Down...
35 (PFH & Quataert 2010) Bars w/in Bars (Shlosman et al. 1989) It s Bars all the Way Down... More accurately... It s Non-axisymmetric Features all the Way Down... Derive Instability Rate: Ṁ 10 M yr 1 Disk Total 5/2 1/6 M BH, 8 M gas, 9 R 3/2 0,100
36 Step 3: Observed Sources of AGN Feedback Fabian (Perseus Cluster) Jets heat IGM/ICM (low-density), but not dense ISM?
37 Step 3: Observed Sources of AGN Feedback Jets heat IGM/ICM (low-density), but not dense ISM Radiation Pressure LAGN >> Lstars Roth, Kasen, Quataert, PFH in prep
38 Step 3: Observed Sources of AGN Feedback Jets heat IGM/ICM (low-density), but not dense ISM Radiation Pressure LAGN >> Lstars Accretion Disk Winds Broad Absorption Line Winds Proga et al., Novak et al. Roth, Kasen, Quataert, PFH in prep
39
40 Put all of this into a cosmological simulation, and... (?)
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