1. Stellar & AGN Feedback in Galaxies GLCW8 Columbus 2007

2. Evidence for Feedback (Self-limited Star Formation?) M b ~ 3 M * ~ 4 Krabbe et al astro-ph/0703804

3. Inefficient Star Formation-Feedback? Kennicutt 1998 Implies same physics over 4 decades in gas

4. Evidence for Feedback: Winds- significant mass & momentum in cold gas M82 (Subaru) e.g., Heckman et al. 00; Martin 04,05

5. Evidence for Feedback (self-limiting BH accretion?) Greene & Ho 05

6. Large-Scale Feedback Fabian et al (2006) Perseus Cluster

7. Fabian et al (2006) Perseus Cluster Large-Scale Feedback

8. Feedback Mechanisms Energy Input –Stars (local) SN HII Winds –AGN Via Radiation Jets (large scale) Winds (Broad Absorption Line QSOs) Momentum Input –Stars SN Radiation –AGN Radiation

9. Radiation Pressure Feedback Dust absorbs the radiation produced by starbursts or AGN Dust collisionally coupled to the gas: mfp ~ 1 a 0.1 n 1 pc Starlight provides turbulent pressure support of ISM Momentum-driven wind: V ~ V c L/c M W V L ~ 10 -3 M * c 2 ~ M W V c M W ~ M * Efficient mechanism for blowing cold dusty gas out of a galaxy (i.e, couples to the phase of the ISM with most of the mass) · ····

10. Terminal Velocity of Outflowing Cold Gas Data from Martin (2005) V term ~ 2.5 ~ V esc ULIRGs LIRGs Dwarfs Hot gas inferred to have V hot ~ 500 km/s independent of Ram pressure in hot wind V term ~ V hot ~ 500 km/s L ~ L EDD V term ~

11. The Maximum Luminosity of Starbursts

12. Black Holes Efficient angular momentum transport in mergers can trigger BH growth and AGN activity Dust present outside R sub ~ 1 L 1/2 46 pc If L L M, AGN can blow dusty gas out of its vicinity, controlling its own fuel supply 1/2

13. The Maximum Luminosity of Quasars from width of OIII line in NLR

14. The Origin of the M- Relation? Inside R sub ~ 1 L 46 pc, dust destroyed Normal optically thin Eddington limit applies With sufficient fuel supply, L ~ L EDD M BH As BH grows, L L M 4 1/2

15. Is the BH or Stellar Feedback Responsible for the Bulk of the Gas Removal? L * =4f g 4 c/G seen; implies radiation limited (not BH limited) star formation rate Winds are seen; if massive enough, Faber-Jackson follows. Not blown by AGN BH is affected by but not f g ; fine tuning required to arrange for Faber-Jackson See ongoing star formation in ellipticals (at low level)- -no supression of star formation in situ But AGN feedback likely restricts mass accretion from large radii

16. Feedback in Galactic Disks Marginally Stable: H/R~v T /v c roughly constant Stars form in molecular gas dN/dM~ M -1.8 => mass in big clouds Most stars form in Giant Molecuar Clouds

17. Clumps and Star Clusters IRDCs: dN/dM~M -1.97 (Simon et al. ApJ 2006) Clumps: dN/dM~M -1.8 Molecular Cloud Cores dN/dM~ -1.7 (Lada, Bally & Stark 1991) Clusters: dN/dM~M -2 (Lada & Lada 2003) => Most stars form in massive clusters

18. Carina Mass GMC ~ 5x10 5 Solar masses Radius GMC ~ 40pc L=2.5x10 7 L sun (~10 41 erg/s) –70% from Trumpler 16, 16% from Tr 14 –R cl ~ 2pc X-rays consistent with standard IMF

19. Clumps in Carina

20. Forces Acting In Carina Inward –Self-Gravity of shell -GM sh (R) M sh (R)/R 2 –Turbulent pressure 4 r 2 v T 2 –Ram pressure 4 r 2 v sh 2 Outward –HII gas pressure 4 r 2 nkT = 4 r 2 (3Q/4 r 3 ) 1/2 kT –Radiation pressure (1+ )L/c, <1 –Jet ram pressure dM/dt v jet

21. Dynamical Model (1D)

26. Summary (Local Feedback) Star formation is observed to be inefficient Scaling relations imply a single mechanism SN too late to halt SF in Starbursts/ULIRGS HII helps in MW, not in ULIRGS Stellar Winds seem ineffective Radiation pressure on dust can work