1. Gas Dynamics, AGN, Star Formation and ISM in Nearby Galaxies Eva Schinnerer (MPIA) S. Haan, F. Combes, S. Garcia-Burillo, C.G. Mundell, T. Böker, D.S. Meier, E. Emsellem, U. Lisenfeld, D. Downes, D. Calzetti

2. ISM in Nearby Galaxies Why do we care? Star Formation (SF) Active Galactic Nuclei (AGN) Gas Kinematics & ISM Properties PDRs -- Photon Dominated Regions XDRs -- X-ray Dominated Regions Shocks Neutral Gas (Atomic & Molecular) fuel feedback

3. Spiral Arms (i.e. Density Waves) Large-scale Stellar bars Double/Inner/Nuclear Bars nuclear Spiral Density Waves Fueling nearby AGNs (e.g.NUGA - see talk by M. Krips): m=1 modes warps viscosity … Gas Kinematics Main Drivers Outer disk center

4. Gas in Bars Gas in Bars Basics Meier & Turner (2004) 2 1 NGC 4303 Schinnerer et al. (2002) CO(1-0) Roberts & StewarT (1987)

5. HI-NUGA- Gas Dynamics Over the Entire Disk VLA HI Survey of 16 Nearby Active Galaxies AIM: Trace Gas Flow from Outer Disk to Very Center S. Haan, PhD Thesis

6. Seyferts LINERs Non-AGN Intensity Map Intensity Map Intensity Map Velocity Field Velocity Field Velocity Field Findings (haan et al. 2008): LINERs - more large HI rings - more kinematically disturbed  specialTime for Gas Flow in Barred Galaxies  AGN activity linked to overall Disk kinematics

7. 22. Jan. 2008 Seyferts LINERs Non-AGN HI Intensity Map HI Intensity Map HI Intensity Map Velocity Field Velocity Field Velocity Field Findings (haan et al. 2008): LINERs - more large HI rings - more kinematically disturbed  particular time for gas flow in bars  AGN activity linked to overall Disk kinematics

8. Finding Inflows using Gravity Torques Gas Dynamics within the DIsk Haan et al. (in prep.) Stellar Potential Gas Distribution Torque Maps Show In/Outflow Angular Momentum transfer Inflow outflow Noncircular Motions = inflow

9. Gas Flows and Mass Transfer Efficiencies Gas Dynamics within the DIsk Significant Gas Mass Redistribution Larger Gas Inflow Rates in Centers Gas Flow Across Corotation Resonance => Strong Secular Evolution within Disks Haan et al. (in prep.)

10. NGC 6946 - Central Mass Build-Up Molecular Gas Kinematics And Star Formation Tracers at High Spatial Resolution

11. Molecular Gas at ~10pc Resolution mm-Interferometry IRAM, Plateau de Bure High Spectral (few km/s) & Spatial (<1’’) Resolution Up-graded IRAM Plateau de Bure Interferometer: ~ 0.3” resolution (at 1mm) 3x more sensitive ~ 10x faster Multi-Line Observations --> Chemistry New Band: 2mm

12. Nuclear Region of NGC 6946 Stars vs. Molecular Gas D=5.5 Mpc; 1” ~ 25 pc D=5.5 Mpc; 1” ~ 25 pc PA ~ 35 o ; Incl. ~ 35 o PA ~ 35 o ; Incl. ~ 35 o Large-Scale Bar Large-Scale Bar 50pc HST H band Stellar Bar in NIR w/ Length ~ 10” - 15” PdBI 12 CO(2-1) 20pc Schinnerer, Böker, Emsellem, Lisenfeld (2006) Gas Shows Classical Response Pattern for a Bar

13. Bar-Driven Fueling NGC6946 CO(2-1) Model Intensity Velocity 400pc long bar Redistributes gas ~ 10 7 M sun (r < 30 pc) CR @ 260 pc  bar =510 km/s kpc -1 Schinnerer, Böker, Emsellem & Lisenfeld (2006)

14. Where and When Stars Form Central 50pc of NGC6946 Schinnerer, Böker, Emsellem, Downes (2007) Pa  HCN(1-0) 3mm Continuum SFR ~ 0.1 M sun /yr Age ~ 5-10 Myr SFR ~ 0.06 M sun /yr Age ~ < Myr SFR ~ 0.1 M sun /yr Age ~ couple Myr Star Formation in small Area over ~ 10 Myr Fueling via Inner bar Mass Build-Up of ~ 10 6 M sun In central 50pc (over last ~ 10 Myrs) 20pc

15. IC 342 - Nuclear Fueling & Star Formation Feedback Impact of Nuclear Star Formation Onto the Gas Flow

16. Nuclear Cluster in IC342 A Late-Type Barred Spiral (Böker et al. 1997, 1999) Nuclear Stellar Cluster: star formation ~ 4 - 30 Myrs ago Cluster mass ~ 10 7 M sun HST V D=3.3 Mpc; 1” ~ 16 pc PA ~ 35 o ; Incl. ~ 31 o Bar Length ~ 11 kpc

17. IC 342: Distribution of Molecular Gas 110 pc OVRO CO (1-0) H 2 Mass (1’) ~ 4.4 x10 7 M sun Masses ~ 10 6 M sun Diameters ~ 20 - 50 pc (Wright et al. 1993, Levine et al. 1994) Meier & Turner (2005)

18. Zooming in - IC342 Gas vs. nuclear cluster (Schinnerer, Böker, Meier, Calzetti, in prep.) 16pc Molecular Gas & Dust Coincide Gas reaches close To nuclear cluster (even more so in dense gas)

19. Ongoing Fueling? - IC342 H  Bubble fills CO Cavity  stellar winds/SN appear to Shape inner edge of Eastern spiral arm (obscured) HII region (Schinnerer, Böker, Meier, Calzetti, in prep.)

20. Self-Regulation of Star Formation What is happening - Suggested Scenario Before SF after SF Nuclear SF changes Gas Flow Timescales: v winds (15-20 km/s): ~ 3 Myrs age SF ~ 4-30 Myrs Energies: E mech (SB99) ~ 5e52 erg E GMC (2e6M sun ) ~ 3e52 erg Scenario plausible (Schinnerer, Böker, Meier, Calzetti, in prep.) Nuclear Star Cluster (almost) Shuts Off Its Own Supply ---> Feedback process!

21. What’s Next: - Star Formation, ISM And Gas Kinematics Molecular Gas Chemistry Utilizing Multiple Molecules

22. Next Steps - NGC 6946 Chemistry Schinnerer, Meier, Böker, Downes, Emsellem in prep. Locate: star forming gas (chemically) fresh gas [from atomic reservoir] (chemically) altered gas (SF, Gas Dynamics) Census of multi-phase ISM

23. (Gas) Kinematics & Star Formation Kinematics Kinematics --- ionized Gas (different ISM Phase) --- ionized Gas (different ISM Phase) --- Stellar Velocity Fields/Dispersion --- Stellar Velocity Fields/Dispersion => Better Models of Kinematics => Better Models of Kinematics (see Talk by G. Dumas) (see Talk by G. Dumas) Star Formation Star Formation --- History, Population, Location --- History, Population, Location --- Energy Injection into ISM --- Energy Injection into ISM --- Feedback Processes --- Feedback Processes

24. Summary & Conclusion Gas Kinematics Gas Kinematics --- Ongoing Gas Redistribution within Disk --- Ongoing Gas Redistribution within Disk --- bars work (in general, Small & Large) --- bars work (in general, Small & Large) --- Sustained Nuclear fueling for > 10 Myr --- Sustained Nuclear fueling for > 10 Myr Nuclear Star Formation Nuclear Star Formation --- can alter gas flow --- can alter gas flow --- self-regulated fueling --- self-regulated fueling => repetitive SF => repetitive SF time-variable time-variable (models) (models) Future Bright : ALMA ALMA ALMA site ALMA test facility